SMITHSONIAN

CONTRIBUTIONS

to

ASTROPHYSICS

Smithsonian Institution

Astrophysical Observatory

Volume 10, Number 1

An Analysis of the

Atmospheric Trajectories

of 413 Precisely Reduced

Photographic Meteors

By Luigi G. Jacchia,

Franco Verniani, and

Robert E. Briggs

Smithsonian Institution Press

Smithsonian

Contributions to Astrophysics

VOLUME 10, NUMBER 1

AN ANALYSIS OF THE ATMOSPHERIC TRAJECTORIES

OF 413 PRECISELY REDUCED PHOTOGRAPHIC METEORS

by LUIGI G. JACCHIA, FRANCO VERNIANI, and ROBERT E. BRIGGS

SMITHSONIAN INSTITUTION PRESS

Washington, D.C.

1967
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Contents

Page

1. Basic meteor theory 2

2. The observed decelerations; errors, fragmentation 3

3. The tables of basic observational data 5

a. Explanation to table 1.1 5

b. Explanation to table 1.2 7

4. Heights, lengths, and durations 7

a. Description of least-squares analysis; interrelation of variables . 7

b. Results of least-squares analysis 10

c. Tables and diagrams 14

d. Small-camera meteors 15

e. Position of maximum light 17

f. Duration 19

5. Decelerations 20

6. Magnitudes and "color index" 24

a. Magnitudes 24

b. "Color index" 28

7. The ablation coefficient a 28

a. Dependence of the mean <r on the other parameters 28

b. The variation of a along the trajectory 32

8. The fragmentation index X 33

9. Wake and blending 38

10. Peculiarities of individual showers; meteors with abrupt beginnings; asteroidal meteors 41

a. Showers 41

b. Meteors with abrupt beginnings 42

c. Search for asteroidal meteors 43

Acknowledgments 44

References 44

Abstract 46

Tables 47

in

An Analysis of the Atmospheric Trajectories of

413 Precisely Reduced Photographic Meteors

Luigi G. Jacchia,1 Franco Verniani,2 and Robert E. Briggs

 3

A previous paper (Jacchia and Whipple-, 1961)

contains a discussion of the orbital characteristics of 413 precision-reduced meteors doubly

photographed with the Baker Super-Schmidt

cameras in New Mexico. The present paper

contains an analysis of the atmospheric trajectories of those same meteors and deals with

the physical aspect of the meteor phenomenon.

A description of the observational material

has been given in the above-cited paper by

Jacchia and Whipple (1961); reduction techniques have been fully described by Whipple

and Jacchia (1957) and will not be repeated

here except for points that need more detailed

explanation. We shall outline here the criteria

used in the selection of these 413 meteors out

of a total of about 3500 meteors doubly photographed by the Super-Schmidt cameras during

the same time interval. The shutters of the

Super-Schmidt cameras have two 45° openings

and rotate at 1800 rpm; the meteor trail is thus

interrupted 60 times a second and presents the

aspect of a row of segments separated by wider

breaks. In making the selection we deliberately

chose only those meteors that were likely to

yield excellent decelerations. On this basis we

discarded nearly all meteor trails showing less

than 20 clearly discernible segments and those

whose segments were too closely spaced, as

1

 Harvard College Observatory and Smithsonian Astrophyslcal Observatory.

1

 Centro Nazionale per la Fisica dell' Atmosfera e la Meteorologia del

CNR, Rome, Italy; formerly at Harvard College Observatory and

Smithsonian Astrophyslcal Observatory.

* Smithsonian Astrophysical Observatory.

well as trails appearing against rich star fields

or too faint to be measured with accuracy.

The selected meteors have an average of 40 wellmeasured segments on the better of the two

films, and 34 on the other, and for all but 17

meteors the instant of appearance was recorded

visually. A secondary criterion for selection

was that comparable numbers of meteors should

be chosen in the low, medium, and high-velocity

groups, and for each month of the year. For

months particularly rich in meteors, the standards of acceptance were set a little higher so

that the month in question should not exert

an overwhelming weight in the analysis of

seasonal effects on decelerations. On the other

hand, we have occasionally included a larger

number of meteors belonging to a few selected

showers (Quadrantids, for example) because

their reductions were deemed useful for orbital

purposes.

As a result of this selection, the data presented here do not represent a random sample,

a fact that should be kept in mind in evaluating the analysis. In particular, it should be

remembered that by excluding meteors with

closely spaced trail segments we have eliminated

more of the low-velocity than of the highvelocity meteors. The bias introduced by our

selection is added, of course, to the bias already

inherent in meteor photography.

Basic trajectory data are presented in table 1.1; the individual determinations of velocity and decelerations with other quantities

derived from them are collected in table 1.2.
SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

1. Basic meteor theory

In this paper meteor theory is considered only

as a framework for the reduction of the observational material and is used in its simplest,

most unsophisticated form. We expect that

the observed deviations from this basic theory

might be of some help in future theoretical

work. Here is a summary of the basic equations and assumptions.

The acceleration v of a body of mass m and

frontal area A moving with velocity v through

a gas of density p can be written as

(1)

where CD is the so-called drag coefficient. For

supersonic velocities, CD has a nearly constant

value close to two for free-molecule flow, and

again a nearly constant value of 0.92 in the case

of continuum flow. The meteors photographed

with the Super-Schmidt cameras have dimensions that are generally small compared with

the mean free path of atmospheric molecules

at the heights at which they are observed, so

we have assumed that free-molecule flow is

valid for them and we have assumed CD=

constant.

The presentation area A can be written as

A=am2/3, where a is a proportionality factor,

which depends on the density and shape of the

body. We have taken a=constant, which is

equivalent to assuming that all meteors have

the same density and shape factor. Equation (1) can thus be written as

(2)

where C is a positive constant. This equation

is generally referred to as the "drag equation."

The value of C can be determined from the

observed velocities and decelerations if p and

m are known.

The mass m can be computed from the observed light curve of the meteor under the

basic assumption that the am'ount of light Iv

in the photographic domain emitted by the

meteor body at any instant is proportional to

the kinetic energy of the atoms in the meteor

coma that collide with atmospheric molecules (Opik, 1933). The number of atoms in

the meteor coma is, in turn, proportional to

the rate dm/dt at which the meteor loses its

mass, so we can write (Whipple, 1943)

_ Tpdm ,

lp

~ 2 dt ' (3)

where TP is a proportionality factor; the subscript p refers to photographic intensities. This

equation is generally called the "luminosity

equation."

Since the spectra of meteors consist mainly

of a discrete number of emission lines whose

relative intensities greatly vary with meteor

velocity, we must expect TP to depend on v.

Let us assume that

Tp = TOpV

n

. (4)

Whipple (1943), on the basis of Opik's

theoretical results, had assumed n=l. Using

this value of n, Jacchia (1948) derived from

Opik's data the value T O P=6.46X1O- 1 9 (c.g.s.),

when the photographic intensity Ip is expressed

in units of the intensity of a zero-magnitude

star. These values of n and rOp were used by

Jacchia (1948, 1949a, 1952) for deriving the

masses of meteors of the Harvard-M.I.T.

meteor program.

Recently, Verniani (1964a), using the observational material of the present paper,

found n= 1.0±0.15 and T O P=1.OX1O- 1 9 ; the

same values were found to apply also to the

brighter meteors photographed with small

cameras prior to the use of the Super-Schmidt

cameras. Masses (m^) computed using this

new value of TOP are given in table 1.1, after

the values computed with the old coefficient

(m^,). It is these "new" masses (mi) that

have been used in the present analysis; whenever the symbol m appears in the tables without a subscript, it is understood that the mass

it represents was computed using TOP= 1.0 X10"19

(c.g.s.).

Meteor masses can be computed from equation (3). Integrating and taking n = 1, we have

2 r' 61 mt>—ma= ~£dt,

T0pJta V

(5)

where the subscripts a and b refer to two arbitrary points on the meteor trajectory. Removing tb to infinity and assuming that the
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS

residual mass of the meteor, after complete

deceleration, is zero, we have

Top Jt IT TOpV*

(6)

Here, v stands for the effective mean velocity in

the course of the visible trajectory and

E

•=r

Ldt (7)

is the meteor brightness integrated from the

point corresponding to the time t to the end of

the trajectory. The mass of the meteor before

entering the atmosphere is, then,

TOpJ2ET

(8)

EPa> is the total photographic light energy radiated by the meteor. For most meteors v does

not change by more than a few percent in the

course of the trajectory, so mm can be easily

evaluated from EPm. The quantity logi0 EPa> is

used in the present analysis as an index of

brightness and is called ea.

In a time interval dt the meteor body strikes

a mass Apvdt of air. This provides a kinetic

energy ^Aptfdt that is used to heat, melt,

vaporize, and fragment the body, causing it to

lose a mass dm. We can thus write

where /? is a proportionality factor that depends on the efficiency of the energy-transfer

process and on the physical characteristics of

the meteor body.

Dividing (9) by (1) we obtain

dm—cmvdv, (10)

where <r=f}/CD. This equation is sometimes

called the "mass equation." Since CD should

be nearly constant (we take it as being constant) and is known with a greater degree of

accuracy than any other parameter of the

theory of meteors, we see that equation (10)

provides the means of determining the factor

/3 for individual meteors when m, m, v, and v

are known. The factor <r, which is the directly

determinable quantity, is sometimes referred

to as the "ablation coefficient."

In (10) we can replace m and dm with their

expressions from the luminosity equation;

solving for a we have

h ^•dt

—vv —vv

(11)

an equation that contains only observable

quantities.

Integrating (10) between two points of the

trajectory characterized by the subscripts a and

b, respectively, we have

<r=2

In ma—In m^ (12)

Whenever more than one independent determination of the velocity is available in the

course of the trajectory it is preferable to determine a from equation (12), which involves the

integrated light curve and not the instantaneous

brightness as in equation (11); in this fashion

the effect of short-lived flares is smoothed out.

Actually, equation (11) is slightly inconsistent

from the observational point of view because

the instantaneous value of Iv can always be

determined, while v is computed from smoothed

data covering a sizable time interval.

2. The observed decelerations; errors, fragmentation

The process for deriving instantaneous decelerations has been described in detail elsewhere

(Whipple and Jacchia, 1957); here we shall

repeat only the essentials. Distance Dt from

an arbitrary point is computed for the observed

centers of all shutter-induced trail segments i

on each of the two plates. The constants a,

b, c of the equation

are computed by least squares; k is determined

from four equidistant points on a curve of

Di—vjtt as a function of tt. In the above

equation, b is the velocity of the meteor before

the onset of deceleration, vm; the instantaneous

velocity is given by

v=b+kcekt

and the instantaneous acceleration by
SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

The aim has been to derive accelerations

about 20 times larger than their inner probable

error. Trails of longer duration, for which it

appeared that a single least-squares solution

would have yielded a much larger ratio v/p.e.,

were subdivided into separate sections, for

each of which an independent deceleration was

computed. In addition to yielding accelerations at different points of the trajectory,

this division of long trails into sections has

the advantage of ensuring an excellent fit of

equation (13), which cannot be expected to

hold perfectly from beginning to end of a

long trajectory.

The sources of error in the results of meteor

reductions have been discussed by Jacchia and

Whipple (1961). They include effects deriving from the occasional lack of visual timing

or from a small angle of intersection of the

two meteor trails. Since meteors were not

included in the present material when the

geometric solution was not satisfactory, errors

from these causes in the heights, velocities,

and decelerations can be considered small.

We shall, however, repeat here what was said

in the paper on orbits concerning the effect

of a shutter flutter since this source of error

is greatest in the decelerations.

After a number of Super-Schmidt meteors

had been completely reduced, there was clear

evidence that a "flutter" affected the rotation

of all camera shutters. Although this instrumental trouble was later eliminated by the

installation of more powerful motors, it was

nevertheless present during the entire period

of time covered by the meteors included in

this paper.

The shutter flutter was semiregular in character and exhibited widely different amplitudes,

ranging from zero to 5°, with a fundamental

period of 0^23, but with occasional lapses into

cycles half or twice that length. When two

or more cycles of the flutter are covered by the

photographic trail, its effect can be eliminated

with relative confidence (Whipple and Jacchia,

1957). For shorter trails, however, the process becomes more questionable, and a few

meteors had to be rejected for this reason. It

should be kept in mind that for short trails

the shutter flutter may be the most important

source of scatter in the deceleration data.

When the observed accelerations v are compared with the theoretical accelerations vT computed from equation (2), a striking feature

emerges. While the accelerations in the early

part of the trajectories are in general statistical

agreement with the theoretical values, they

become increasingly too large, compared to

theory, as one proceeds toward the end of the

trajectories. This systematic effect has been

attributed to progressive fragmentation of the

meteor body (Jacchia, 1955). It was found

that in the course of an individual trajectory

the variation of log (v/vT) is roughly proportional

to that of the quantity

which was called the "mass-loss parameter."

The proportionality coefficient x> ie.,

d , v

X=-7-logi0—'

ds 6 vT

(15)

was called the "fragmentation index." Levin

(1961) rightly thinks that it should more appropriately be referred to as the "progressive

fragmentation index." The introduction of the

fragmentation index has proved very useful—

we could say indispensable—in the analysis of

the Super-Schmidt decelerations.

Severe fragmentation is found to affect the

factor a of the mass equations (10) to (12). While

it may be reasonable to assume that <r is nearly

constant for bodies of similar composition that

experience a gradual and regular ablation in

the course of their atmospheric trajectories, it

is hard to see how it could keep the same value

if the body dissolves in a train of fragments.

In such a case, the numerator in equation (11)

refers to the light emitted by all the fragments,

while the deceleration in the denominator is

probably that of the larger fragments in front

of the train. While the meaning of a may then

become obscure, it still remains a useful parameter since it characterizes the rate at which

the meteor is destroyed. If we take two

meteors with the same initial mass, velocity,

and angle of incidence, but characterized by

different values of <r, the one with the larger a

will have a shorter duration and greater maximum brightness.
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS

A question that logically arises is: what is

the meaning of the observed deceleration of a

fragmenting body? As long as the fragmentation consists of the progressive flaking off of

the outer layers of the meteor body, we shall

observe the same body at different points of

the trajectory, and the deceleration will refer

to this body. When, however, we have to deal

with a train of fragments of various sizes

that keep fragmenting, we may observe different bodies at different times and the measuring of the acceleration becomes more obscure.

In such cases we often observe a progressive

elongation of the photographic segments ("terminal blending") and, since we measure the

center of these segments, a contribution to the

acceleration may arise from the progressive

shift of the segment center, unless the elongation

happens to increase linearly with time. It

would be wrong, however, to attribute the

anomaly in the observed decelerations (x>0)

entirely to this effect. Although a statistical

correlation exists between x and the magnitude

of terminal blending, it is not infrequent to

find relatively large values of x among meteors

with no observable terminal blending, even in

the presence of favorable conditions for its

detection (long meteor duration, small angle of

incidence). This is what we could expect if

the spectrum of fragment sizes were to vary

greatly from meteor to meteor.

3. The tables of basic observational data

As was mentioned earlier, tables 1.1 and 1.2

list the basic observational data pertaining to

the 413 Super-Schmidt meteors involved in the

present analysis. An explanation of the headings of the tables is given below.

a. Explanation to table 1.1

Trail No. Serial number of trail photographed at the Dona Ana

station.

Date Year (1952, 1953, or 1954; the

first two digits are omitted),

month and day, with the fraction of the day given to

O^OOOOl, in U.T.

Shower No. Identification of associated

meteor shower, if any, as indicated in table 3 of Jacchia and

Whipple (1961); the table is

Apparent

Radiant

SinQ

CosZB

Mpm

H

HB

repeated at the end of these

explanations. Only the betterknown showers have been included; the letter "Q" after

the code number indicates a

questionable association.

The right ascension a and the

declination 8 of the apparent

radiant of the meteor trajectory. (The true radiant,

after correction for zenith

attraction and diurnal aberration, can be found in Jacchia

and Whipple, 1961.)

Sine of the angle formed at the

apparent radiant by the trails

as seen from the two observing

stations.

Cosine of the zenith distance of

the apparent radiant.

Velocity with respect to the

stations, corrected for atmospheric drag, in km/s.

Photographic absolute (i.e., reduced to a standard distance of

100 km) magnitude reached by

the meteor at maximum light.

Height above the geoid. The

heights listed are as follows:

Height corresponding to the beginning of the photographic

trajectory. The letter "G"

after a beginning height indicates that the beginning of the

meteor trajectory occurred outside the film limits and that

the actual beginning height was

greater than the given value.

Height corresponding to the

center of the first measured

trail segment (BD=beginning

dash).

Height of the point where the

absolute photographic magnitude of the brightening meteor

reached the value +2.5.

Height of the point where the

meteor reached its maximum

absolute brightness.
SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

HED Height corresponding to the

center of the last measurable

segment (.ED=end dash).

HB Height corresponding to the

end of the photographic trajectory. The letter "L" after an

end height indicates that the

end of the trajectory was cut

off by the edge of the film

and that the actual end height

was lower than the given value.

LA, LB Length, in degrees, of the trail

as photographed at the Dona

Ana (A) and at the Soledad

(B) stations, respectively.

The letter "G" indicates that

part of the trajectory was cut

off by the edge of the film and

that the true length is greater

than the given value.

D Duration of the photographic

trail, from HB to Hs, in seconds.

The letter "G" has the same

meaning as after LA and LB.

nA, nB Number of measurable segments on the trails photographed at Dona Ana (A) and

Soledad (B), respectively.

AM Magnitude difference between

the maximum light of the meteor and the film limit, on the

better of the two photographs.

Vis. A, Vis. B Visual magnitudes recorded by

the observers at Dona Ana (A)

and Soledad (B), respectively.

C.I. "Color Index," i.e., photographic minus visual magnitude, obtained by comparing

the maximum of the smoothed

photographic light curve with

the visual magnitude recorded

by the observer. If the visual

magnitude was recorded by two

observers, the mean of the two

values was taken. The photographic emulsion was Kodak

X-ray, a blue-sensitive film.

<» A measure of the integrated

brightness of the meteor; this

quantity is defined as

X

+co

Ipdt,

log

W, B

Rem.

where Ip is the absolute photographic brightness of the meteor expressed in units of zeromagnitude stars.

Mass of the meteor, computed

from the integration of the

photographic light curve, according to the formula

m,

' TopJ-. »»

dt.

Two values are given for the

mass: ra^i is the mass in the

Opik-Jacchia system used in

previous listings (Jacchia, 1948,

1949a, 1949b, 1952), computed

using for the photographic

luminous-efficiency coefficient

the value T O P=6.46X1O- 1 9

(c.g.s.; Ip in zero-magnitude

units); ma2 is the mass computed using T0p=1.0X10~19

(c.g.s.; Ip in zero-magnitude

units), a value close to that

derived by Verniani (1964a).

Logarithm of the quantity a =

(dm/dv)/mv. The given value

is the one that best fits the

whole trajectory. For fuller

explanation, see text (p. 28).

The "progressive-fragmentation index." For explanation,

see text (p. 33).

Wake and blending, respectively, expressed in an arbitrary

scale from 0 to 4. For fuller

explanation, see text (p. 38). A

letter "Q" indicates that the

given quantity is questionable.

The letters in this column describe peculiarities in the trail,

as follows:

A: abrupt beginning

F: one or more fragments became detached in the course

of the trajectory
ATMOSPHERIC TRAJECTORIES OF 413 METEORS

S: trajectory of unusually

short duration; the film

probably recorded only a

broad flare.

Code for identifying meteor showers listed

table 1.1

in

Shower

No.

None

1

2

3

4

5

6

7

8

9

Shower

Sporadic

meteors

a Capricornids

Southern

Taurids

Southern

t Aquarids

Geminids

8 Aquarids

Lyrids

Perseids

Orionids

Draconids

Shower

No.

10

11

12

13

14

15

16

17

18

19

20

Shower

Quadrantids

Virginids

K Cygnids

Leonids

X Orionids

Ursids

a Hydrids

Northern

Taurids

Andromedids

v Aquarids

Northern

i Aquarids

6. Explanation to table 1.2

All data refer to the center of the trajectory

sections from which velocities and accelerations

were derived by least squares. For each meteor

the data derived from the photograph taken at

Dona Ana are listed first in consecutive order,

followed, in the same order, by those derived

from the Soledad photograph.

Trail No. Serial number of trail photographed

at the Dona Ana station.

H Height above the geoid of the

point in the trajectory for which v

and v were determined.

v Instantaneous velocity of the

meteor, in km/s.

v Instantaneous acceleration of the

meteor, in km/s2.

p.e. Probable error of the acceleration,

in km/s2.

n Number of trail segments used in

the least squares.

Wi The instantaneous mass of the

meteor, computed from

m=-

log

log

A log pob,

A log pc

using the old value T O P =6.46X1O- 1 9

(c.g.s.; IP in zero-magnitude units).

The mass-loss parameter

s=\

The logarithm of the quantity

<r=(dmfdv)/mv, determined from

the instantaneous values of m, v,

and dv/dt.

The logarithm of the atmospheric

density computed from the drag

equation

v=-Cm-1/z ptf.

The adopted value of the constant

is log (7=0.333 when the masses are

expressed in the "old" system (mi)

and log (7=0.603 when the "new"

masses (mz) are used.

The difference log pobt — log p,t,

where p,t is the density tabulated

in the U.S. Standard Atmosphere

1962 (1962) for the observed height

H.

This quantity is defined as

A log pcorr = A log pobt— X(S— So),

with so=O.

The weight of A log pcorr, computed

according to the formula

4.

where

*(z)=#[l+erf (2.5 log x-2.1)]

(erf is the notation for the probability integral).

Heights, lengths, and durations

a. Description of least-squares analysis; interrelation of variables

We have considered four sets of heights:

beginning height HB, corresponding to the

first discernible dash on either of the two

plates; the height Ht.t, corresponding to the

point where the absolute photographic magnitude of the meteor reaches the value +2. 5

(Jacchia, 1960); the maximum light height
8 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

HML; and the end height HS) corresponding to

the last discernible dash on the two plates.

The heights Hz.i are generally quite close to

the beginnings of the meteors. They have

been chosen for the analysis with the purpose

of eliminating the scatter due to the variability

of the plate limit. Since the increase in light

of a meteor in the early part of its trajectory is

mostly gradual, even small differences in the

plate limit can have a considerable effect on

the height of appearance.

From the basic equations of meteor theory it

is possible to derive expressions that relate

these four sets of heights—or rather the

corresponding atmospheric densities p—to the

parameters -that characterize the meteor

body and its flight. Combining the drag

equation (2), the mass equation (10), and the

luminosity equation (3), we obtain (Jacchia,

1949a)

I=CI^am

2lW, (16)

from which we can compute p at any given

point, provided we know I, m, v, and a. With

the conditions proper to each set of heights,

we obtain

m;

2/3

(17)

p2.5=(l/5CV0p)<r-K8 m-J'3, (18)

PML=(yCHp)a-1(vl-\-&/<x)-1m

1

J1

3

 cos ZR, (19)

and, from the integration of equation (9),

cos ZR. (20)

In equation (17), the symbol /„„ indicates the

limiting magnitude of the film. For a random

selection of meteors we can assume that the

angular velocity is proportional to the velocity

v, so that Ium^Vn, which would result in a

change from —6 to —5 in the power of vm in

the equation. Our meteors were not randomly

selected, but the relation between IHm and t>«,

can be assumed to be still valid in a first

approximation.

In equations (19) and (20), the symbol Hp

indicates the atmospheric pressure scale height;

in the last equation, v is a mean velocity, which

is denned as

J B

pdl

JB

where dl is an element of distance along the

trajectory and B and E indicate the beginning

and end points, respectively.

In all four equations the first factor, in parentheses, is a combination of quantities that we

can regard as constants. We have excluded a

from the parentheses because it is a basic

parameter, variable from meteor to meteor,

whose value is generally determined. The other

basic parameters that we find with various exponents in all four equations are vw, m^, and

cos ZR. It is true that in equation (19) the

velocity term is (v^+Q/a)'1, but this is equivalent to vZn

, with n close to 2 (2.2 for ^=2 0

km/s, 2.1 for ^=3 0 km/s; 2.0 for higher

velocities). In equation (20) we commit only

a tolerable error if we replace v with vm. It is

these four fundamental parameters (v^, m^,

cos ZR, a) that we shall use in the analysis of

the observed heights; we shall add to them a

fifth, the fragmentation index \, which is also

likely to affect the heights. For all sets of

heights we shall write the equation of condition

in the form

log p=C0+Ci log COS ZR + Ci log Va

-f c3 log m, +c 4 log <r-\-CiX- (21)

Since the proper form in which x enters the

equation is not known, we have selected the

simplest form, remembering that x is already a

logarithmic quantity. In view of the relatively

weak dependence of p on x, a change in the form

of the last term would leave the solutions essentially unaltered.

Because of natural selection and other factors,

hardly any of the five parameters can be considered to be entirely independent of all the

other four. For example, there is an obvious

relation between mass and velocity. A less

obvious relation exists between ZR and velocity,

and, therefore, also between ZR and mm, since

the field covered by the Super-Schmidt photographs was always close to the zenith. A dependence of a on velocity is apparent from the

analysis of the section devoted to the ablation
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 9

coefficient. The degree of interrelation between the various parameters can be appraised

by examining tables 2.1, 2.2, 17.1.2, and 19.3.

An analysis with all possible combinations of the

basic parameters would have led to an enormous, and probably meaningless, number of solutions, so we decided on four sets of solutions

for each set of heights, starting with the solution

for c0, Ci, and Ct only, i.e., with only cos ZR and

va as variable parameters, and adding the remaining parameters one at a time, until the last

solution contains all five of them. The order in

which the parameters are added after the first

solution was decided on the basis of the prospective importance of the parameter in affecting

the heights.

A further proliferation of solutions is dictated

by the advisability of separating special categories of meteors from the solutions and of

evaluating their effect when they are included.

Thus, we have excluded, singly or jointly,

meteors of the following categories: 123 meteors

in well-established showers (Sh); 26 meteors with

an abrupt beginning (A); 12 meteors with short,

flarelike trails (S); 22 meteors with highly anomalous deceleration (D).

In addition, separate solutions have been

made for meteors with aphelion distances respectively smaller and larger than 6 a.u., for

three different groups of log a « —11.4, between — 11.4 and —11.0, and > —11.0), and

three groups of x (—0.2 < x <0.2 and x >0.2

and x >0.4). Altogether, the following tables

of solutions were computed:

3.1 All Super-Schmidt (S.S.) meteors

3.2 All minus D

3.3 Sporadic (Sp) [=all minus Shi

3.4 Sp minus D

3.5 Sp minus (A+S)

3.6 Sp minus (A+S+D)

3.7 Sp minus (A+S+D) with log cr<-11.4

3.8 Sp minus (A+S+D) with —11.4 < log a

< -11.0

3.9 Sp minus (A+S+D) with log* > —11.0

3.10 Sp minus (A+S+D) with -0.2 <

X < 0.2

3.11 Sp minus (A+S+D) with % > 0.2

3.12 Sp minus (A+S+D) with x > 0.4

3.13 A only

3.14 Sp with Q < 6 a.u.

3.15 Sp with Q > 6 a.u.

For the sake of comparison we have also

computed two solutions for the small-camera

meteor material, for which most of the observational data have been published by Jacchia

(1952). The first solution includes all available

meteors, while the second solution is limited to

sporadic meteors only (tables 3.16 and 3.17,

respectively).

The results of all these solutions are given

in tables 3.1 to 3.17, in which the coefficients

c0 to c5 can be found with their respective

standard deviations. Table 4 presents what

we believe are the most reliable values of all

the coefficients from a survey of all solutions for

Super-Schmidt meteors.

The coefficient c0 given in all these tables is

not the one defined by equation (21), i.e., the

value log p takes when all the five variables

are zero. Some of the variables, such as log v

and log <r, never come even close to zero; so

c0, defined in this manner, would represent a

tremendous extrapolation and its standard

deviation would be entirely meaningless for

the user of the tables. To bring c0 within the

range of the observed values of p, we have

subtracted from each variable in the equation

a constant close to its logarithmic mean value.

The constants, expressed in the c.g.s. system,

are:

log cos Z s = —0.2

log ^ =6.477 (^=3 0 km/s)

logm^ =-0.523 (ma>=0.3g) Y (22)

log a =-11.20

X =0.25

In computing the theoretical value of c0

for the beginning heights in table 4 we have

assumed, on the basis of figure 3a, that the

plate limit for the "standard" meteor, as

defined by (22), is magnitude +2.6(p#). The

equation for the end points does not contain

the plate limit: in equation (20) the end point

is defined as the point where the mass of the

meteor is reduced to zero. Whenever we

compare the observed meteor heights and

lengths with those given by theory, we must

keep in mind that the latter could be affected

by a systematic error owing to the assumptions

in the computations of the co's.

For the other constants involved in the

computation of the theoretical values of c0 we
10 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

have used (7=4.01 and TOP=1O"19 (c.g.s.);

for Hp we have taken 5.4 km, which, according

to the U.S. Standard Atmosphere 1962 (1962), is

the scale height prevalent in the height range

from 80 to 90 km.

In compiling table 4 we have generally

given the greatest weight to the solutions containing only the "cleanest" and most uniform

material, i.e., sporadic meteors, from which the

most anomalous members—those of classes A,

S, and D—had been removed. Concerning the

results summarized in table 4, a few cautionary

remarks seem to be in order before any discussion. It should be clear that the least-squares

process cannot give a correct solution when the

parameters are interrelated—and, as we said,

nearly all our meteor parameters show some

degree of intercorrelation. The saving factor

in such a situation is the relative looseness of

the correlations. In any case, we must

expect that the variables that—owing to a

large coefficient, or a wide range, or both—can

cause large variations in log p will have the

better determined coefficients. Thus we feel

that the coefficients of log »„, log cos ZR, and

log mm can be trusted to be rather safe, although

in decreasing order. On the other hand, it may

be questioned whether the coefficients of log a

(which varies with »x) and of x (which varies

with Woo and cos ZR) are always significant.

To give an idea of the effect of the interrelations between the variables, we have taken

three groups of meteors, each within narrow

velocity limits, and have computed for them the

value of c3 in the equations

log p=const+c3 log mo

and

(for pfl and p2.5)

log P—const+log cos ZR+c3 log mm

(for pML and pB).

The results are given below. The last line

gives the results for c3 as obtained from the

least-squares solutions for the coefficients c0,

Ci, Ct, and c3, covering all Super-Schmidt meteors.

t>c=(km/s) HB H^

21-24 —0.11 ±0.18 -0.24±0.18

29-32 —0.23±0.11 -0.34±0.10

60-65 -0.35 ±0.09 -0.33 ±0.10

All —0.25±0.04 —0.30±0.04

6. Results of least-squares analysis

The observational values of the coefficients c0

to c5 are compared in table 4 with their theoretical values. As expected, c\, the coefficient

of log cos ZR, is in essential agreement with

theory. In view of the purely geometric nature

of this variable, any difference in Ci from its

theoretical value should probably be ascribed

to inadequacies in the least-squares process

caused by the interrelation of the variables.

The coefficient ci is the only coefficient that

actually conforms to theory. Even a cursory

glance at table 4 will reveal that the discrepancies between theory and observation are

quite large, and it may come as a surprise that

the largest discrepancies in all coefficients, except Ci, occur in the beginning heights. Tn the

case of c0 there might be a partial justification

for this discrepancy in the fact that the values

of C and a in equations (17) to (20) come from

decelerations at points that are mostly located

in the second half of the trajectory. This,

however, is definitely no reason why the other

coefficients should also be anomalous for the

beginning heights.

While the discrepancies in the heights of maximum light and in the end heights can be blamed

on the effects of fragmentation, it is more difficult to do the same for the beginning heights

and for Hz*, where fragmentation should presumably be less important. While it cannot be

excluded that even near the beginning of the

trajectory, fragmentation might play some role,

it appears probable that at least part of the

discrepancy can be explained by assuming that

in the early parts of the photographic trail a

nonnegligible fraction of the heating energy is

dissipated as surface radiation. The heating

energy available to a spherical meteor of radius

r and velocity v is %\itr2p^dt, where A is the

heat-transfer coefficient and p the atmospheric

density. The energy radiated by the meteor

surface is Airr^eaTtyt, where « is the emissivity,

a the Stefan-Boltzmann constant, and T the

temperature of the radiating surface. Thus, the

" M L

0.45±0.12

0.33±0.10

0.29±0.14

0.41 ±0.03

HE

0.48±0.11

0.34 ±0.09

0.30±0.13

0.45±0.03

No. obs

41

45

25

~400
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 11

ratio of the energy radiated by the meteor to

the heating energy is

Since we can expect to have e/A> 1 and

T>2000° K, we shall obtain a minimum value

of R if we put e/A=l and T=2000° K. For

the average Super-Schmidt meteor, the velocity

is 35 km/s and the height of appearance is 100

km, where, according to the U.S. Standard Atmosphere 1962 (1962), the density is 5.0 X10"10

g/cm3. Using the above values, we obtain

#=0.33; in other words, at least one-third of

the heating energy is radiated from the meteor

surface. In view of the interplay of v, p, and T

in the beginning heights, it is understandable

that in the early part of the trajectory R

should be velocity-dependent, thus altering

the relation between velocity and height of

appearance as derived under the assumption

that surface radiation is negligible.

Thus, according to observations, for the

beginning heights we have p^-5=const, when

we consider meteors of equal masses, instead

of the theoretical relation pt^+=const. For

the fixed threshold of magnitude +2.5 on the

ascending branch of the light curve, we have

pv*=const instead of pv

6=const. The effect

of the meteor mass on the height of appearance

is, according to observations, less than one-half

of the effect predicted by theory, and the effect

of o- is nil—a fact that looks rather puzzling.

For the heights of maximum light and end, the

dependence on the mass is close to theory, but

the coefficients of log v and log a are smaller

than their theoretical values.

For a standard meteor, whose characteristics

are given by equation (22), the observed values

of c0 are —9.23 at the beginning and —8.06 at

the end; these values correspond to a height of

appearance of 99.0 km and a height of disappearance of 84.5 km. We thus have a height

range of 14.5 km, which corresponds to a length

of trajectory of 23.0 km. This compares with

a theoretical length of 34.1 km. The length of

the observed trajectory is thus only 67 percent

of the theoretical length.

Since, according to observations, a affects

the end heights but not the beginning ones, its

ultimate effect is that of changing the length of

the trajectory. From the values c4=0 for the

beginning points and c4=— 0.4 for the end

points, we deduce that two meteors, identical

except for a difference of one unit in log a

(log <r= —10.7 and —11.7, respectively, are

well within the observed range) will appear at

the same height but will disappear at heights

differing by 5 km. The meteor with the larger

a has a shorter trajectory, and the difference

(about 35 percent) arises from the greater end

height.

This effect can be seen also from the inspection of the co's in the sets of solutions given in

tables 3.7, 3.8, and 3.9. Since the meteors

within each group have a small range in log a,

it is best to take the solutions for the first four

coefficients only. Converting densities to

heights, we have the results given below for

the three groups of meteors. From these data

we have dL/d log <r~ — 8.

As we can see, the theoretical trajectory

length is approached as we go to lower values

of a. From the above data it looks as if a

meteor with a value of log a in the vicinity of

— 12.0 should have a length close to that

predicted by theory. Starting from the length

of our standard meteor and extrapolating

linearly with Ac4= +0.4 to low values of er,

we must go to log a— —12.5 before we reach

agreement with theory. This extrapolation,

however, is less justifiable than the first

because the relation between A log p and log a

does not appear to be linear and the value

Ac*= +0.4 was derived from all meteors whose

majority have values of log a larger than

-11.3.

The coefficient c5 of x is generally rather

small and close to its standard deviation for

the heights of maximum light and end. The

beginning heights and H2i, on the other hand,

show a more definite dependence on x- The

11.

11.

Group

log(r< —11.

4<logcr<—11.

0<log a

4

0

Mean log <r

-11.55

-11.19

-10.86

log p B -lo g pE

— 1.

- 1 .

- 1 .

54

19

07

H

19.

14.

13.

B —

2

9

3

Hs

km

km

km

Length

30.

23.

21.

5 km

6 km

1 km
12 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

difference between the value of c5 for the

beginning heights and that for the end heights

is Ac5= +0.3. As in the case of a, the larger

X is, the shorter the trajectory. With the above

value of Ac5 we find that a meteor with x= l

has a trajectory 6 or 7 km shorter than an

otherwise identical meteor with x=0; the

shorter trajectory is mainly due to a lower

beginning point. The effect can also be seen

comparing the values of c0 in tables 3.10, 3.11,

and 3.12, as follows.

are derived from the integrated luminosities

according to equation (8). We shall then have

Group

lx!<0.2

x >0.2

X>0.4

Mean x

0.04

0.49

0.70

: log PB—log Pi

— 1.26

— 1.06

-0.9 7

s HB —

15

13

11

.7

.1

.9

Length

24.9

20.8

18.8

From these data we derive dL/dx=—$- For

the variation of L with a we had previously

found dL/d log a= — 8. If we want to compare

the relative effects of the observed scatter in a

and in x on trajectory lengths, we must multiply

these derivatives by the standard deviations

for one observation in <r (±0.235) and in x

(±0.29), respectively. Thus we find that the

observed scatter in x has an effect 1.4 times

greater than the observed scatter in a.

Comparing the respective effects of a and x

on the trajectories, we see that a affects mainly

the end heights, while x has its greatest effect on

the beginning heights. The effect of a is what

would be expected if a controls the rate of

ablation: the larger a, the higher the end of

the meteor. The significance of the effect of

X on the beginning heights—a lowering of the

beginning height when x is larger—is not so

clear. Verniani (1964a) found that the luminous efficiency rOp of Super-Schmidt meteors

varies with the fragmentation index x according

to the relation

dlog TOp/dx=— 0.50

with a probable error of ±0.11.

A change in rOp in equation (16) involves a

corresponding change in ma , since our masses

dlog PB=—%d\og

and

d log PB d log PB d log TOP 1 / 1\ 1

dx ~ dlog TOP dx 3 \ 2/6 '

This is just about the value of c5 we found for

the beginning heights (table 4). It thus

appears possible that the effect of x on the

beginning heights might come about through a

variation of the luminous efficiency with xIn this connection it will be recalled that

Millman (1935) and Russell (1960) have noted

that the excitation of the iron vapor in meteor

spectra is lowered in flares. On the other hand,

according to Millman and McKinley (1963),

it is quite normal for the ionized elements to

appear strong in bursts.

Since fragmentation lowers the height of

appearance of meteors, the case of the highly

fragmentable Draconids, for which Jacchia,

Kopal, and Millman (1950) and Jacchia (1963)

found anomalously great heights, remains more

puzzling than ever. We can only surmise, on

the basis of the unique appearance of some

members of this shower (Jacchia, 1956, 1963),

that this group of meteors is so different from

the ordinary meteors. regarding their physical

characteristics that in their flight other phenomena overshadow the usual effects.

It may be of interest to compare the values

of ct and c3, the coefficients of log v and of log TO,

in the three sets of solutions, tables 3.10, 3.11,

and 3.12, which cover different ranges of xTaking c% from the solutions for c0 to c3 we have

the beginning heights as shown below.

As we can see, an increase in fragmentation

causes the coefficients to stray more from their

theoretical values; it is clear, however, that

even for x=0we are still very far from having

agreement with theory. For the heights of

maximum light and end, the dependence of

the coefficients on x is considerably less evident.

Group

lxl<0.2

x>0.2

x>0.4

rheoretio

Mean x

0.04

0.49

0.70

xl values

-3.60±0.21

—3.32 ±0.23

-3.07 ±0.40

(—5+)

c3

-0.29 ±0.06

—0.11 ±0.07

-0.03 ±0.12

2/

No. obs

117

109

50
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 13

-11.0

-10.5 •

-100

-9.0

3 -85

(km)

- 70

-7.0

15 20 30 40 50 60 70

a

-7.5

-10.8 -11.0

- 80

-11.2 -11.4

log a- (cmV)

-7.5

0.1 015 02 0.3 0.4 05 0.6 07080910

CosZ,

FIGURE 1.—Heights of the standard meteor for all Super-Schmidt meteors: a, means for velocity groups when velocity is varied;

b, means for mass groups when mass is varied; c, means for ablation coefficient groups when ablation coefficient is varied; d,

means for zenith angle groups when zenith angle is varied.

The separate solutions for meteors with

aphelion distances greater than 6 a.u. and

smaller than 6 a.u., respectively (tables 3.14

and 3.15), confirm the effect found by Jacchia

(1958, 1963) for the beginning heights, namely

that meteors in long-period orbits appear at

greater heights than those in short-period

orbits. The difference between the two groups

is about 1.8 km (0.12 in log p), and with little

change it carries through to the heights of

maximum light and end. The average values

of log <r and x for the two groups are as follows:

a.u.

Q<6 a.u.

log a

— 11.27 ±0.02

-11.14±0.02

0.24 ±0.03

0.26 ±0.03

The difference in x is inconclusive, while the

difference in a is accounted for by the difference

in velocity between the two groups (see sec. 7).

The solutions for the 26 meteors with abrupt

rise from beginning to maximum light (table

3.13) show that such meteors become visible,

on the average, 4 km lower than the other

meteors with the same characteristics of mass,

velocity, and angle of incidence, and disappear

about 1 km lower than these. (These data

have been taken from the solutions for the first

four coefficients only, since a larger number of

unknowns is bound to make the solutions

unreliable with such a scanty sampling; actually

the difference becomes a little larger when all

six variables are introduced.) By having an

abrupt beginning, a meteor trajectory is,

therefore, shorter by 20 percent on the average.

225-636 O-67—2
14 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

-11.0

120

- 8 0

-11.2 -11.4

log <r(cm2s

2

)

-11.6

-9.5

-9.0

-8.5

-8.0

-7.5

-7.0

-10.0

-9.5

"p. -9.0 •

-8.5 •

-8.0 •

d

-7.5

O.I

1 1 i i

i 1 _

J70

no

H

(km)

- 90

• 80

0.15 0.2 0.3 0.4 0.5 0.6 070.80910

Cos ZR

FIGURE 2.—Heights of the standard meteor for sporadic Super-Schmidt meteors only, excluding classes A, S, and D: a, means for

velocity groups when velocity is varied; b, means for mass groups when mass is varied; c, means for ablation coefficient groups

when ablation coefficient is varied; d, means for zenith angle groups when zenith angle is varied.

An abrupt rise to maximum is invariably

followed by a gradual blurring of the shutter

breaks; clearly the phenomenon is caused by a

sudden disintegration of the meteor body. If

it had not been for this disintegration, with its

concomitant increase of effective presentation

area, the meteor probably would not have

been visible at all on the photographs, because

it was too faint; this explains the lower heights

of appearance of such objects.

We shall conclude this account of the leastsquares analysis of the heights of Super-Schmidt

meteors by giving, for quick reference, the

equations for log p at the four usual heights

with the observational coefficients from table

4—except for c0, which here has the same

meaning as in equation (21).

log P B =13.26-3. 5 log va — 0.25 log ro.-f-0.2x

(23)

log P25 = 16.59—4.0 log v,,—0.28 log ro.

+0.1 log cos Zfl (24)

log Puh—— 2.61 —1.7 log t>.+0.37 log mm

+ 1.0 log cos ZR—0.5 log o- (25)

log PE= -3.00 —1.4 log ©.+0.40 log-ro.

+ 1.2 log cos ZR-0A log (T-O.lx- (26)

c. Tables and diagrams

The correlation between meteor heights and the

variables that were used in the least-squares

analysis is better visualized when we vary one

parameter at a time. To do this we must first
-10.5

-10.0

-9.5

"1

3

1

 -9.0

Q.

-8.5

-8.0

-7.5

-7.0

ATMOSPHERIC TRAJECTORIES OF 413 METEORS

-10.0

15

• or o Q < 6 a u

x or o 0 > 6 a u 120

- 9 5

-9.0

-8.5

-8.0

-7.5

-7.0

-KH.

.'*'''

no

too

90 H

(km)

80

70

80

- 70

b

10"'

mjg)

a

20 3 0 40 50 60 70

-I0.0

-9.5

-9.0

2 -8.5

a.

o>

o

-80

-75

-

HB

- H e -

HUL*

X--—

HE

-

. -"

- ^

• Q < 6 a u

x 0 > 6 o u.

_ _ ^

~ 2 • -

- I00

90 H

(km)

- 80

- 80

-II.6

-7.5

d

0.3 Q4 05 06 07080910

CosZ.

-108 -110 -11.2 -11.4

C log <r (cni2s

2

)

FIGURE 3.—Heights of the standard meteor for all Super-Schmidt meteors, divided into two groups according to aphelion distance

Q: a, means for velocity groups when velocity is varied; b, means for mass groups when mass is varied; c, means for ablation

coefficient groups when ablation coefficient is varied; d, means for zenith angle groups when zenith angle is varied.

reduce the heights to standard values of all the

other parameters, then divide the heights into

groups that fall within convenient intervals

of the variable in question, and finally take

means of the values within each group. The

standard values that were selected for the

various parameters are the same that were used

for the computation of c0, equation (22). For

the reduction to standard values we used the

coefficients obtained from the particular leastsquares solution pertaining to the group of

meteors analyzed.

The results of these efforts appear in tables

5.1.1 to 5.6.4 and figures 1 to 4. For the sake of

completeness we have added in tables 6.1 to 6.2

and figure 5 the unreduced means of the four

types of heights for the usual velocity and mass

groups. The latter data may be useful for

purely statistical purposes.

The relation between log va and log p corresponding to the various heights we consider is

not strictly linear. As a result the averages

computed for all meteors do not necessarily fall

on the curves of log p as a function of vm.

Whenever mean values appear in tables

throughout this paper, we have also given their

standard deviations. These appear as confidence marks in all diagrams where means are

plotted.

d. Small-camera meteors

Basic data for 119 meteors photographed in

Massachusetts and in New Mexico with small-
16 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

-90 h

-8.5 h

-80 k

-7.5 h

i r

-

-

1 i

—i—i—i—

A

/N

A

y>~*~— ^ ^

• IXI < 0.2

* X > 0.2

1 1 i__

—1 1—

HB -

/ " •

i i

-9.5 V

-9.0 1-

-8.5 h

A IOO «-

H -8.0

(km)

-70

mjg)

d70

30 40 50 60 70

-80h •

X

— > ^

—•«^TM-•*

IXI S 0 2

X >0 2

l ,

r

i

i

i

i

~ — *

~~~-x -

1

-95 h

Hioo

90 H

(km)

"t "9.0

-8.0

H80

-7.5

I I i i

110

80

-112 -114

log o- (cm2s

2

) d

O.I 015 02 0 3 04 05 06 07080910

Cos ZR

FIGURE 4.—Heights of the standard meteor for sporadic Super-Schmidt meteors minus (A + S-f-D), divided into two groups of the

fragmentation index x: a, means for velocity groups when velocity is varied; b, means for mass groups when mass is varied;

c, means for ablation coefficient groups when ablation coefficient is varied; d, means for zenith angle groups when zenith angle

is varied.

aperture patrol cameras have been published

by Jacchia (1952). Several more of such meteors have been reduced with precision techniques; altogether we now have data for 210

small-camera meteors. For many of these it

was impossible to obtain reliable decelerations,

not to speak of such quantities as a and x,

which require first-class data. The first of

these, a, was computed for only 88 meteors,

and the second, x» for only 58. In spite of the

heterogeneity and much lower quality of this

material, we thought that it would be appropriate to run it through the analytical process

so that the results could be compared with

those of the Super-Schmidt meteors.

The results of the least-squares solutions

(tables 3.16 and 3.17) are given after those for

the Super-Schmidt meteors. Even a cursory

glance at these tables shows that the coefficients Ci and C2 undergo drastic changes when

the mass is added to the variables, indicating

a higher degree of interrelation among the first

three variables (cos ZB, v^, mm) than in the

Super-Schmidt material. The further changes

that occur in nearly all coefficients when log a

is added to the variables may be attributed,

perhaps, to the fact that the meteors for which

a can be determined are a selective group,

which cannot be directly compared with the

average small-camera meteor. When x is

added to the variables, the coefficients again

change appreciably; this time the cause must

be sought in the relatively small range of x

and in its relations with mass and velocity.
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 17

Under such conditions it would be imprudent

to draw any conclusions from these solutions.

If anything, they can be considered an object

lesson in the danger of applying a least-squares

analysis to a nonhomogeneous material when

the variables are anything but independent,

and a justification for the laborious photographic program with the Super-Schmidt cameras. We shall limit ourselves to pointing out

that the large discrepancy between the theoretical and the observed values of a, the coefficient of log vm, in the beginning heights is

found again here, just as for the Super-Schmidt

meteors, when we consider only the solutions

with the first three variables. When <r and x

are introduced in the solution, the discrepancy

becomes smaller, but there is reasonable doubt

that these solutions are really representative.

More significant is, perhaps, a comparison

of the observed values of c0 with those obtained

from theory. Since the average values of most

parameters, especially those of the mass, for

small-camera meteors are considerably different

from those of the Super-Schmidt meteors, we

shall use here a different "standard" meteor,

for which the parameters are as follows: va =30

km/s; log cos Z B =-0.2 ; log moo=0.77; log a

= — 11.52; x = 0 .

For the beginning heights we shall assume that the plate limit is —1 magnitude

(photographic) (see below). As we can see, the

agreement is quite good. From these data we

derive a trajectory length of 30.0 km, which is

97 percent of the theoretical length. Since the

limiting magnitude of the photographs cannot

be determined with any degree of accuracy (it

varies as much as two magnitudes for different

cameras in different locations), this last comparison must be taken with more than a grain

of salt.

e. Position of maximum light

The relative position of the maximum light on

the trail can be described by the parameter F,

defined as:

H

(km)

mjg)

FIGURE 5.—Average observed heights of all Super-Schmidt

meteors for: a, velocity groups; b, mass groups.

HB—HMI

HB—HE (27)

The observed values of F range from 0.032

(abrupt meteor) to 0.965. The distribution of

F is plotted in figure 6. The average value is

0.65±0.01. According to the data of table 4,

the theoretical value of F for the standard

meteor should be 0.684. According to the same

Beginning

Co

theor.

-8.76

93.1

obs.

-8.79

93.4

Maximum light

theor.

-7.85

81.9

obs.

—7.75

80.6

End

theor.

-7.28

73.7

obs.

-7.33

74.5
18

SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

100

80

No. 60

40

20

n

i i i i

-

i i i i

0.2 0.4 0.6

F

0.8 1.0

FIGURE 6.—Frequency distribution of F, the fraction of the

trajectory corresponding to the position of maximum

light, for all Super-Schmidt meteors.

table the observational value is 0.697.4 We

should recall that the observed F always refers

to the actual maximum light even if it occurs

in a flare.

The average value of F has been computed

for two of the principal showers, the Geminids

and the Southern Taurids, which are known to

differ rather widely in the physical characteristics of their members. The position of the

maximum light proves, however, to be near to

that of sporadic meteors (see table 7.1). For

abrupt-beginning meteors, the maximum is, of

course, much closer to the beginning. However, some of the A meteors reach their maximum light after the initial burst at a normal

position in the trail. For the standard smallcamera meteor FOb* is 0.68, while the theoretical

value of F is 0.58. This reflects the greater

frequency of flares toward the end of the

trajectory in bright meteors.

Table 7.2 shows F as a function of velocity.

As we see also in figure 7a, F slightly increases

with increasing vm. The result of a least^squares

solution (va in km/s) is F= (0.64±0.01) + (0.0016

± 0.0006) (vm—30). The solution is not fully

' The difference from the average value of 0.65 is essentially due to the

adequate; the figure shows that between about

dF

10 and 40 km/s we have -r-, =0.03 ±0.01,

d log va

dF

while -n a 0 when vm ">40 km/s.

d log vm

Table 7.3 shows Fa s a function of log a.

With the exception of the first point on the side

of small values of a there is a smooth decrease

of F with increasing a. The least-squares solution yields F=(0.62±0.01)-(0.177±0.034)

(log (T+11.0). However, between about —11.4

and —10.7 a better approximation (fig. 7c) is

F=0.61-0.32 (log cr + 11.0).

Finally, table 7.4 shows Fa s a function of the

fragmentation index %• A least-squares solution yields F= (0.67±0.01)-(0.065±0.032)*.

Tables 7.2 to 7.4 and figure 7 do not actually

represent the behavior of F as a function of vm,

<r, and x because of the well-known intercorrelations between these parameters. The actual dependences can be found from tables

5.1.1 to 5.6.4 for meteors having standard values

of all the parameters except the one that in each

case is the variable.

0 7

0.6

n «i

-

i I \ I

i •

I -

0.2 Q3 0.4 0.5 0.6 0.7 0.8

X

j

I —I r~

i

>

i

i 1 1 —

i

— i — •

_ /HB-HML\ HB-HHL

difference bet ween F= I I and .

\HB-H.J HS-H.

-11.6 -11.5 -11.4 -11.3 -11.2 -III -11.0 -10.9 -10.8

C log o- (cmV)

FIGURE 7.—The position of maximum light as a function of:

a, velocity; b, fragmentation index; c, ablation coefficient.

(F is the fraction of the trajectory corresponding to the

position of maximum light. All Super-Schmidt meteors.)
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 19

From the analysis we can draw the following

conclusions:

1. F varies strongly with velocity proceeding from 0.51 for 18 km/s to 0.86 for 68

km/s. The average value of

dF is about

d log va

0.6 (compared with 0.03 quoted above). Recalling that for 30 km/s Fis 0.70, it is clear that

the increase of F with log va is not linear and

becomes slower at high velocities.

2. F strongly increases with increasing

mass, from 0.37 for mo,=0.03 g to 0.77 for

ma,=8.3 g. Also in this case the relation between F&nd log mm is not linear and the increase

slows down for large masses. The average

dF value of

d log

is about 0.15.

3. F increases with increasing cos ZR; it

is 0.6 for cos Z«=0.25 and 0.71 for cos Zfl=0.95.

dF

Average value of TT ^-«0.15.

d log cos ZR

4. F decreases with increasing a for log a

> —11.2; in the range from —10.8 to —11.2

JP

we have -r\ =—0.25. For values of log a

d log a

smaller than about —11.2, F is constant.

5. F is independent of x- It is interesting

and a little surprising to find that the degree

of fragmentation does not on the average affect

the relative position of the maximum light.

/. Duration

The duration of a meteor is clearly given by

D==HB—HB

(28)

~v cos Zs

where v is the average velocity between the

heights of appearance and disappearance.

Both the theoretical and the observed durations

can be expressed in terms of the meteor parameters by means of equations (17) and (20),

or equations (23) and (26), recalling that HB—

HB=Hp(lnpB—lnpB), where Hp is the average

density scale height. We have

Dob,=

Hllnll (-16.26+2.1 log 0.+O.65 log mm

v cos ZiR

+ 1.2 log cos ZR—0.4 log <r-0.3x) (29)

and

H

v cos

+log cos Z*-log Ilim). (30)

Equation (29) gives approximately the dependence of the duration on velocity, mass,

zenith angle, and other parameters. Equation

(30) has been used to provide a comparison

with the observed durations.

The observed durations range from 0!l7 to

3!84. The standard meteor should have a

theoretical duration of 1*13, while the observed

duration is, according to table 4, only 0!76, i.e.,

67 percent of Dth. The average duration of all

Super-Schmidt meteors is 0?79±0.02.

The average ratio of durations 77^ is 0.61

±0.01. The two extremes are, respectively,

0.129 (A meteor) and 1.178. Table 8.1, which

shows the average ratio for several characteristic

groups of meteors, also contains the differences

AH between observed and theoretical heights.

The theoretical heights are obtained by equations (17) and (20) with the following numerical values: C=4.01 c.g.s. units; TOP=10~19

c.g.s. units; /Hm=10-°-4a'»-; Mitm=Mpm+AM=

effective plate limit. For AM see the explanation to table 1.1.

For obvious reasons, S meteors have the

lowest mean value (0.35) of 77^- Also A

meteors are, on the average, much shorter

than required by theory (TJ^=0.4 5 V In this

matter, no difference is found between shortand long-period meteors. Shower meteors appear to have a duration a little less anomalous

than sporadic meteors.

Table 8.2 shows the ratio of durations for

groups of increasing velocity. With the exception of the first group, the meteors have a

tendency to become shorter than expected

when the velocity increases (fig. 8a). The

discrepancy between observed and theoretical

beginning heights increases strongly with v^,

while AHML and AHB remain practically

constant.

Table 8.3 and figure 8b show 77^ as a function

of the mass. There is no significant dependence of this quantity on mass. The discrepancy between observed and theoretical

beginning heights increases with mass, while

AHML and AHB do not vary much.
20

SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

The ratio of the durations decreases rapidly

with increasing <r (table 8.4, fig. 8c);

A— ( Um ) is about —0.25. From equations

log<T\Dth/

(29) and (30) we can compute ^ .

he numerical agreement

dlog

cos ZR

turns out to be quite good.

A similar decrease occurs in -yp1 when

Lfth

increases (table 8.5, fig. 8d). We find ^ 0

«—0.2, in agreement with the expression

d_ /D£i!\-0.mnl0 tha t ean ^ obtame d

dx\DthJ DthvcosZR

by equations (29) and (30).

The values of AHB and AHML increase in

modulus with both <r and x- The dependence on

a is stronger, and HHB does not vary appreciably.

Table 8.6 and figure 8e show -j^ as a function

Lfth

of Cc (it is almost a constant). A rapidly increasing discrepancy of AHB between observed

and theoretical heights is shown, while AHML

and AHg are nearly constant.

Among the showers, the Southern Taurids

have an average value of -77^-*=0.84 ±0.02 and

Lfth

the Northern Taurids have §p=0.7 7 ±0.05,

rather high values, as could have been expected

from less fragmenting objects. Also, three a

Hydrids have a high value of §p-' :0.87±0.10.

On the other side, a single Draconid has

^-'=0.18; a Leonid has §p-'=0.44, and the

Uth Lfth

5 Aquarids have §f^=0 .

The average difference AH2.5 between observed and theoretical heights at magnitude

2.5 is peculiar for each shower. For details on

the peculiarities of individual showers, see

section 10.

5. Decelerations

Before the systematic use of rockets made it

possible to measure atmospheric densities and

pressures at high altitudes, meteors provided

a

20 30 40 506070

voo(km/s)

-11.6 -11.4 -11.2 -11.0 -IO.8

log a- (cm2s

2

)

/obs

0.2 0.4 0.6 0.8 1.0

FIGURE 8.—Ratio DO4,/D<k of the observed and theoretical

durations of all Super-Schmidt meteors as a function of:

a, velocity; b, mass; c, ablation coefficient <r; d, fragmentation index x; e, brightness.

the only means for deriving atmospheric densities at heights between roughly 50 and 100 km

(Whipple, 1943; Jacchia, 1948, 1952). Now

the approach can be reversed, and we can assume

the atmospheric densities as known and can try

to derive some information on the meteor

process. Although the mean atmosphericdensity profile can be considered as sufficiently

well established in the meteor region, we can

still use meteor decelerations to test the presence

of seasonal fluctuations in the upper atmosphere.
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 21

A similar analysis had already been made

earlier by Jacchia (1957a), who used 178

Super-Schmidt meteors. He also searched for

the presence of lunisolar tidal oscillations in

the atmosphere; the results showed no evidence

of such oscillations, and we shall not attempt

to repeat this part of his analysis. We will

follow here essentially the same procedure of

investigation.

From the drag equation, we have

log p,6,=log (—v) +% log ra—2 log v—log C.

(31)

To correct all the observed values of the

atmospheric densities for the effects of fragmentation, we introduce the fragmentation

index x and reduce log p^, to a given point on

the trail where s=s0. We have thus

log Pearr = l0g p«*,—x(» —S0)- (32)

For each deceleration we can define A log pC0TT as

A log pe0rT = l0g pCorr —log pT, (33)

where pT is the atmospheric density corresponding in the U.S. Standard Atmosphere 1962

(1962) to the height where the meteor had

velocity v, acceleration v, and mass m. For

each meteor we will define A log pcorT as

(34)

where k is the number of decelerations determined for the meteor and pt is the weight of the

i-th deceleration given by

*=l o<Fr>('

l

'-3)1(0"'

 (35)

where p.e.i is the probable error of the deceleration vt

, nt is the number of segments used in

the computation of vit and $(x) is defined as

*(*)=K[l+erf (2.5 log z-2.1)]. (36)

(

TO Y / 2 • —- I is introduced to decrease

the importance of decelerations near the end of

trajectories, where fragmentation might be so

severe as to make a correction meaningless.

In the analysis of fragmentation effects we

have not used this factor, of course; see, for

example, equation (37).

We will select the value of s0 in a way that

the scatter in A log peorr reaches a minimum.

First, a preliminary analysis is necessary to

eliminate the meteors that display clearly

anomalous values of A log peorr. In doing this

we have assumed so=O from the results of

Jacchia's (1957a) analysis. We have used all

the Super-Schmidt meteors with the exception

of (1) nine meteors without decelerations; (2)

three meteors without x; (3) 20 Geminid

meteors known to give systematically smaller

values of A log pe0TT (Jacchia, 1952); (4) three

Draconid meteors known to give very high

values of A log pC0TT (Jacchia, 1956); (5) meteors

nos. 3037, 8215, because of their uncommon

values of x, respectively +2.97 and —0.85.

As a result of this preliminary analysis, we have

eliminated from the final analysis 26 more

meteors

 5 whose values of A log pC0TT differed

from the overall average more than twice the

standard deviation of an individual meteor with

average weight. We are thus left with 350

meteors.

We now can find the value Som that minimizes the scatter in A log pwrr, i.e., the quantity

?=SX<(Alogpwrr<-

where

and

N'

(37)

N' is the total number of decelerations of our

350 meteors (iV'=1168). It is easy to find the

analytical expression of sOn:

AT'

• Nos. 3288, 3651, 5273, 5370, 6429, 6961, 7002, 7052, 7067, 7609, 7188, 7734,

7946, 8054, 8147, 8192, 8294, 8415, 8668, 9284, 9833, 9955, 10064, 10173, 10279,

10480. Many of them have large negative values of A log pc#Tr and are slow

or very slow meteors.
22

SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

where

At=A't-A';

N'

S X,

^'<=logpo6, <—logpr<—XiS(. (38)

Here, obviously, x, is the same for all the

decelerations pertaining to the same meteor.

10 100

0 (o. u.)

1000

FIGURE 9.—Average residuals A log peOrr as a function of

the aphelion distance Q: a, natural values; b, logarithms.

[The broken line represents correction applied to A log peor r

in equation (42).]

The result is: sOm=0.05±0.03 and r) is given

by i7=constX(l—O.13so+1-21^). The solution found by Jacchia (1957a) was *0in=0.00

and 7?=constX (l+0.96sJO for 121 meteors.

There seemed to exist a dependence of sOm on

the average fragmentation index of the group

of meteors used to find sOm itself. To reveal

this dependence we have taken 78 meteors

with x comprised between —0.07 and 0.07 and

combined them, in succession, with four

groups of meteors divided according to xSolving for s0 in the same manner as before,

we obtain:

meteors with x ^ 0 : sOm= — 0. 20;

meteors with x^0 . 2 : sOm= —0. 01;

meteors with 0. 2>x<0.4:s O m = 0.07;

meteors with x>0. 4 : sOm= 0. 10.

As we see, the dependence of sOm on x is not

very strong. We will adopt, henceforth, sOm=O.

We will then choose C such that

log Peerr r=0. (39)

Here, AT is the number of meteors (Ar=350) and

wr is the weight of the r-th meteor defined by

\l/2

H S N •

The result is

log G= 0.603 ±0.012. (40)

According to the classical theory of meteors, G

is given by MCnAoPn2'

3

, where CD is the drag

coefficient, Ao the shape factor, and pm the

density of the meteor body. For the SuperSchmidt meteors we can assume CD=2.2,

i.e., the value of CD in free molecular flow. For

a sphere we have 4, = (9ir/16)l/8=1.21. For any

shape other than spherical, if we have random

orientation, Ao will have a somewhat larger

value. Here we shall assume with Whipple

(private communication) that for the average

meteor Ao—1.5. Accordingly, the average

meteor density turns out to be

Pm=0.26 ±0.01 g cm' (41)

Before we study the seasonal variations of

the atmospheric densities, it is necessary to

apply another correction to A log pcorr (and to

A log peorr) due to the variation of A log pcorT

with the aphelion distance Q. Jacchia (1958,

1963) showed that the beginning heights of

short-period meteors are lower than those of

long-period meteors having the same mass,

velocity, and zenith angle. Verniani (1964a,

1964b) found that meteors in elongated orbits

have a lower density than those in short-period

orbits. This difference is probably caused by

the fact that large, loosely assembled meteor

bodies have a greater probability of being disrupted in interplanetary space (by collisions,

solar-wind erosion, and thermal effects) when

they are in short-period orbits. We can, therefore, expect an increase of A log pt0TT with

increasing Q. This is what we find on the

basis of table 9 and figure 9. Accordingly, we

have considered the quantities A log pt0Tr

defined by

Alogpeorr+0.053

when <2<4

 a

-

u

-

Ai * _ U log Pcor,+0.053 (5-Q) A log P

A log peorr—0.053

whenQ>6a.u. (42)
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 23

A similar relation defines also A log p*0TT. We

have correlated the values of A log p*0Tr with

the height H and the values of A log p*0Tr

with the mean velocity vm (the velocity at the

trajectory point where s=0) to check their

independence from these quantities. The following correlations were obtained:

d log v

-=—0.051 ±0.063 (vm in km/s)

and

inkm).

We have also computed

where

The result is

dH

rr.. .

dH

There is no appreciable difference from the

previous result in which individual decelerations

were used. These derivatives can be considered satisfactorily insignificant. Jacchia

(1957a) found for them values much closer to

zero; this was due to more restricted conditions

that the meteors accepted for the analysis

had to satisfy.6 Tables 10.1 and 10.2 show,

respectively, average values of A log p*0TT and

of A log p*0TT as functions of vm and H. Table

10.3 shows A Jog P*OTT as a function of H. The

data are also plotted in figures 10a and 10b.

The dependence of A log p*0TT on vn is

negligible.

The dependence of A log p*0TT on the height

H is very interesting. Between 85 and 103

km there is no dependence of A log pforr on H.

Below 85 km, A log p*0TT decreases steadily

when the height decreases. This should be

'He used also a somewhat different procedure; weights were not

employed and the corrections for Q not applied. Our data may be

slightly OYercorrected at values of Q>20 a.u., and this explains the

negative value of

due essentially to the deeper penetration in

the atmosphere of denser bodies. Here apparently lies the principal obstacle to the

determination of atmospheric densities from

meteoric decelerations. The same phenomenon

also precludes the possibility of effectively

determining the exponent n of the luminosity

law TV= TOpv

n

 from an analysis of the systematic

trend of the residuals A log p with height. If

we consider only meteors with |x|<0.2 and

vary n we find that dA log p^0TT/dH vanishes

-0.4

FIGURE 10.—Average residuals A log p^, as a function of:

a, velocity vm corresponding to the point at which the

meteor has lost half of its mass; b, H, the average for each

meteor of the heights for which decelerations were

determined.

when n«3 . We would not, however, attach

any importance to this result; we would rather

refer, in this connection, to the derivation of

n by Verniani (1964a, 1966) using other methods.

We have further analyzed the 350 meteors

by least squares for a possible seasonal variation in the atmospheric densities. The

equation of condition is

(35^24

where t is the time in days, a is the semiamplitude of the oscillation, and <A> is the phase

angle. The weights w have been employed.

The result is

a=0.026±0.016

A log P*COTT=<* sin (

d lOg Vm
24 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

The semiamplitude is about 0.03, less than three

times as large as its probable error; the amplitude of the seasonal variations is then about

14% in the natural value of the density.

The phase angle puts the maximum on September 16 with a probable error of 27 days.

The same amplitude was found in the preliminary analysis of Jacchia (1957a), which,

however, gave a maximum on August 7 with a

probable error of 35 days.

If we exclude from the analysis all meteors

with x>0.40, we are left with 267 meteors and

we obtain

a=0.029± 0.021

.«,= —133°±37°,

i.e., essentially the same amplitude, but a

maximum on August 14. This solution is

probably the better of the two.

These variations refer to a height corresponding to the average value of H, which, according

to table 10.3, is 91.0 km. This height practically coincides with that of a well-known

isopycnic layer in the atmosphere, and this fact

explains the small amplitude of the observed

effect.

6. Magnitudes and "color index14

a. Magnitudes

According to classical theory, the maximum

photographic luminous intensity 1^ is given

by (Verniani, 1961)

6£

W

 C0S

where

vm=velocity at the point of maximum

v= velocity at an intermediate point

between beginning and maximum

light,

Hp=pressure scale height (at maximum

light),

By assuming for v an intermediate value7 be7

 - ; T 6 , 11 1i/«

»-Vr«r.-»oD l+-j - in r±r.\

tween vm and t^, adopting the usual value of

TOp, and expressing the other parameters in c.g.s.

units, we obtain from equation (44) a theoretical

expression for the maximum absolute magnitude

of a meteor as a function of its parameters:

M^ =45.56 —10 log »«,— 2.5 log m*

—2.5 log cos Zfi+2.5 log HP

-5log/+7.5log (1+2/)

(45)

On the basis of equation (45), it appears

reasonable to assume for the actually observed

Mpm a dependence on the meteor parameters of

the form

Mpm=k<i+ki log v log mm+k3 log cos ZB,

(46)

and then find the values of the constants k0,

k\, ki, k3 by least squares. To avoid the effects

of the correlation between m. and ^ we have

also tried to use a simpler equation of condition

that did not contain the mass; however, the

dependence of Mpm on mass is so clear-cut that

it cannot be ignored. Consequently, a solution

that omits the mass does not have any

meaning.

The results of the least-squares solutions with

the condition equation (46) are listed in tables

11.1 to 11.6. Just as in the height analysis (section 4), the absolute term k0 does not represent

any realistic magnitude unless we subtract from

each variable a constant close to its mean value.

As before, we have taken the following constants: fla.=30 km/s, m«,=0.3 g, log cos ZR=

—0.2. For a meteor with these characteristics,

equation (45) gives 214^=0.63; this is the theoretical value of kQ, which should be compared

with the least-squares results of tables 11.1 to 11.6.

An inspection of table 11.1 shows at a glance

that for Super-Schmidt meteors k0 is in all cases

smaller than 0.63; i.e., the observed maximum

brightness is greater than its theoretical value.

The other coefficients, ki to k3, are all smaller

in absolute value than their theoretical counterparts; in other words, the observed dependence

of Mpm on the three parameters of equation (46)

is smaller than predicted.
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 25

For the sake of comparison we have also included in table 11.4 the results of similar leastsquares solutions for small-camera meteors. If

uncritically accepted, these solutions would indicate that for small-camera meteors the dependence on the three basic parameters is closer

to theory than for Super-Schmidt meteors.

This agreement, however, must be considered

fortuitous and caused by the presence of big

flares in more than one-third of the small-camera meteors. If we exclude from the analysis

the 80 meteors that had flares brighter than

0.5 magnitude above the general light-curve

level, we find that the results agree with those

from Super-Schmidt meteors.

One of the major differences between .SuperSchmidt and small-camera meteors is to be

found in their respective mean value of %• The

fact that the two groups do not behave too differently regarding the maximum brightness and

its dependence on the basic parameters would

indicate that x is

 n ot very important in determining Mvm. This can be confirmed by dividing the sporadic Super-Schmidt meteors

(classes A, S, and D excluded) into two groups of

Xi one with x—0.2 and the other with x>0.2,

and comparing the solutions (table 11.2). On

the other hand, we see from table 11.2 that all

coefficients are appreciably affected by differences in a. The few Super-Schmidt meteors

with log <r< —11.4 show much better agreement with theory than those with larger <r. It

should be remarked that, while it looks as if x

is less important than a in modifying the coefficients ki to k3, it is only a little less efficient than

a in modifying k0, i.e., M^ itself. From the

various solutions for groups of a and x we obtain

dMpm/d log <r=-0.70 and dMpm/dx= -0.45.

Since the standard deviations of a single observation, for Super-Schmidt and smaD-camera

meteors combined, is ±0.28 in a and ±0.29 in

X, we see that the effect on Mvm of the observed

scatter in x is about two-thirds as large as the

effect of the scatter in <r.

Since it is a matter of geometry, we might

expect to find a simple proportionality between

Iprn and cos ZB(I~m~pa

r

^'COs ZR). Instead

we find a value of — k3 remarkably smaller than

2.5. This could be due to the correlations,

owing to selection, that affect all the principal

quantities. The smaller values (in modulus)

of ki and ki could be due to this anomaly in k3.

Therefore, we have computed another leastsquares solution, postulating k3 — — 2.5. The

results are practically the same as before, with

a small improvement in the case of the SuperSchmidt meteors that can be considered

negligible. Table 11.6 shows these results in

some detail, for both Super-Schmidt and

small-camera meteors. It becomes clear now

that the deviations from theory of the values of

ki and ki do not depend on the anomalous value

of k3. Even the standard deviations are the

same in both cases.

From the results of table 11.1 we can obtain

the empirical dependence of / ^ on mass,

velocity, and zenith angle. On the average, for

Super-Schmidt meteors we find, in c.g.s.,

7^=7.3X10 cos0

(47)

Introducing magnitudes, we have

Mpm=55.34—8.75 log »„— 2.25 log TO*.

-1. 5 log cos Zs. (48)

According to equation (48) the initial mass of

a zero visual magnitude meteoroid (color

index = —lm86) with a velocity of 40 km/s and

a zenith angle of ~50° (log cos ZR=— 0.2) is

0.76 g. Previously, and using the same value

of TO as here, Verniani (1964a) had found

for such a meteor a mass of 0.84 g. His computation was based on the relationship between

luminous intensity and integrated brightness

empirically derived by Jacchia (1958) that

we can now improve by means of equations

(47) and (48). We have

(49)

V J * cos2/3

or in logarithmic form,

e.=5.29-0.89 log ^-0.44 4 Mvm

- f log cos ZK. (50)

These equations hold approximately also for

nonflaring small-camera meteors and for

Super-Schmidt and nonflaring small-camera

meteors taken together (table 11.5). Table

12 shows the mass of a zero visual magnitude
26 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

- 3

- 2

- 1

0

• 1

+2

1 1

•

-

15 20 50 40 50 60 70

vjkm/s)

1.4

1.2

1.0

0.6

0.4

0.2

• c

-

-

• T

I"

I-

/*.

X

-

-

-

0.3 0.4 0.5 0.6 0.7 0.8 0.91.0

CosZ,

-9

-8

- 7

- 6

- 5

- 4

- 3

- 2

-1 i t i i

•4

i

i

-

-

-

m.(g)

04 05 06 07 08 09 IC

Cos ZR

FIGURE 11.—Photographic magnitude: a-c, Super-Schmidt meteors reduced to: a, wioo=0.3 g and cos ZR=0.6 3 as a function of

velocity; b, t»«D=40 km/s and cos ZR=0.63 as a function of mass; c, 0,0=40 km/s and woo=0.3 g as a function of zenith angle

of the trajectory, d-f, Small-camera meteors reduced to: d, ma= 10 g and cos Z*=0.63 as a function of velocity; e, vm=^

km/s and cos Z«=0.63 as a function of mass;/, peo=40 km/s and «„ = 10 g as a function of the zenith angle of the trajectory.
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 27

meteoroid as a function of initial velocity and

zenith angle. As we have seen from the

results in table 11.4, different relationships

hold for all small-camera meteors:

/^.=5.0XlO-28^

0TM1

,

0

 cos07 ZR (51)

Mrw=63.26—10 log va—2.5 log m^

—1.75 log cos ZR (52)

00 (53)

 vm cos0-

7

 ZR

e.=7.44—log t?,—0.4M,TM—0.7 log cos ZR. (54)

From equation (52) we obtain mo, =0.60 g for a

zero visual magnitude meteor with »«, =40 km/s

and log cos ZR=— 0.2. This result is less

reliable than that obtained from Super-Schmidt

meteors owing to the nonhomogeneity of the

observational material and the difficulty of

eliminating flares.

Because of the observational correlations

between mass, velocity, and zenith angle, it is

useless to consider the functions MPm(t'a,),

A^j>m(tfia>), MpmiZft) directly derived from the

observations, unless we reduce them to constant

values of the other two variables. This can be

done by means of equation (48) for SuperSchmidt meteors and of equation (52) for smallcamera meteors. Table 13.1 shows Mpm as a

function of the velocity for Super-Schmidt

meteors reduced to moo=0.3 g and log cos ZR=

—0.2. The results are plotted in figure lla.

Similarly, tables 13.2 and 13.3 show Mpm as a

function, respectively, of the mass and of the

zenith angle; in the first, the observed absolute

magnitudes have been reduced to vm =40 km/s

and log cos ZB=—0.2; in the second, to »«=40

km/s and m« =0.3 g. These results are plotted

in figures lib and lie. Figure ll a also clearly

shows the small systematic difference in brightness between low- and high-velocity meteors

due to the difference between short- and longperiod meteors. Long-period meteors are

roughly one-fourth to one-half magnitude

brighter than short-period meteors.

Tables 13.4 to 13.6 and figures lld-f show

similar results for small-camera meteors. The

only difference is that they have been reduced

to m. = 10 g instead of m«,=0.3 g.

The discrepancy between observed and theoretical magnitudes has been investigated for

both Super-Schmidt and small-camera meteors.

The differences ^Mpm=Mpm—M

(

* for sporadic and shower meteors are listed in tables

14.1 and 14.2. At first glance it may be surprising that the average values of AMp^ for

Super-Schmidt and small-camera meteors

should be roughly the same. Actually, the

presence of big flares completely distorts the

results for small-camera meteors. When there

are no flares, the observed magnitude of a

small-camera meteor is often close to the

theoretical value, while flares can produce a

difference of as much as three magnitudes.

The average value of AM^, is —0.3 ±0.1

for meteors with flares smaller than 0TM5 and

— 1.0 ±0.3 for meteors with flares greater than

0TM5. These figures indicate a good agreement

with theory; a small flare of 0TM3 occurs quite

often in the smoother light curves. The discrepancy is much more systematic for SuperSchmidt meteors; this is shown also by the

smaller value of the standard deviation of one

observation, 0.50 instead of 0.76. Among the

showers (Super-Schmidt) the Taurids show a

very small value of AM,TM. The same is true

also for a Hydrids and for Lyrids, but these two

showers have only three meteors each on our

list. Geminids also show a moderate value of

AM^. On the other hand, the 5 Aquarids are

about one magnitude brighter than the theoretical value. The Draconids, of course, are

very anomalous. As a curiosity, the only

member of the Leonid shower contained in our

list appears less bright than predicted by

theory. Among all meteors only 27 have a

positive AM: among these, 12 are sporadic, 5

are Taurids, and 5 are Geminids.

The departure from theory appears to be

greater for short-period meteors than for those

in long-period orbits.

The difference AMpm turns out to be independent of mass, velocity, zenith angle, and

height. There is, however, as we expected, a

clear-cut dependence on the fragmentation

index x> shown in table 14.3. The smallcamera meteors do not show such a correlation,

but those having all the data for computing

M^m are too few and the flares are present

also among meteors with a value of x close to
28 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

zero. We can also see that those SuperSchmidt meteors that do not show progressive

fragmentation are about half a magnitude

brighter than expected on theoretical ground.

b. "Color index"

Visual estimates of brightness were recorded

for 390 out of the 413 precisely reduced SuperSchmidt meteors. For these 390 meteors we

can compare photographic and visual magnitudes and analyze the difference between the

two, the so-called "color index." A previous

analysis of the color index (Jacchia, 1957b)

covered 336 of these same meteors, or about 86

percent of the present material. The present

analysis is conducted along the same line as

the previous investigation, and the numerical

results are essentially the same. We refer the

reader to the aforementioned paper for a description of the techniques used to derive photographic magnitudes to be compared with the

visual estimates. Here we shall simply repeat

that the emulsion used in the photography

was the blue-sensitive Kodak X-ray for the

Super-Schmidt meteors. For small-camera meteors it was mostly Cramer Hi-speed or Kodak

103a-o emulsion with spectral-sensitivity curves

similar to that of Kodak X-ray.

The analysis was made twice, first with all

the 390 meteors and then discarding the meteors

of classes A, F, and S (48 meteors). The results

are quite similar in both cases, and we present

here those obtained from all 390 meteors.

Table 15.1 shows the color index as a function

of the velocity (fig. 12a) and its distribution

for five velocity groups. Little dependence,

if any, is found on the velocity; C.I. = — 1.37

±0.04 for all velocities seems the best conclusion.

Table 15.2 shows the color index as a function of the absolute photographic magnitude

(fig. 12b) and its distribution for seven magnitude groups. In figure 12b we have plotted

also the dot corresponding to the mean C.I.

for small-camera meteors (Jacchia, 1957b).

The color index turns out to be almost a linear

function of the magnitude between Mpm= —1.5

and MPm=-{-l.O and can be represented by

constant value of about —1.0. For Mpm< —2

the color index is roughly constant and its

value is close to —1.95.

In its range of validity equation (55) is

equivalent to

MP=%M,-2M (56)

or to

MV=%MP+1.36. (57)

20 30

v.(km/s)

40 50 60 70

C.I.

• Super - Schmidt meteors

o Small camera meteors

<1.0). (55)

For fainter magnitudes C.I. seems to reach a

-08

-1.0

-1.2

-1.4

-1.6

-1.8

-2.0

-6 -5 -4 -3 -2 -I

FIGURE 12.—Color index as a function of: a, velocity for

Super-Schmidt meteors; b, absolute photographic magnitude for Super-Schmidt and small-camera meteors.

7. The ablation coefficient a

a. Dependence of the mean <r on the other

parameters

For all Super-Schmidt meteors, "instantaneous" values of a were computed from equation (11) from each observed deceleration.

In addition, equation (12) was used whenever

more than one deceleration from the same

plate was available on the meteor trajectory.

A mean value of a was derived for each meteor

on the basis of all these determinations; those

derived from equation (12) were given greater

weight in calculating the mean. Since a

generally varies during the trajectory, the

value obtained for those meteors for which

only one deceleration was available for each
ATMOSPHERIC TRAJECTORIES OF 413 MET30RS 29

film depends on the location on the trajectory

of the point to which the deceleration refers.

Therefore, a correction had to be applied to

make the a's of those meteors comparable

with those obtained mainly from the "integrated" equation (12). Let us suppose for a

moment that the only anomaly introduced by

fragmentation concerns i. From equation (10)

we should then have

v

<rT=<r—>

VT

when aT corresponds to the theoretical value

vT of the deceleration. We can assume that

<TT is approximately constant during the trajectory. Therefore, differentiating with respect to the mass-loss parameter s (equation

(14)), we have

d log <r d , » 0=—-2—1_ iOg __,

ds ds 6 vT

and recalling the definition of the fragmentation index x (equation (15)),

d log a

X. (58)

Since equation (58) suggests that there might

be a linear dependence on x, we have put

d log a (59)

and determined a and b by least squares for the

143 Super-Schmidt meteors with more than two

decelerations and thus several instantaneous

values of a. Each value of d log <r/ds was given a

weight As/D2, As being the maximum difference

between the values of s employed in the computation of the derivative and D the standard

deviation of the derivative itself. The result

was:a=-0.84±0.05;6=0.02±0.01. The correlation coefficient between d log ajds and x is

— 0.81. The average value of d log <r/ds is —0.09

± 0.01, in perfect agreement with the mean value

X=0.13 obtained from these 143 meteors. The

complete theoretical derivation of d log a/ds is

given in section 7b; here we are just concerned

with the correction to apply to the values of a

for the meteors with only two decelerations (or

less). Clearly these <r's must be reduced to a

225-636 O-67—3

standard value s' of s by means of equation (59).

The value of s' was determined as follows. For

each multideceleration meteor, there are available several instantaneous values of a, which

correspond to different values st of the mass-loss

parameter s. Moreover we have the average

value log a determined mainly through the use

of equation (12). From these meteors we selected the sporadic ones with x>0.15 or x<C —0.1

so that the corrections were greater than or

equal to 0.1. There are 59 such meteors and

for each of them a value «o has been computed

such that:

where k is the number of the decelerations of

the meteor and (log o-,),=^ is given by

(log <ri).-.£=log «r,+ («;-a,)

j

Then we computed JZ—~

n

Here, n is

the number of meteors with multiple decelerations (n=59). The result is 0.03 ±0.04. A

check on the reliability of this value was made

by computing the quantity 8i' that minimizes

the sum

where

A log ai =log ffi - £ JC Oog o-,),.,;.

We find si=0.07±0.04. On the basis of these

results we have assumed the round value

s'=0. The final log a for a meteor with two

decelerations is therefore:

(log<ri)t-0+X2

rj— _

where X< is the weight for individual decelerations, defined by equation (37).

The observed values of log a for SuperSchmidt meteors range from —10.42 to —12.02.

Meteors of the classes A and S have been

systematically excluded from the present analysis, as well as those meteors for which the

determination of a was deemed to be too

unreliable. Table 16.1 shows the distribution
30 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

of log <r, both for all meteors (fig. 13a) and for

sporadic meteors only. Table 16.2 and figure

13b cover small-camera meteors; a comparison

will 6how the difference in the two distributions.

It is known that a is a function of the velocity

and of the integrated brightness (Jacchia, 1958).

Tables 17.1.2 and 17.2 show the dependence of

<r on these quantities, both for all meteors and

for sporadic meteors only. The latter have

been also divided into two groups, Q<6 a.u.

-K>.4 -10.6 -10.8 -11.0 -11.2 -11.4 -11.6 -11.8 -12.0 -12.2

log <r (cmV)

20

15

No. 10

-10.6 -10.8 -11.0 -11.2 -11.4 -11.6 -11.8 -12.0 -12.2 -12.4

log <r {cm*s*)

FIGURE 13.—Frequency distribution of the ablation coefficient

a for: a, Super-Schmidt meteors; b, small-camera meteors.

1 I 1 1

b -

and (£>6 a.u.; there is no appreciable difference

in the behavior of log a for these two groups

(table 17.1.1 and fig. 14b). The apparent

differences between the values of log a for the

two groups in the same range of ea are due only

to the different mean velocities and masses of

the two groups. As was already known, a

decreases when vm or em increases. The variation of a with va is quite similar both for all

meteors and for sporadic meteors only (fig.

14a). The latter group seems more regular

since it is not affected by the peculiarities of the

individual showers. If we limit our attention

to sporadic meteors, we see that the decrease

of log a with velocity appears to be linear up to

about 40 km/s; thereafter a is roughly a constant

(around —11.33). From 15 to 40 km/s, we

have approximately log c— —10.24—0.65 log va

(v in km/s). A least-squares solution for the whole

range of velocity gives log <r=(—10.40±0.11)

— (0.51 ±0.07) log vm. If we also introduce

the mass as an independent variable, we

get log<r=(—10.29 ±0.13) — (0.63 ±0.1 l)logt>.

— (0.05±0.03) log ma.

As a result of selection effects, mass and

velocity are correlated, as is shown in table 2.1.

Therefore, the preceding solution has little, if

any, meaning. Moreover, this correlation

makes it necessary to correct the preceding

results. Since the brightness is not an independent variable, a must be regarded essentially as a function of mass and velocity:

a=ff(va>, m^). Table 17.3 shows <r as a function

of mass. It appears that for the Super-Schmidt

material a depends more on vm than on mm.

By using a method of successive approximation

we can find the values of <r=a(vai) at mm~

const and <T=o(mm) at va= const. These

functions are listed in tables 17.1.2 and 17.3

for the values mco=0.8 g and va =30 km/s. In

the reduction to moo=0.8 g of the uncorrected

civ^), the values of a of the small-camera

meteors have been very useful. The functions

(r(vm) at m^^const and <r(mm) at va>=const

have been determined by successive approximations also for small-camera meteors;

unfortunately only for 88 among more than

200 small-camera meteors has <r been determined. Tables 17.4 and 17.5 show results of

small-camera meteors, while table 17.6 gives

results of shower meteors, both Super-Schmidt

and small-camera.

Figure 14c shows <r(va) for Super-Schmidt

and small-camera meteors, for a constant mass

of 0.8 g. This value for the mass has been

chosen because it is the average mass for SuperSchmidt meteors and is still on the plateau

where a does not vary with mass (see below).

The results of the small-camera meteors do not

agree very well with those of the Super-Schmidt.

For the Super-Schmidt we can describe approximately <rasa function of vm as follows:
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 31

-11.0

~ - -M.8

~ -11.3

-11.4

- • All meteors

• Sporadic meteors

- * Coinciding

t-4-l

1 1If- If

T 1

a

•

40 50 60 70

-io.a

-10.9

-11.0

-ii.i

-M.2

-11.3

-11.4

-11.5

-11.6

-11.7

I -.1.4

b

° -M.6

-11.8

-12.0

1 1 r—

-

• • Super-Schmidt

o Smoll comera

i i •

1 1 1 1—

c

•

\ •

—i i i i

-ILO

-11.2

-11.4

-11.6

• 4

•

*

X Q > 6

• Q< 6

b •

(

t

L L , •

1

 1

30

v.tkm/5)

40 50 60 70

40 50 60 70

-11.0

-11.2

-»- 4

-11.6

-11.8

-12.0

i« j 4 7 *« nij ^

-

- • Super - Schmidt

° Smoll comera

1- f"

d .

•

mjq)

-

e

-

FIGURE 14.—Ablation coefficient as a function of: a, velocity for Super-Schmidt meteors; b, velocity for sporadic Super-Schmidt

meteors in short-period and long-period orbits; c, velocity for Super-Schmidt and small-camera meteors, reduced to standard

mass of 0.8 g; d, mass for Super-Schmidt and small-camera meteors, reduced to standard velocity of 30 km/s; e, brightness for

Super-Schmidt and small-camera meteors together; /, perihelion distance q for all Super-Schmidt meteors.

formm=0.8 g,

log <r=— 9.90—0.90log vm («;«,:<40km/s)

log <r= —11.33 (t?a>>40 km/s).

For the small-camera meteors an approximate

representation of aiv^) is:

for meo=0.8 g,

log cr=— 9.46—1.20 log vm.

Figure 14d shows <r(nia>) for Super-Schmidt

and small-camera meteors reduced to a velocity

of 30 km/s. In the overlapping region (between 1 and 10 g) the results of the SuperSchmidt agree very well with those of the small

camera. Average values of log <r for groups of

increasing mass for all meteors (Super-Schmidt

and small-camera) are given in table 17.7.

Between about 10"2 and 1 g there seems to be

no dependence of a on mass. A clear dependence is noticeable, however, between 1 and

about 70 g, at which point <r again becomes
32 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

practically independent of mass. Between

0.01 and 0.9 g, the results are well represented

by ( ^ = 30 km/s), log o-= —11.23 (0.01 On .

<0.9 g) for both Super-Schmidt and smallcamera meteors. When m is greater than 0.9 g,

a curve is more adequate than a straight line to

describe the function ^(m^); however, a rough

linear approximation is (voo= 30 km/s), log a—

— 11.24—0.23 logra,,, (0.9<mm<70 g); (t>.=

30 km/s), log <T= — 11.67 (70<ma)<1000 g).

Combining together these and the previous

results for a^vj) we find an approximation of

the function a{ma, va) [see formula (60)].

Table 17.8 and figure 14e show a^ ) for SuperSchmidt and small-camera meteors. These

results are quite similar to the previous ones

obtained by Jaccbia in 1958. Table 17.9

presents log a as a function of the zenith angle

ZR for Super-Schmidt meteors. We see that a

is practically independent of cos ZR. The same

conclusion is reached if we reduce the results to the same mass and velocity. Table

17.10 shows log <rasa function of the aphelion

distance Q; a decreases when Q increases, but

this is only the consequence of the variation of

Q with the velocity va, as can be seen from the

column that gives log <r reduced to a standard

velocity of 30 km/s. Table 17.11.1 shows log a

as a function of the perihelion distance q (see

also fig. 14f). It appears that log <r increases

rather regularly with q; again the slight decrease

of va with q contributes partially to this effect.

Table 17.11.2 shows log a versus q for shortperiod and long-period meteors.

Lastly, table 17.12 shows that a is, surprisingly, quite independent of x and vice versa.

This result is quite important for a better

understanding of the different meaning of a and

X- We cannot describe the behavior of a

meteor if we do not know both of these basic

parameters. For a discussion of the different

manner in which a and x may be related to

fragmentation, see section 8.

log a=

—9.90—0.9 log vm

—9.91—0.9 log vw—0.23 log ma

-10.34-0.9 log »„

-11.33

— 11.34—0.23 log mm

1-11.77

b. The variation of a along the trajectory

Although a turns out to be independent of x,

we have seen that fragmentation must be

responsible for the variation of a in the course

of the trajectory. We have seen also that in

first approximation d log a/ds is equal to — x

[equation (58)]. Let us now evaluate correctly

this variation. From equation (10) we have:

I — In (—7ti\

ds In 10 [_ds

ds ds J

Recalling the definitions of s [equation (14)],

X [equation (15)], and the drag equation (2), we

have also:

d j , • \ _ 1 F d2TM • dm s~|

c* —m\_ ds2 ds sj

d . 10'lnlO

ds 10*+1

- ^ ln(-vv) = -(ln

Moreover, we have

"T 1°£

1 dlnm 3dlnv

3 ds ds

ds

d?m —n,

ds2

(1O'+1)2

l(Bio*(foio)2

(i-io*)

(10*+1)3

—mam

(lnlO)m(ma—m)

( m . — m) —f m2 m I m2

•• _ \_mz m J m

"

S

 (^10) (m^—m)2 '

and from equation (3)

(»oo<40 km/s; 0.01<mo<0.9 g)

(»0O<40 km/s; 0.9 ^ m ^ 70 g)

(«<D<40 km/s; 70<moo<1000 g)

(»o>>40 km/s; 0.01<mm<0.9 g)

(wa>>40 km/s; 0.9<m^<70 g)

(»<D>40 km/s; 70<moo < 1000 g)

(60)
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 33

The expressions written above allow the determination of d log aids. Considering this derivative at the point s=0 (i.e., when m=^\

and indicating with the subscript 0 all the

quantities taken in the points s=0, we have

(Hp=pressure scale height)

\ ds +

3 <rovovo

(61)

We have randomly selected 12 meteors and

computed ( —-^— ) according to the preced-

\ ds /i=o

ing equation. The result,

was in good agreement with the least-squares

solution obtained before.

Using the 143 meteors with more than two

decelerations, we have searched for a dependence of d log a/ds on vm and log <r itself.

No dependence has been found:

=—0.008 ±0.002

= -0.01 ±0.13.

d log vm\ ds

d /d log

d log o- \ cfe

8. The fragmentation index X

Whenever several decelerations are available

along the trajectory of a meteor, X can be

evaluated directly from equation (15) by

plotting

A log po»,=log Pobt—log pr=log YT

against s and fitting the best straight line

through the points of the diagram. When only

one deceleration per plate is available, or the

different decelerations correspond to points too

close to each other, the value of x can be computed approximately by an equation that can

be obtained by differentiating the drag equation

and reads (Jacchia, 1955)

where Hp is the density scale height. From

equatioi

tion (3)

equation (13) we have ^-=k, and from equam

m + » r

V

3 dt

m m.

i - * * \ (62)

The fragmentation index x is zero when

-=-^) that is, when the relative rate of change

in the "dynamic" mass of the meteor coincides

with the relative rate of change of the "photometric" mass. It takes positive or negative

values according to whether the former is

larger or smaller than the latter. If a faster

rate of change of the dynamic mass is interpreted as due to fragmentation, x emerges as

a measure of the fragmentation process. It

should also be clear that x will always be

positive when the meteor is fragmented. A

negative value of x cannot be physically

justified any more than a negative meteor

deceleration. Negative values of x> however,

are much more frequent than negative decelerations. The negative values of x that are

occasionally observed must be ascribed to (a)

observational errors, (b) variations in the

atmospheric density profile, (c) systematic

errors in the standard atmospheric density

profile, (d) variations either in the shape of

the meteor or in the drag coefficient y (for

small-camera meteors, which on the average

are larger and lower; the latter is a distinct

possibility; for some of them there probably

occurs a transition from free-molecule to

continuum flow in the course of the trajectory),

and (e) the presence of a residual mass, which,

according to equation (6), is always assumed to

be zero.

Whenever fragmentation is present, a knowledge of x is necessary for the correction of all

the quantities computed by means of the

decelerations. This correction is made simple

by the near constancy of x during the observable part of the meteor flight. We have

employed x in ^ne analysis of the atmospheric

densities (as Jacchia already did in 1957a), in

the reduction to s=0 of all the values of log a,

and in the heights analysis. The determination

of the luminous efficiency TP by Verniani
34 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

(1964a) has been made possible by the knowledge of the fragmentation index. Otherwise,

the scatter in the computed quantities would

be so large as to make it impossible to draw

any meaningful and reliable conclusion. The

study of the correlations of x with the physical

parameters of meteors permits us to relate

them to the physical behavior of meteors in

the atmosphere; we will find, for instance, that

the relative degree of fragmentation is high for

small meteors and decreases when the mass

increases. It should be clear then that the

fragmentation index is an important characteristic of each meteor as well as an efficient

tool in handling the observed decelerations.

For a nonfragmenting body, the ablation

coefficient a is presumably a constant and x is

zero. In an ordinary, crumbling meteor, however, the meaning of <r becomes obscure and is

reduced more or less to a parameter of the

smoothed light curve. On the other hand, x

tells at a glance how much the presence of

fragmentation contributed to the discrepancy

between observation and theoretical behavior.

Differences in fragmentation must result in

different values of both a and x; each of these

parameters, however, reflects a different effect

of fragmentation. If a meteor keeps shedding

fragments during its flight, but maintains a

single main body, the ablation rate may become

noticeably larger than for a nonfragmenting

body, while the deceleration, which contains an

m~1/3 factor in its expression, may not be too

anomalous. The increased ablation rate, which

results in a greater a, will raise the maximum

brightness and the height at which it occurs.

In those cases when the disintegration of a

meteor is more complete, to the point where it

may become difficult to identify a main body,

x will generally be noticeably different from

zero and a will be even larger—although it is

conceivable that beyond a certain level of

crumbling a may not appreciably increase.

That this may actually be the case is suggested

by the comparison of the mean values of a and x

for all meteors as a function of €„ (figs. 14e and

16d; see also Jacchia, 1958, fig. 1), from which

it appears that, proceeding to fainter meteors,

a increases earlier than x and reaches a nearconstant maximum value long before x has

stopped rising.

An analysis of the fragmentation index for

most of these Super-Schmidt meteors has been

published earlier (Jacchia, 1958). It confirmed

the dependence of x on the integrated brightness

(Jacchia, 1955) and showed the existence of a

clear correlation between fragmentation and

zenith angle (x=0.5—0.27 cos ZR). It also

established a dependence of x on velocity and

suggested a difference of fragmentability between long-period and short-period meteors

(x near 0.30 for meteors with uaJ<C40 km/s

and x~0.38 for meteors with v~>40 km/s).

The present analysis repeats the earlier investigations in somewhat greater detail. The

present values of x are appreciably different

from those of the earlier investigations that

were computed on the basis of the ARDC 1956

atmosphere (Minzner and Ripley, 1956); the

values used in the present analysis have been

computed using the U.S. Standard Atmosphere

1962 (1962). The present values of x are, on

the average, smaller than the preceding ones;

the mean value of x was close to 0.32, while the

present average for all Super-Schmidt meteors

is 0.27.

The values of x for Super-Schmidt meteors

range from —0.85 to +2.97. The distribution

of x for these meteors is given in table 18.1 and

plotted in figure 15a. In figure 15b (see also

table 18.2) we have plotted also the distribution

of x for small-camera meteors. In the following

general analysis we have not used all the 401

Super-Schmidt meteors for which a value of

x was computed; the meteors of classes A

(abrupt beginning) and S (flarelike meteors)

have been excluded from the general analysis

and studied separately. We have also excluded

four meteors whose values of x were quite

exceptional (meteor no. 8215: x = — 0.85; no.

8817: x=l-73; no. 8951: x=2.46; no. 3037:

x=2.97). [Meteor no. 8951, however, a member of the Draconid shower, has been used to

determine x for the shower itself in table 19.7.]

We are, therefore, left with 359 Super-Scbmidt

meteors, 249 of which are sporadic. We have

also 58 values of x for small-camera meteors;

since a comprehensive analysis of these data

has never been made; it seemed proper to do it

here. Though they are quite few, these smallcamera meteors provide a useful basis of com-
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 35

parison with meteors of much larger mass and

greater brightness.

Table 19.1.1 shows the dependence of x on

the velocity both for all Super-Schmidt meteors

(fig. 16a) and for sporadic Super-Schmidt

meteors. We see that the trend is irregular.

Meteors with v<40 km/s have a mean value

of about 0.22, while fast meteors (y>40 km/s)

have x~Q33 o n the average; however, most

of this otherwise remarkable difference appears

150

100 -

No.

50 -

-I

a

- i

20

N o ' . o

V

-0.6 0 0.6

X

-

-

FIGURE IS.—Frequency distribution of the fragmentation

index x for: a, Super-Schmidt meteors; b, small-camera

meteors.

to be due to the different mass distribution of

the two groups. Table 19.1.1 also lists mean

values of x reduced to a mass of 0.8 g. If we

take these values, we find the average values

of x to be respectively 0.23 for slow meteors

and 0.26 for fast meteors, with a difference

roughly equal to the standard deviation of the

second value alone (sum of standard deviation

of both groups =0.05). For sporadic meteors

we have:

fl«,<40km/s, mean x=0.23±0.02,

(mean x)mOD-o^g=O.24

©«,>40 km/s, mean x=0.30±0.03,

(mean x)ma>=o.8«=O.23.

There is no difference here between corrected

averages. It therefore seems that in the mass

range of the Super-Schmidt meteors, x is

independent of velocity. However (see table

19.4), x shows a clear decrease with velocity

for small-camera meteors, being equal to

0.07 ±0.04 at ©. = 15 km/s and to —0.12 ±0.04

at 0=57 km/s. Values, corrected for mass

dependence, are, respectively, 0.08 and —0.18

(at ra«,=30 g). Table 19.1.2 lists x versus v*,

separately for short-period and long-period

meteors. Again the trend is irregular for both

groups (see also fig. 16b), but we find a rather

surprising result: Short-orbit meteors seem to

have a greater x than those in elongated orbits,

at variance with the result of Jacchia's (1958)

analysis. If we look at unconnected results,

this difference is negligible: x=0.26±0.03 for

meteors with Q<6 a.u. and x=0.24±0.03 for

meteors with <2>6 a.u.; however, the mean

values reduced to constant mass of 0.8 g are,

respectively, 0.27 and 0.20. It should be

noted that in the present analysis the critical

aphelion distance for dividing the orbits into

long-periodic and short-periodic is 6 a.u.,

whereas it was 7 a.u. in Jacchia's (1958) paper.

Table 19.2.1 shows the dependence of x on

the integrated brightness «» both for all and

for sporadic meteors only. At faint magnitudes

the results look more scattered than those

previously obtained by Jacchia; otherwise

there are no remarkable differences (except, of

course, for the systematic difference caused by

the difference in the reference atmosphere).

Table 19.2.2 gives x versus «„ for the two

groups of short- and long-period meteors. No

particular comment is needed, except for

recalling that on the same row the meteors

have the same brightness but quite different

masses and velocities.

Table 19.3 gives the dependence of the

fragmentation index x

 o n mas s

 for all SuperSchmidt meteors and for sporadic Super-Schmidt

only. There is no difference between "all"

and "sporadic" in the dependence on mass.

For masses comprised between 0.05 and 5 g,

we conclude that x is constant and on the

average equal to 0.23 ±0.02. For meteors

with m between 0.01 and 0.05 g we have

x=0.40±0.04, while on the other side of the

distribution for meteors with m=o>5 g, we have

X=0.08±0.04. For these few big meteors the

standard deviation of the individual value of
36 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

a

I

4 0

1" -

30

vjkm/s)

40 50 60 70

04

0.3

0.2

X 0.1

0

-0.1

-0.2

• 1 " '"

•

-

i i r

d

1- ).

1"

1 1 I

-

-

T-

-

-

08

06

0.4

0.2

1

- I

1

1"

1 1

i

34

1

• <

e

\* i"

i - •

-

0.2 0.3 0.4 0.5 0.6 07 08 0.9

CosZ,

b

/

fI* {»

.. i i

-

b -

0.2 0.3 0.4 0.5 0.6 0.7 08 09

q(o.u)

s

: l'

; l

g

•I • h I ttK

 Xa.

[tt 11 1

T

• Q<6

x Q >6

T ,

1 J

o. u.

0. U. -

-

I03

0.2 0.3 0.4 05 06 07 08 09 1.0

q(a u)

FIGURE 16.—Fragmentation index x

 a$ a function of: a, velocity forall Super-Schmidt meteors; b, velocity for short-period and longperiod sporadic Super-Schmidt meteors; c, mass for Super-Schmidt and small-camera meteors together; d, brightness em

for Super-Schmidt and small-camera meteors together; *, zenith angle ZR of the trajectory for all Super-Schmidt meteors; perihelion distance q for: /, all Super-Schmidt meteors; g, two groups of Super-Schmidt meteors, short-period and long-period

orbits. The points at q <0.2 a.u. for short-period meteors are strongly influenced by two showers: Geminids (mean ^=0.142

a.u.; 20 meteors) and i Aquarids (mean y=0.084 a.u.; 8 meteors).

X is less than half the average, ±0.14 instead

of ±0.29. It may also be worth noting that

the standard deviation of the individual values

of x for small-camera meteors is smaller than

for Super-Schmidt meteors (±0.20 against

±0.29). As previously stated (Jacchia, 1958),

this difference reflects the fact that the relative

amount of fragmentation greatly varies among

fainter meteors.

Tables 19.4, 19.5, and 19.6 contain results

concerning small-camera meteors. They show

that for these meteors % decreases both with

mass and with velocity; the data must, therefore, be reduced respectively to a constant mass

and a constant velocity. There is a small

region of overlap in mass for Super-Schmidt

and small-camera meteors; the agreement in

this region is quite good, although the data

are few. No dependence of x on cos ZR is

found among the small-camera meteors.

Table 19.7 gives the mean value of x f°r

each shower, for both Super-Schmidt and
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 37

small-camera meteors. Each shower has its

own peculiar mean value (the same happens

for log a). The low value (x=0.04±0.05) of

the Southern Taurids, whose light curves are

known to be generally smooth (Jacchia, 1955),

is remarkable. Small values of x are found

also for the Northern Taurids (5 meteors:

X=0.03±0.07); a Hydrids (3 meteors: x =

0.04±0.04); Lyrids (3 meteors: x=0.08±

0.09); K Cygnids (4 meteors: x=0.11±0.09);

for the lone member of the r) Aquarid shower

(x=0.09); and the two Northern i Aquarids

(x=0.10±0.26).

Values of x for small-camera shower meteors

are available for a few showers: Geminids

have x=0.00±0.07, but if we reduce this value

to Wo, =30 km/s and to m=0.8 g (standard

Super-Schmidt mass), we get x«~0-15, in good

agreement with the value for Super-Schmidt

Geminids. For Southern Taurids we have

x=—0.17±0.07, which, after reduction, becomes x*<=0.02, in excellent agreement with

the Super-Schmidt value. Very good agreement is also found for Northern Taurids

(x=— 0.13±0.10, which after reduction becomes x««~0.10). There is fair agreement

forthePerseids (x=-0.13±0.10, i.e., x,«=0.15,

which compares with x»«~0.22 for SuperSchmidt meteors). A shower not present

among Super-Schmidt meteors is that of the

X Orionids, four members of which were photographed by small cameras and permitted the

determination of an average value of x- The

result is x=0.06±0.05 and xu~Q2§. On the

average, there are no differences between

sporadic and shower meteors with regard

to x.

When Super-Schmidt and small-camera

meteors are considered together, we have

values of x f°r masses ranging from 10~2 to

2X103 g (extreme averages 0.03 and 555 g)

and for a range in integrated brightness between

— 1.4 and 3.4 (extreme averages —1.14 and

3.02). The resulting mean values are listed

respectively in tables 19.8 and 19.9 and plotted

in figures 16c and 16d. From an inspection of

the tables we see that x remains approximately

constant up to a mass of about 5 g (x^O ^

±0.02) and then decreases to zero for a mass

comprised between 25 and 30 g. The dependence of x on €» looks roughly linear for eoo<2.

For brighter meteors one would expect x to

level off to a value near zero, and this seems to

be corroborated by the few meteors with

e»>2, although the data for them are very

scanty.

Table 19.10.1 shows mean values of x as a

function of the zenith angle both for all SuperSchmidt meteors (fig. 16e) and for sporadic

meteors only. We confirm that the fragmentation index decreases when cos ZR increases.

The correlation can be expressed by the linear

expression, mean x=0.53—0.4 cos ZR} or, if we

use values reduced to a constant mass of 0.8 g,

mean x=0.49— 0.37 cos ZR (63)

Since the correlation of x with cos ZR is rather

clear-cut, it may seem necessary to correct

the other correlations for this effect. Fortunately, there is practically no correlation

of cos ZR with the mass nor can the slight

correlation of cos ZR with v* affect the preceding results on x (»»)• Table 19.10.2 shows

x (cos ZR) for sporadic Super-Schmidt meteors

in groups Q<6 a.u., Q> 6 a.u.

Table 19.11 shows x as a function of the

aphelion distance Q. There is nothing to add

to the remarks made earlier in this section.

The correlation, or better, the lack of correlation, between x and log «r among the SuperSchmidt meteors has been fully discussed in

the section on log <r; however, we may add

here that a slight correlation between x and

log a exists among small-camera meteors

(table 19.12). Meteors having log a close to

— 12.0 show a mean value of x of —0.11

±0.05, while those with log a greater than

— 11.6 have x=0.03±0.03. On the other

hand, meteors with x<0 have log cr= —11.65

±0.05, while those with positive x have log

a= -11.45 ±0.08.

Table 19.13.1 shows x as a function of the

perihelion distance q both for all Super-Schmidt

meteors (fig. 16f) and for sporadic meteors

only. In table 19.13.2, x(?) is given for

sporadic meteors with Q<6 a.u. and Q>6 a.u.,

respectively, while table 19.13.3. is a similar

listing for all and not only sporadic meteors

(fig. 16g).

While no clear trend is visible among the

meteors with g>0.2. a.u., it appears significant
38 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

that those meteors that approach the sun

to a distance less than 0.2. a.u. have a considerably larger fragmentation index.

9. Wake and blending

We define "wake" as the short train that

follows the meteor head. On Super-Schmidt

films it shows as a tapering appendage of the

bright segments cut out by the shutter on the

meteor trail and gives these segments a characteristic teardrop appearance. The brightness

of the wake relative to the head varies from

meteor to meteor. As a rule, it is always visible

when the meteor brightness is five magnitudes

or more above the plate limit. Occasionally,

however, a meteor only two magnitudes

brighter than the plate limit may display a

conspicuous wake.

We define "blending" as the gradual increase

in length of the bright trail segments, which

occasionally results in their blending together

into a continuous-appearing trail. A considerable number of meteor trails show complete blending on Super-Schmidt films toward

the end of the trajectory. In very rare cases

blending may follow the occurrence of a flare

and then clear up before the end.

We have tried to give a rough quantitative

estimate of the intensity of wake and of blending, by assigning to each meteor a grade for

each of the two phenomena in a memory-based

scale ranging from zero to four. These grades

are listed in table 1.1 as W (wake) and B

(blending), respectively. Although in most

instances W and B were recorded as integers,

we sometimes found it necessary to use finer

subdivisions such as 0+, 0-1, 1~; for the most

exceptional cases of blending we have used 4+.

The subdivisions were transformed to approximate decimal fractions in table 1.1.

Mean values of B and TTand their distributions for all meteors and for sporadic meteors

only, as well as for particular groups, are

listed in table 20.1. The same quantities are

given in table 20.2 for shower meteors. The

mean values for all meteors are 5=0.51 ±0.05,

PF=0.74±0.05. Of all meteors 53 percent

show some wake, while only 32 percent show

some blending. The sporadic meteors show

less blending and more wake than shower

meteors do; however, according to the following figures, these differences do not appear

important.

Sporadic meteors

Shower meteors

All meteors

B±s.d.

0.47 ±0.05

0.63 ±0.08

0.51 ±0.05

TTis.d.

0.77 ±0.06

0.67 ±0.08

0.74 ±0.05

While meteors in short-period orbits have

slightly larger values of B and W than longperiod meteors, the results are not conclusive.

For sporadic meteors we find:

a.u.

l=0.46±0.08

5=0.37±0.07

W=0.73±0.08

W=0.70±0.09.

Meteors of classes A and S were excluded in

these two groups, so that the preceding values

agree with the overall average: 5 = 0.42,

W=0.71, slightly smaller than the averages for

all sporadic meteors.

Of the class A meteors (abrupt beginning),

77 percent show some blending; their average

value of B is 1.35 ±0.24, almost three times the

average of all other meteors. This is in agreement with what might be expected if the sudden

increase in brightness that makes the meteor

become visible is caused by a complete disintegration of the meteor body into fragments of different sizes. With respect to

wake, however, class A meteors are normal

(W=0.59±0.13).

Opposite behavior is shown by meteors of

class F, i.e., those from which one or more large

fragments become detached from the main

body in the course of the trajectory. Of these

meteors, which presumably represent a hardier

group whose members are less apt to be

pulverized, 10 out of 11 showed no blending

at all. On the other hand, 82 percent of them

showed some degree of wake, and their average

value of W (2.1 ±0.4) is nearly three times the

mean of all meteors. This feature, however,

may simply reflect the fact that most class F

meteors are quite bright.

Among the showers the Taurids are the most

remarkable. All 18 Southern Taurids have

B=0 and 15 of them also have_W=0. The

five Northern Taurids also have 5 — 0 (four of

them have B=0, and the remaining one has

5=0.3, or 0+). The wake of the Northern

Taurids is normal. The results for the Southern
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 39

Taurids are in agreement with the well-known

smoothness of the light curves of these meteors.

The 11 Perseids have 2?~*0 (10 out of 11 have

B=0) and normal wake (W=0.96±0.35). The

absence of blending is probably just a consequence of the short duration of the trajectory,

which prevents the fragments from becoming

widely dispersed. Both Draconids have 5= 4

and W=0.

The 115 Aquarids show a high value of the

blending (B= 1.55 ±0.27) and low wake (W

=0.21 ±0.12). Only one out of 11 has B=0,

while eight out of 11 have W=0. The 14

a Capricomids also have a large value of B

(1.0 ±0.3) and normal W, while on the contrary,

the Geminids (20 members) have a large

W (1.5 ±0.3) and normal B.

The dependence of wake and blending on

the various meteor parameters has been investigated. Table 20.3 shows the variations

with the velocity of B and W and of the percentages of the different groups. As was

expected, both ~B and W decrease, although

somewhat irregularly, when v*, increases (fig.

17a). Table 20.4 gives the mean values of B

and W and their distribution as a function of

the mass. The behavior of B is irregular, while

the dependence of W on mass is quite strong.

There is practically no wake for small meteors;

then W increases regularly with mass and the

wake is generally well developed for the largest

meteors (W=2.5±0.3). This is apparently

just an effect of relative brightness, not of the

mass itself. Figure 17b shows the plotting of

these results. Table 20.5 lists the same quantities as functions of the difference AM between

the plate limit and the maximum photographic

magnitude. As we can see also in figure

17c, W increases strongly with AM, from

about zero for AM—I to about 3 for AM>5.

B shows a parabolic trend with AM; it could

also be considered roughly as a constant.

Tables 20.6 to 20.10 show the mean values of

B and W and their distributions as a function

of €», log <r, x> co s ZB, and Q, respectively.

These results are plotted in figures 17d-h.

Since the integrated brightness <„ is a function

of mo and v*,, Bit*) and W(e*>) are functions

that could be derived from the results of tables

20.1 and 20.2. W increases with eo, while B

has a parabolic trend. The dependence of B

and W on log a is quite interesting. Meteors

with log <r< —11.45 (log (r= —11.66) show

normal values for both B and W. They do

not follow the trend of all the other groups.

As a matter of fact, if we exclude them, we

note a clear-cut and regular increase of 2? and

W when log a increases: B rises from 0.22 at

log a= —11.37 to 0.74 at log a= —10.83, while

W increases from 0.54 to 1.02. The behavior

of W for sporadic meteors is just about the

same as that for all meteors; however, the

value of B for sporadic meteors with log

<r<^ —11.45 is smaller than the corresponding

one for all meteors and is not in disagreement

with the general trend.

In table 20.8 we see that the wake is independent of the fragmentation index x> while

B increases with x- This increase is very

slow for sporadic meteors from x=~0 1 to

X=0.5, since B increases only from 0.31 to

0.40. Then ~B jumps to 1.1 ±0.2 for the last

group (x=0.89). The behavior of all meteors

is more regular; there is an increase from

0.3 to 0.6 when x increases from —0.1 to 0.5

and then a jump to 5 = 1.2±0.2 for x=0.9.

The wake is also almost independent of the

zenith angle. There is, however, a very regular

decrease of the blending with the increase of

cos ZR. This is in accordance with expectation, because meteors with low angles of incidence have longer durations; also, the effect

will be more conspicuous on photographs taken

near the zenith, as was the case of the SuperSchmidt photographs.

The list of results ends with table 20.10,

which is devoted to the correlations of B and W

with the aphelion distance Q. The wake does

not seem to depend at all on the type of the

orbit; however, there are some differences in

the blending. If we examine all meteors,

there is a small difference between the first

three groups (Q<7 a.u.) and the remaining

two ((£>7 a.u.), since the average value of

B for the former is around 0.6, while for the

latter it is 0.3. If we look at sporadic meteors

only, the picture is different. There is a large

difference between the first group (Q<3.5 a.u.)

and the others. In fact, we have 5=1.0±0.2

for Q=2.6 and B=0.38±0.05 for all the other

meteors (Q from 3.5 a.u. to •=). A further
40 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 41

subdivision among these meteors shows that

for meteors having Q comprised between 3.5

and 7 a.u., B is about 0.4 and decreases to 0.33

for meteors with <2>7 a.u. The difference

between the behavior of the sporadic meteors

and all meteors is, of course, due to the showers;

Taurids and Geminids lower the value of B

in the group with Q<3.5 a.u., while a Capricornids, Quadrantids, and 5 Aquarids increase

it in the group between 3.5 and 7 a.u.

10. Peculiarities of individual showers;

meteors with abrupt beginnings;

asteroidal meteors

a. Showers

Table 21 gives a synoptic survey of the physical

characteristics of those of our Super-Schmidt

meteors that belong to major showers. In the

upper part of the table we have compared means

for shower meteors with means for all meteors,

for sporadic meteors, and for meteors with

abrupt beginnings (A) and short trails (S).

The number of observations refers to quantities such as vm and cos ZB, which were available for all meteors (413) without exception.

For each individual parameter the mean was

taken over the available data, the number of

which was occasionally smaller than the number in the last columns. (For example, we had

only 400 values of the duration D and 396

values of log <r.) The mean value of A log pe0TT

for "all" meteors refers to the 350 meteors that

were used in the analysis of the decelerations.

The same is true for the mean A log pC0TT for

sporadic meteors.

For two parameters, log a and x> means for

individual showers were computed and listed in

the respective sections dealing with the analysis

of these quantities (sees. 7 and 8). These

means are not necessarily identical with the

means listed in table 21, because meteors of

classes A and S were excluded in their formation

in harmony with the analysis of sporadic meteors. The means of table 21 apply to all

meteors.

The means are all unweighted except the ones

of A log pe0TT for which we have used the

weight w. Draconids and Geminids, which have

large systematic peculiarities in A log pCOrr, were

eliminated in computing the mean of this quantity for shower meteors (actually, their inclusion would not have changed the mean although

it would have increased the standard deviation

by a factor of three).

Meteors whose membership in a shower may

be subject to some doubt (those marked with a

Q after the shower code number in table 1.1)

were included in the means of individual showers, except for meteor no. 4513, whose physical

characteristics are so different from those of

the two bonafide Draconids that its inclusion

would have spoiled the uniqueness of the

Draconid data. On the other hand, we have

eliminated meteor no. 5180 from the means of

the Northern Taurids because of its drastically

different physical characteristics, although its

membership in the shower does not seem to be

in question.

In the column headed A'H2&, we have listed

the difference between the mean value of H2.5

for individual showers and meteor groups and

the means of H2_6 for sporadic meteors. These

means are all reduced to a standard meteor

mass of 0.3 g using the coefficient of log ma

from table 4. [log pt.5 standard=log p2i observed+0.28 (log Wo,+0.52); the mean mass

for each group is a logarithmic mean.] The

means were plotted on a diagram (fig. 18), in

which smooth curves were drawn through the

points representing sporadic meteors separating those with aphelion distances larger than

6 a.u. from those in short-period orbits. The

differences A'H2S were taken from these smooth

curves. For the sake of completeness we have

also given A'H25 for meteors of classes A and

S; the residuals were taken from a smooth

curve through points representing the sporadic

meteors without those of classes A and S.

The parameters that best characterize the

physical peculiarities of each shower are A'H2S,

A log peorr, log a, x, and B. The means of these

quantities for individual showers are plotted

in figure 19, which enables us to tell at a glance

how one shower differs from another. Thus

we can see that the Draconids are exceptional

in just about every respect, and the Geminids

are nearly four times denser than the average

(A log Peorr=— 0.39), but crumble just as

easily as any ordinary meteor (normal x and B)

and appear at normal heights (AH2S= — 0.5

km). Delta Aquarids are crumbly (large x»
42 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

large B) and appear lower than the average

(A'#2.5=— 3.1 km), but their decelerations

are normal. The Southern Taurids have

great tensile strength (x and B just about zero),

but apparently are not denser than the average

since their decelerations are perfectly normal

(Alog P=0).

All these clues are far from adding up to

the picture of meteor structure and composition that we could have by studying specimens

in the laboratory, but at least they tell us

something about the diversity to be found in

the meteor population and may be useful in

reconstructing the processes of comet formation and disintegration.

6. Meteors with abrupt beginnings

The results of least-squares solutions for the

heights of meteors with abrupt beginnings

- -10.0

-8.S

• Sporadic meteors with Q £ 6 a u

» Sporadic meteors with 0 > 6 a. u

10 15 20 30 40 50 60 70

vM(km/s)

FIGURE 18.—The height i/2.5 at which meteors reach absolute magnitude +2.5 while brightening, as a function

of velocity. Logarithms of the atmospheric density p

(g/cm*) in ordinates at left; heights, in km, at right.

Dots: sporadic meteors with Q<6 a.u.; crosses:

sporadic meteors with Q^>6 a.u.; circled dots: meteors

in individual showers. Smooth curves have been drawn,

for reference, through the points representing sporadic

meteors. Theoretical values from equation (18) are

represented by the broken straight line.

(class A meteors), involving all the five basic

parameters, are given in table 3.13; comments

on these solutions are found in section 4b. In

view of the statement often repeated in meteor

literature, that the abrupt increase in brightness

in such meteors, which clearly indicates a breakup of the meteor body, occurs at a point in the

trajectory corresponding to a constant value

of py2 (McCrosky, 1955a; Whipple, 1959;

McKinley, 1961), we have tried to see if we could

confirm or disprove this assertion on the basis

of our material.

Altogether our Super-Schmidt material includes 26 meteors with an abrupt beginning,

or about 6 percent of the total number.

McCrosky (1955b) estimates that 13 percent of all

Super-Schmidt meteors belongs to this category;

the smaller percentage in our material is probably due partly to selection (many meteors of

class A are of too short duration to yield good

decelerations) and partly to a more stringent

rule for classification (several meteors of class

S display a fast rise to maximum and could

almost be classified as A's). Even among our

26 class A meteors some have a less abrupt

beginning than others; for 12 of them the rise

is almost instantaneous.

If we take the atmospheric density pAB corresponding to the abrupt beginning of all class

A meteors and put pABDa,=const, we find by

least squares K=3.6±0.3. Using only the 12

ultra-abrupt meteors, we obtain JK==3.0±0.5.

Taking the density pB corresponding to the

beginning heights of all Super-Schmidt meteors

and putting pBv5= const, we find K—3.0±0.1;

this compares with 2£=3.7±0.3 for the actually

observed beginnings of all class A meteors.

We see, then, that fragile meteors tend to

break up at a point corresponding to a constant

value of pw3 rather than of pw2, and that the

power of v is not too different from that found

from the beginning points of ordinary meteors.

Abrupt meteors do, however, begin 4 km lower,

on the average, than ordinary meteors (see sec.

4b).

The p«3=const relation would suggest heat

transfer rather than pressure as the trigger for

the breakup of meteors. This could be the case

if we have to deal with a body so porous that

air molecules will penetrate deep inside to do
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 43

-10

-11.0

-11.2

-11.4

-11.6

-

_

• a Cop

T

Ivir T

Tt

S.TouN.Tou{ Tf 1 /

1 j.

Dro ^-14.9 ±0.8

3em

S^qrjr

"•Qua

f

br

T

JaHya

a

30 40 50 60 70

v-,(km/s)

20 30 40 50 60 70

v-Jkm/s)

0.4

X

0.6

0.4

0.2

0

Drot

-

-

I.9S0.6

laCop

1 S.Toui 1

8 A V |

4 Qua

1

fLyr T

tOri

r *LM

Ptr

.TjAcjr

d

20 3 0 40 50 60 70

-0.6

20 30 40 50 60 70

v_ (km/s)

60 70

FIGURE 19.—Physical characteristics of individual meteor showers arranged in order of increasing velocity: a, deviation of the

height #2.5 from the meat! curve corresponding to sporadic meteors (see fig. 18), taking into account the aphelion distance Q;

b, acceleration values (see table 1.2; a high value means that the meteor had an abnormally high deceleration; the opposite

is true for low values); c, logarithm of the ablation coefficient <r; d, fragmentation index x ; e, blending index B. (The standard

deviations of the mean value of B for Southern Taurids (18 meteors) and a Hydrids (3 meteors) are equal to zero.)

their heating and melting, thus destroying the

precarious cohesion of the body as a whole. In

larger meteors the penetration of air molecules

will be relatively smaller, owing to the shielding

by the outer layers; this could explain why no

meteors with abrupt beginnings are found

among small-camera meteors. This process of

flaking off of large meteors and complete

breakup of small meteors was described by

Jacchia (1955) in his first paper on fragmentation.

c. Search for asteroidal meteors

Since several of the major meteor showers are

associated with comets and since the heights,

decelerations, and other physical characteristics

of shower meteors, taken in their totality, do

not differ from those of most sporadic meteors,

we must conclude that the overwhelming majority of the photographic meteors are of cometary

origin. This does not exclude the possibility

that a few asteroidal meteors might be included

in our sampling.

In comparison with a cometary meteor, an

astefroidal meteor should presumably be much

more dense and of greater tensile strength. For

such a meteor, then, we must expect to find

some peculiar characteristics, such as

1. an abnormally small deceleration, i.e.,

a strongly negative value of A log pe0Tr',
44 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

2. low fragmentation index x;

3. low ablation coefficient <r;

4. long trajectory, resulting in an exceptionally low end height;

5. absence of terminal blending;

6. rather smooth light curve, at least in the

early part of the trajectory; never an

abrupt beginning.

In addition, on the basis of what we know

about asteroids, we would expect the orbit of

such a meteor to have an aphelion well inside

Jupiter's orbit.

Only one of our 413 Super-Schmidt meteors satisfies all these requirements, namely

meteor no. 7946. This meteor entered the

atmosphere with a velocity of 18.5 km/s at an

angle of 26?6 with respect to the vertical. It

became visible on the photographs at a height

of 88.1 km, reached a maximum brightness of

—017 (photographic, absolute), and disappeared

after 2.55 seconds at the height of 49.3 km, the

lowest on record for any of our Super-Schmidt

meteors. A single fragment became detached

a little before midtrajectory and could be

followed on the photograph for 0!l0. The

orbit has a major axis of 2.49 a.u., a perihelion

distance of 0.94 a.u., and an aphelion distance

of 4.04 a.u. The deceleration is much smaller

than the average for a meteor with comparable

mass, velocity, and angle of incidence. The

mean value of A log p for the whole trajectory

is —0.85, which compares with a mean value

of —0.05 for meteors with Q=4 a.u. The trail

shows no trace of terminal blending. The

mean value of the fragmentation index x for

the whole trail is -f-0.08; but in the early portion of the trail, before the loss of the fragment,

it is about —0.1; after the loss of the fragment

it jumps to +0.3. The mean value of log a

is —11.46. The light curve is quite smooth,

except for some minor flaring during the last

hah* second of the visible trajectory. The ratio

of the observed duration to the theoretical

duration is 0.93, while the mean for all SuperSchmidt meteors is 0.61, and the mean for

meteors with a velocity of 18 km/s is 0.58.

According to equation (41) the mean density

of all Super-Schmidt meteors is 0.26 g/cm3.

For standard conditions of meteor shape and

atmospheric density a value of —0.85 in

A log pCOTT corresponds to a factor of 19 in the

density; this would result in a density of 4.9

g/cm3 for meteor no. 7946. While we would

not give any weight to this individual density

determination as such, we want to point out

that it is of the right order of magnitude for

an asteroidal meteor.

Acknowledgments

Aspects of this research were supported in the

past by the Office of Naval Ordnance, the

Office of Naval Research, the Air Force Cambridge Research Center, Geophysics Research

Directorate, and the U.S. Army Office of

Ordnance Research.

As stated in the orbital analysis of the present

meteor material (Jacchia and Whipple, 1961),

a great many people contributed to the success

of this meteor program, in its manifold aspects,

involving instrumental design and construction,

station operation, photography, visual observing, measuring, and computing. For a list of

the principal persons and agencies involved

we refer to the paper quoted above. In addition, the present analysis required a great

deal of electronic computing, which was programmed principally by J. C. Cherniack, R. L.

Emerson, and B. M. Fardon.

References

JACCHIA, L. G.

1948. Ballistics of the upper atmosphere. Harvard Coll. Obs. and Center of Analysis

M.I.T. Tech. Rep., no. 2; Harvard

Reprint Ser. II, no. 26, 30 pp.

1949a. Photographic meteor phenomena and theory. Harvard Coll. Obs. and Center

of Analysis M.I.T. Tech. Rep., no. 3;

Harvard Reprint Ser. II, no. 31, 36 pp.

1949b. Atmospheric density profile and gradients

from early parts of photographic meteor

trails. Harvard Coll. Obs. and Center

of Analysis M.I.T. Tech. Rep., no. 4;

Harvard Reprint Ser. II, no. 32, 12 pp.

1952. A comparative analysis of atmospheric

densities from meteor decelerations observed in Massachusetts and New

Mexico. Harvard Coll. Obs. and Numerical Analysis Laboratory of M.I.T.

Tech. Rep., no. 10; Harvard Reprint

Ser. II, no. 44, 37 pp.
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 45

1955.

1956.

1957a.

1957b.

1958.

1960.

1963.

JACCHIA, L.

1950.

JACCHIA, L.

1961.

LEVIN, B. J

1961.

The physical theory of meteors, VIII:

Fragmentation as a cause of the faintmeteor anomaly. Astrophys. Journ.,

vol. 121, pp. 521-527.

On two 1953 Giacobinids and on some

physical characteristics of shower meteors

(abstract). Astron. Journ., vol. 61,

pp. 6-7; see also Sky and Telescope,

vol. 15, p. 207.

A preliminary analysis of atmospheric

densities from meteor decelerations for

solar, lunar and yearly oscillations.

Journ. Meteorol., vol. 14, pp. 34-37.

On the "color-index" of meteors. Astron.

Journ., vol. 62, pp. 358-362.

On two parameters used in the physical

theory of meteors. Smithsonian Contr.

Astrophys., vol. 2, no. 9, pp. 181-187.

Individual characteristics of meteor families (abstract). Astron. Journ., vol.

65, p. 53.

Meteors, meteorites and comets; interrelations. In The Solar System, vol.

IV, ed. by B. M. Middlehurst and G. P.

Kuiper, University of Chicago Press,

Chicago, pp. 774-798.

G.; KOPAL, Z.; and MILLMAN, P. M.

A photographic study of the Draconid

meteor shower of 1946. Astrophys.

Journ., vol. Ill , pp. 104-133.

G., and WHIPPLB, F. L.

Precision orbits of 413 photographic meteors. Smithsonian Contr. Astrophys.,

vol. 4, no. 4, pp. 97-129.

Physikalische Theorie der Meteore und die

Meteoritische Substanz in Sonnensystem. Akademie-Verlag, Berlin.

MCCROSKY, R. E.

1955a. Fragmentation of faint meteors (abstract).

Astron. Journ., vol. 60, p. 170.

1955b. Physical and statistical studies of meteor

fragmentation. Thesis, Harvard University.

MCKINLBY, D. W. R.

1961. Meteor Science and Engineering. McGrawHill, New York, 309 pp.

MILLMAN, P. M.

1935. An analysis of meteor spectra: second

paper. Ann. Harvard Coll. Obs., vol.

82, pp. 149-177.

MILLMAN, P. M., and MCKINLBY, D. W. R.

1963. Meteors. In The Solar System, vol. IV, ed.

by B. M. Middlehuret and G. P. Kuiper,

University of Chicago Press, Chicago, pp.

674-773.

MINZNEK, R. A., and RIPLEY, W. S.

1956. The ARDC model atmosphere, 1956. Air

Force Surveys and Geophys., TN 56-204

(no. 86), p. 15.

OPIK, E.

1933. Atomic collisions and radiation of meteors.

Harvard Reprint Ser. I, no. 100, 39 pp.

RUSSELL, J. A.

1960. A time-resolved spectrum of the terminal

burst of a Perseid meteor. Astrophys.

Journ., vol. 131, pp. 34-37.

U.S. STANDARD ATMOSPHERE 1962

1962. Prepared under NASA, USAF, and U.S.

Weather Bureau, Washington, D.C., 278

pp.

VERNIANI, F.

1961. On meteor ablation in the atmosphere. II

Nuovo Cimento, vol. 19, pp. 415-442.

1964a. On the luminous efficiency of meteors.

Smithsonian Astrophys. Obs. Spec.

Rep., no. 145, 62 pp.; also Smithsonian

Contr. Astrophys., vol. 8, no. 5, pp. 141-

172, 1965.

1964b. On the density of meteoroids, II: The

density of faint photographic meteors.

II Nuovo Cimento, vol. 33, pp. 1173-

1184.

1966. Meteor masses and luminosity. Smithsonian Astrophys. Obs. Spec. Rep., no. 219,

46 pp.

WHIPPLE, F. L.

1943. Meteors and the earth's upper atmosphere.

Rev. Mod. Phys., vol. 15, pp. 246-264.

1959. Solid particles in the solar system. Journ.

Geophys. Res., vol. 64, pp. 1653-1664.

WHIPPLE, F. L., and JACCHIA, L. G.

1957. Reduction methods for photographic meteor trails. In Smithsonian Contr. Astrophys., vol. 1, no. 2, pp. 183-206.

225-636 O-67— 4
Abstract

In this paper we present a statistical evaluation of the atmospheric trajectories of the 413 precision-reduced meteors,

doubly photographed with the Super-Schmidt cameras in New Mexico, for which orbital data have been previously

published and analyzed by Jacchia and Whipple (1961). We have studied the dependence of heights, lengths, decelerations, and magnitudes on such basic parameters as velocity, angle of incidence, and mass, as well as on derived

parameters such as the ablation coefficient and the fragmentation index; the latter are in turn related to the other

geometric and physical characteristics, including the phenomena of wake and terminal blending. A comparison

with classical meteor theory shows again and again that fragmentation is the most important factor in causing the

wide discrepancies between theory and observation.

Owing to strong interrelations among the basic parameters, mostly inherent in the meteor phenomenon, we

have tried not to rely entirely on the least-squares process for the analysis; where the least-squares method was used,

we have often added the variables one at a time in the solution, in order to evaluate the effect of the interrelations and

the reliability of the solutions. Our analysis confirms the results previously obtained by Jacchia (1955, 1956, 1957a,

1957b, 1958, 1960, 1963) using part of the present material, concerning the systematic variation in the accelerations,

the ablation coefficient, the fragmentation index, and the color index, with meteor brightness, as well as the physical

peculiarities of individual meteor showers and the systematic differences between meteors in short^period and in

long-period orbits. The maximum brightness of fragmenting meteors is greater than for nonfragmenting ones;

Super-Schmidt meteors are, on the average, half a magnitude brighter at maximum than predicted by single-body

theory and are about one-third shorter in duration and length.

For meteors that suddenly break up (abrupt-beginning meteors) we find that the breakup occurs at a point

in the trajectory that corresponds to a constant value of pi? (p=air density, i>=velocity). This suggests heat transfer

rather than dynamic pressure as the break up trigger and leads to the picture of a meteor body so porous that air

molecules can penetrate to its core; shielding by the outer layers prevents the complete breakup of larger meteors.

Using Verniani's (1964a) value, 1.0X10"19 zero mag g~J cm"3 s4, for the photographic luminous-efficiency coefficient TOp, we find that the average Super-Schmidt meteor has a density of 0.26 g/cm3

; a meteor that enters the

atmosphere with a velocity of 40 km/sec and makes an angle of 45° with the vertical must have a mass of 0.69 g to

reach visual magnitude zero at maximum. Among showers we find that the Geminids are four times denser than

the average meteor, but crumble just as easily, while the Southern Taurids have normal densities but do not fragment much; the Draconids are unique in their extraordinary fragility.

A search for meteors of asteroidal origin has led us to conclude that only one of our 413 Super-Schmidt meteors,

namely no. 7946, possesses all the requisites to qualify as a member of this group.

46
Tables 1.1-21
48 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 418 Super-Schmidt meteors: Trajectories

Apparent radiant eln Q "2.5

2961

3000

302*

3037

3051

3072

307*

3076

3088

3217

3228

323*

32SO

3265

3271

3277

3286

3288

3295

3299

3SO3

3307

3312

3327

3332

333*

33*0

3342

33**

3355

3360

3377

3379

3386

3393

3399

3*05

3*07

3*11

3416

3*2*

3*50

3*63

3487

3*97

52

52

52

52

52

52

52

82

52

52

52

52

52

52

10 2.22043

4 3.45698

4 1.13079

3 30.39983

3 20.16674

3 21.40481

3 21.41403

3 22.41288

3 28.34066

4 22.43214

4 23.32587

4 23.36348

4 26.32654

5 1.36734

4 22.35236

5 31.33476

5 25.22660

5 24.28819

5 23.40982

5 23.35833

5 22.28093

5 22.27047

5 22.25789

5 21.36274

5 21.34855

52 5 21.32504

52 5 21.30844

52 5 21.31213

82 5 21.21701

52 7 19.41152

7 21.35983

7 24.34757

7 24.36850

7 25.27043

7 25.42131

7 25.44425

7 26.22340

7 26.25526

7 26.27789

7 26.35994 1

27.27810 5

20.31172 5

28.31997 5

29.42639 5

4.46209

15 51

289 14

272 36

235 9

117 27

210 20

213 46

167 43

280 14

271 39

265 40

227 59

222 6

326 41

271 44

309 29

273 10

229 46

261 15

252 9

222 28

225 15

193 39

257 10

242 6

283 31

306 4 7

218 52

209 56

316 58

334 8

10 22

302 28

303 34

311 11

336 45

304 9

320 19

305 23

305 19

336 39

339 36

338 1

341 20

271 57

HO 12

»36 51

-6 13

-45 36

-13 58

-5 53

• 33 1*

• 42 29

-1 50

-3 55

• 51 30

• 33 27

• 41 42

-33 20

-34 47

-6 14

-7 37

-4 41

• 61 25

• 61 ?'•

-23 ' •

• 10 47

• 14 14

• 14 43

-29 33

• 68 31

-16 7

-16 59

• 36 40

-7 19

• 20 42

-16 14

-7 47

-15 13

-9 48

-8 11

-15 43

-15 29

-15 1

-15 9

• 76 46

.205

.311

.155

.1SS

.608

.137

.188

.072

.282

.451

.SOI

.271

.309

.288

.330

.348

.031

.281

.333

.431

.390

.140

.090

.222

.617

.174

.299

.388

.392

.504

.291

.552

.147

.309

.517

.036

.082

.035

.339

.008

.068

.118

.466

.072

.790

.848

.219

.196

.666

.777

.438

.709

.560

.983

.811

.819

.803

.493

.824

.787

.102

.377

.727

.749

.779

.871

.812

.550

.900

.807

.498

.397

.809

.605

.631

.755

.755

.822

.613

.674

.554

.731

.701

.490

.572

.607

.655

.488

31.22

49.58

68.85

59.92

16. 10

38.90

55.35

16.82

25.93

48.04

40.76

28.94

29.37

41.45

47.37

50.70

41.37

21.02

32.27

29.OS

17.33

19.24

16.57

35.96

24.60

53.57

62.80

19.54

19.25

34.28

44.34

65.33

24^12

36.05

43.05

26.10

35.16

24.47

25.34

43.23

42.71

43.42

41.82

28.17

-2.2

-0.9

• 0.4

• 0.2

-0.5

-0.6

-0.8

• 0.9

• 1.2

-0.6

• 1.3

• 0.4

• 1.0

• 0.1

-1-.5

-0.9

• I.I

• 1.5

• 1.1

• 1.0

• 1.3

• 0.4

-0.6

-0.9

• 2.3

• 0.9

-0.8

-0.8

• 1.0

• 0.6

• 0.1

-1.7

-0.9

• 1.5

• 1.0

-1.4

-0.7

-0.8

• 0.1

• 0.5

94.4

109.6

112.6

116.3G

94. S

97.9

100.S

92.0

99.a

106.7

105.4

89.4

101.6

105.5

105.7

108.4

99.4

86.4

101.3

101.1

85.7

93.7

9 1 . 1

100.8

93.9

112.9

102.9

93.5

89.5

92.1

112.8

9*.O

98.6

97.1

97.1

92.2

94.0

96.5

102.0

96.8

102.4

97.7

92.3

94.3

108.7

112.4

115.1

94.5

97.4

100.5

92.0

99.6

105.9

105.3

88.9

101.6

105.5

104.4

108.9

99.4

85.7

101.3

99.1

84.1

93.1

89.1

100.8

93.9

110.4

102.9

91.6

111.9

94.0

98.6

96.9

97.0

92.2

94.0

96.2

100.5

96.7

102.4

»7.7

<»2.3

94.1

III.9

119.8

92.3

97.9

102.0

90.9

99.2

107.1

104.8

89.4

99.6

106.6

107.3

108.9

99.4

83.8

100.3

97.9

83.7

91.5

84.6

100.2

91.7

113.2

103.9

90.3

89.1

92.1

112.6

91.9

100.1

96.1

95.8

92.4

93.5

96.5

105.6

98.2

102.0

97.4

92.4

88.9

97.9

104.9

10?.8

80.3

t.O

3. 1

8.9

9.8

10 0.2

94.8

96.2

40. 7

96. 7

92.1

98.4

98.2

78.6

91.5

92.6

81.0

81.5

84.0

95.6

80.4

102.2

91.7

90.0

97.1

88.5

90.5

93.4

85.0

91.3

89.0

91.0

41.6

92.3

92.6

92.7

92.1

78. 1

93.1

102.2

105.4

73.6

B6.9

87.7

76.9

85.5

92.4

90.0

78.5

05.5

94. 7

M5.7

92.6

95.1

11. 0

89.4

88. 1

11.0

80.5

80.0

94.0

89.6

85.4

83.1

85.7

91.9

88.2

85. 7

85.6

86.1

80.7

87.4

87.9

88.3

88.9

89.3

90.8

87.8

87.4

78.0

92.6

102.2

105.4

73. 6

84. 8

87. 7

Ih.t

85.5

92.5

89.6

78.5

85.5

94.7

85.3

92.6

95.1

77.0

77.0

80.5

93.1

76.1

91.8

88. 1

81.6

85.6

91.8

88.0

85.7

85.6

86.1

80.7

87.4

87.9

87.5

88.9

88.9

88.8

87.8

87.1
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 49

TABLE 1.1.—Basic physical data for 418 Super-Schmidt meteors: Trajectories.—Continued

Vis .A Vis.B

296 1

3CCC

3024

1037

3072

1 C H

1C76

3088

3217

3?28

123*

3250

3265

1271

3277

3288

3295

13C3

13C7

1312

1327

3332

?334

334C

3342

3344

3 3 55

3360

3377

3379

33H6

3393

4C5

4C7

411

416

424

45G

463

487

497

4.7

19.4

ie.cc

5. 1

15.7

7.t

1 1 .B

4.2

4.8

4.9

8.3

11.7

1C. 7

e. 7

13.2

7.H

4.8

t . I

•i. 3

5.4

•:. 1

t . 3

11. 5

14. C

3.2

3.9

3.C

5.H

2.C

7.2

1C.3

3.3C

3.4

1.4

12.6

5.5

7.4

4.2

4.0

8.3

21.5

1 3. 8G

t . 1

15. 3

4.9

1C.5

3.8

5.2

5.4

7.6

H. 1

11.7

B.8

12.2

/.5

3.3

4.6

2.6

5.8.

3.C

7.4

12.7

12.1

3.2

3.8

4.4

6.0

3.8

/.t

7.2

12.2

4.7

2.2

6.3

13.0

6.8

8. 1

6. 1

.68

.70

.970

.45

.53

1.3 1

1.C1

. 3C

.48

.47

• 7C

.54

.52

.42

1.2C

.52

.65

.ei

.92

. 38

.82

.49

.46

1.56

.54

.40

.22

. 3B

.51

.45

.45

.95

.25

.35

.54

.62

.29

.52

. 37

. 38

C

35

40

20

31

7C

58

16

25

25

41

32

28

25

6 3

28

27

42

38

24

4 /

0

24

87

21

20

14

23

28

27

24

56

7

20

8

35

14

26

21

16

40

22

33

32 «

22

29 <

80 <

57

17

27

24 ,

32

23

29 '

22

35

50

28

14

45

46

18

39

24

25

84

28

16

13

21

17

18

25

50

16

9

26

34

17

23

17

23

. 8

.2

. 1

.8

.8

.4

.8

.2

.5

.5

.4

• C

. 7

• 3

.8

. 0

. 1

'.0

. 3

.7

B 4

.4

. 1

. 1

.5

.6

.0

1. 7

>.5

? , j

>.C

3.6

.9

>. 2

3.9

. 3

.6

- 2

• 2.5

• 2.5

• 3

• 2.5

-1

• 2

• 1.5

• 2

• C.5

• 1.3

• 2

0

• 2

• 1.5

-1

• 0.5

0

• 1

• 1

• 2

• 2

• 1.5

• 1.8

• 1

• 1

• 2

• 1.8

• 2

• 2

• 1.?

• 1

• 2

• 1.3

• 1.8

• 1

• 1.5

• 2

• 2

• 3

• 1.5

• 0.5

• 2

• 1.5

• 2.5

— 1.7

-1.0

-2.8

-1.8

-2.3

-0.2

-2.2

-0.8

-0.8

-l.S

-Z.6

-0.5

-0.6

-l.l

-0.1

-0.7

-0.1

• 0.4

-1.5

-1.7

-2.4

• 0.2

-1.8

-1.5

-0.9

-1.2

-l.l

-2.5

-1.5

-0.5

-2.0

-1.7

-2.2

-2.0

• •545

-.263

-.517

-.170

-.457

-.154

-.389

-.583

-.442

-.946

-.676

-.785

-.499

• .034

-.279

-.641

-.918

-.845

-1.089

-.663

-.934

-1.039

-.643

-.366

-.214

• .084

-1.296

-1.199

-.529

-.303

— .819

-1.024

-.HO

• .460

-.588

-1.164

-.778

• -'25

-•>67

-.407

-.846.

2.3889

0.0891

0.0187

0.0626

6.7148

0.1201

0.0839

1.9370

0.3164

0.0646

0.0336

0.1808

0.1388

0.0904

0.2066

0.0814

0.5036

0.0749

0.1207

0.3164

0.6457

0.5863

0.0400

0.1293

0.0563

0.0491

3.4420

0.1550

0.0426

0.0730

0.0362

0•2002

0.1324

0.0839

3.3574

0.1201

0.1020

0.2066

0.3357

0.0878

0.0968

0.0510

0.1291

37000

01380

00290

00970

04000

01860

01300

30000

04900

01000

00520

02800

02150

01400

O32Ot>

01260

01500

07800

01160

01870

04900

10000

09080

00620

05100

00872

00760

53310

02400

00660

01130

00560

03100

02050

01300

00750

52000

01860

01S80

03200

05200

01360

01500

00790

02000

-11.09

-11.15

-11.47

-10.52

-10.96

-11.45

-11.23

-11.29

-11.12

-10.93

-11.20

-11.14

-11.24

-11.38

-11.08

-11.42

-10.63

-11.15

-11.05

-11.20

-11.29

-11.42

-11.17

-11.14

-11.24

-11.57

-11.06

-10.83

-11.74

-11.70

-11.22

-10.83

-11.06

-11.27

-11.50

-11.28

-10.82

-11.24

-10.85

-11.26

-11.38

-11.33

-11.50

-10.83

• •36

• .28

• •36

• 2.97

-.02

• •39

• •15

• •25

• .07

• •23

• .31

• .02

-. 13

• .44

-.07

• .00

• .86

• .00

• .00

• •30

• •34

• •30

• .30

-.29

• •09

• .41

• •47

-.14

• .25

• •24

• •32

• •55

• .09

• .41

• -31

• .31

• .09

• .05

• •42

• •67

• .74

• •58

• .30

• -55

10

1

0

2

1.50

1

0

0

1

0.3

0

0

1

0

1

0

0

0

0

O.5U

0

0

0

0

0

1

1

2

0

0

0

0.3

1

0

0

0

3

0

0

0.50

0

0

1

0

0

0

0

0

2

0

1

0

0

0

1.5

0

1

0

2

0

0

2.5

0

0

0

0

0

0

0

0

2

2.5

0

0

3

2

0

2

0

1

3

0

0

OQ

1.5

1.5

2

2.5

I.1)

2
50 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

"2.5 "ED

3567

3573

3604

3610

3612

3629

3633

3636

3640

3643

3651

3655

3657

3663

3784

3786

3813

3847

3861

3877

3886

4103

4111

4125

4136

4138

4141

4143

4147

4151

4153

4181

4199

4216

4229

4289

4311

4313

4328

4330

4340

4351

4360

4369

4388

52 8

52 P

52 a

52 8

52 t

52 E

52 t

52 I

52 t

52 t

52 I

52 I

52 f

52 (

52 E

52 I

52 t

52 f

52 t

52 I

52 «

52 t

52 t

52 <

52 «

52 t

52 «

52 <

52 (

52 <

52 (

52 t

52 (

52 (

52 •

52 «

52

 c

52 <

52 «

52 '

52

52

52 •

52

52

15.32162

15.378T8

18.25543

18.34726

18.35793

18.46233

20.21140

20.24167

20.27477

21.19139

21.29165

21.30888

21.40200

21.46684

22.24496

22.27604

25.44441

30.36452

30.46355

31.47361

L.47897

1.37781

14.19977

19.30147

21.41546

21.42265

22.18470

> 22.19380

> 22.22390

> 22.38093

> 23.28640

> 25.22210

> 29.43208

) 25.26884

> 19.20433

) 10.15042

) 13.27009

) 13.32250

> 14.21329

» 14.23858

) 14.31121

) 14.37389

t 16.15238

) 16.33235

> 17.27972

1

7

20

120

1

1

10

1Q

3

12Q

2

3

7Q

326

350

277

352

52

345

275

324

273

329

329

323

68

349

353

333

266

51

18

4

356

242

227

244

319

5

191

275

264

3

259

277

300

43

218

315

347

308

341

57

352

4

10

353

316

21

27

28

14

20

34

50

19

28

12

3

3

0

10

1

2

58

27

29

56

18

11

52

39

53

37

15

39

44

32

3

37

49

14

59

57

13

20

11

15

54

22

42

11

53

-11

• 5

• 65

• 2

• 61

-2

• 58

-11

• 15

-4

-8

-2

• 66

• 0

-8

-14

• 65

• 63

• 61

• 6

• 0

• 43

-21

• 30

• 35

• 18

• 59

-7

-14

• 12

-13

-8

-14

+ 59

• 74

• 1

-26

• 12

• 13

• 51

-11

-13

• 45

• 7

-0

18

0

9

10

5

25

7

5

36

45

55

19

55

56

53

2

18

29

21

32

35

0

46

16

31

32

50

15

6

24

1

42

34

32

45

54

8

50

20

41

8

9

49

5

54

.427

.462

.309

.134

.322

.329

.255

.121

.355

.083

.4 39

.543

.280

.408

.055

.278

.107

.283

.241

.314

.292

.266

.414

.427

.147

.327

.099

.198

.086

.229

.393

.058

.466

.332

.123

.114

.167

.363

.423

.253

.553

.570

.326

.430

.530

.717

.886

.781

.856

.651

.614

.870

.694

.697

.620

.750

.806

.657

.638

.544

.676

.313

.730

.851

.719

.549

.860

.584

.934

.993

.677

.795

.550

.635

.493

.689

.632

.602

.539

.458

.812

.518

.612

.904

.467

.720

.665

.609

.875

.697

26.85

36.80

31.01

41.56

58.71

34.20

23.91

23.46

15.59

2 7.00

25.12

26.74

55.84

30.35

37.50

21.28

23.11

59.03

52.24

25.95

29.16

18.98

16.82

18.37

53.45

68.79

16.92

29.90

22.70

70.97

20.58

30.45

32.12

60.51

34.18

18.82

20.13

15.37

25.81

6 4. 16

22.74

24.98

45.40

26.73

16.02

• 0.3

-1.6

-0.3

• 0.2

-0.3

• 1.4

• 0.8

• 0.1

-2.0

• 1.6

• 0.8

• 0.3

-O.I

• 0.5

-0.6

-0.3

• 1.6

-0.2

-2.4

• 1.2

• 0.7

• 2.3

-0.8

• 1.3

-1.2

-0.6

• 0.3

• 1.4

-1.9

-0.7

• 0.1

-1.6

• 1.5

• 0.2

• 1.0

• 0.5

-1.1

• 1.6

-0.3

-2.5

• 0.0

• 0.3

• 0.1

• l.l

• 1.6

100.1

100.3

103.7

100.9

112.2

100.6

99.1

99.5

8 7. 8G

99.2

92.1

100.8

107.4

101.2

96.7

89.2

98.1

96.2

111.1

100.0

101.5

90.9

85.7

84.0

10H.5

113.4

83.7

99.5

86.3

111.7

95.2

101.3

98.9

109.6

103.8

90.0

86.7

83.4

94.0

115.9

100.0

92.4

95.5

101.0

83.5

99.4

100.3

103.7

99.1

111.2

99.9

98.4

99.5

87.8

99.2

91.7

100.8

107.4

101.2

96.0

89.2

98.1

96.2

Ul. l

100.0

101 .5

90.9

85.7

84.0

108.5

113.4

83.7

99.5

86.3

111.2

95.2

101.3

98.9

109.5

103.8

90.3

86.0

83.4

92.5

115.9

98.1

92.4

95.5

101.0

83.5

98.8

99.5

105.2

97.5

112.4

100.2

95.3

98.8

90.9

99.7

91.5

98.2

107.5

101.2

97.0

as.6

97.7

97.1

111.4

98.9

101.4

88.9

84.2

83.3

109.1

114.3

83.6

97.0

86.3

121.3

95.5

103.0

96.8

110.2

103.5

90.0

86.0

81.7

91.4

118.4

99.3

91.4

97.4

98.9

82.2

90.3

83.6

96.4

91.5

100. 1

93.7

86.0

83.0

74.3

92.8

89.0

83.1

99.8

87.2

93.0

85.1

94.0

92.4

89.7

88.1

88.5

85.5

74.6

77.7

91.8

102.6

79.8

90.6

77.5

9S.9

86.4

87.4

88.4

102.9

97.4

82.8

85.3

76.4

79.8

108.3

86.5

84.9

90.3

85.6

75.0

87.2

81.0

93.3

85.9

96.3

89.0

82.2

77.1

67.0

89.1

81.0

82.1

97.1

84.9

89.9

80.2

89.9

89.0

88.2

84.8

83.4

83.8

72.7

74.R

89.6

95.7

76.6

86.7

/0.9

95.3

83.9

86.5

86.2

94.0

92.0

76.4

82.4

73.3

77.2

98.5

82.2

80.7

86.4

83.4

72.1

86.0

81.0

93.2

84.8

96.3

88.7

82.2

77.1

67.0

89.1

79.9

82.1

97.1

84.3

89.3

80.2

89.9

89.0

87.9

84.8

83.4

8 3.8

72.6

74.7

H9.3

95.7

75.0

86.6

70.9

95.3

83.9

86.2

86.2

94.0

92.0

76.4

82.4

73.0

77.2

98.5

82.2

80.6

86.4

83.4

72.1
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 51

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

ail No.

3567

3573

3604

3610

3612

3629

36 3 3

3636

1640

3643

3651

3655

3657

3663

3784

3786

3C13

384 7

3661

3877

3886

41C 3

4111

4125

4136

4138

4141

4147

4151

4153

4181

4199

4216

4229

4289

4311

4313

4328

4330

4340

4351

4360

4369

4388

LA

5.8

6.5

5.0

3.1

11.1

9.7

1C.3

ltl.8

7.7

4.9

4.8

7.8

8.4

7.5

5.3

15.1

5.1

8.8

10.4

16.7

6.8

4.5

4.7

7.8

6.0

6.8

11.8

6.2

12.8

4.7

13.3

13.0

6.4

5.2

8.8

3.9

17.5

5.2

4.2

8.2

7.9

6.8

7.3

8.4

3.4

4.7

l.BG

8.1

14.9

13.8

7.1

5.6

6.6

6.6

6.6

6.6

7.1

13.7

5.0

9.2

S.I

16.6

2.7

9.7

3.9

2.5

8.4

3.5

11.4

10.6

7.4

10.8

6.7

12.6

1C.6

4.7

4.0

7.0

6.3

18.1

7.3

5.2

e.i

7.2

6.3

1

2

1

1

1

I

I

1

1

1

D

.74

.60

.44

.46

.43

.55

.42

.06G

.62

.65

.88

.29

.89

.37

.64

.18

.17

.52

.83

.16

• 43

.34

.56

.37

.38

.70

.08

.47

.81

.79

.67

.48

.76

• CO

.43

.14

.73

.60

.10

.72

.34

.77

.08

nA

38

37

23

24

24

30

87

125

37

35

52

17

49

18

39

66

10

30

46

63

76

29

21

24

31

64

28

37

46

27

25

40

54

23

65

39

32

59

38

21

46

66

nB

34

36

21

20

5

25

46

92

28

29

47

14

43

17

39

63

28

35

67

71

33

22

18

29

63

15

47

40

34

21

38

35

20

68

36

31

56

34

19

36

52

2.8

4.9

3.0

2.8

2.8

1.8

3.0

5.0

1.6

2.2

2.8

2.6

2.6

3.5

4.0

1.2

2.9

5.1

2.1

2.4

4.7

2.5

3.9

3.4

3.4

5.4

3.0

3.4

4.6

1.5

2.6

2.2

2.6

4.6

1.6

4.1

4.9

2.6

3.2

2.6

2.2

2.0

Vis .A

0

0

• 1

-1

• 2

• C.5

-1

• 1

• 0.5

• 1.5

• 1

• 1

• 3

• 1.7

• 2

»0.3

• 2

-2

*1

• 1

• 1.5

• 2.5

+ 1.8

• I

• 1.5

• 1

0

• 1.5

• 1.5

• 2

Vis.B

• 1.5

• 1

• 2.5

• 1

• 1.5

• 3

• 1

0

• 2

• 1.5

• 1.5

• 2

• 1

• 1

• 1.9

0

• 1

• 0.5

• I

0

• 2

-1

0

• 1

+ 1.5

• 1.5

• 2.5

• 1

• 2

• 2

0

• 0.5

• 1

• 1

• 1.5

• 2

C.I.

-0.6

-2.8

-1.4

-0.8

-0.5

-1.3

-1.1

-1.5

-1.5

-1.2

-1.1

-1.3

-1.5

-1.5

-0.8

-2.1

-0.3

-0.7

-1.4

-1.1

-2.1

-0.3

-2.0

-2.1

-0.6

-1.1

-1.2

-1.0

-1.4

-2.2

-0.6

-1.8

-2.1

-0.8

-1.0

-1.0

-0.6

-0.9

-.510

+ .073

-.388

-.781

-.414

-.872

— . 756

-.072

+ .750

-.890

-.692

-.521

-.628

-.432

-.427

-.472

-.6b9

+ .313

-.732

-.388

+ .101

-.891

-.212

-.445

-.560

+ .526

-.122

-.370

+ .180

-.957

-.564

-.686

-.442

-.427

-.687

-.536

+ .519

-. 166

-.600

-.674

-.780

-.724

**>

0.3293

0.4842

0.2776

0.0478

0.0381

0.0710

0.2738

1.4269

33.5094

0.1324

0.2544

0.3422

0.0278

0.2776

0.1433

0.7102

0.3564

0.2938

0.2221

0.3487

0•1420

5.8109

0.4197

0.0826

0.0225

1.2138

5.9400

0.0420

1.0330

1.0847

0.0684

0.0245

0.1072

1.2138

0.9782

1.2267

0.3564

0.2518

1.2590

0.3441

0.0478

0.182'

1.0976

m»l

.05100

.07500

.04300

.00740

.00590

.01100

.04240

.22100

5.19000

.02050

.03940

.05300

.00430

.04300

.02220

.11000

.05520

.04550

.03440

.05400

.90000

.06500

.01280

.00348

.18800

.92000

.00650

.16000

.16800

.01060

.00380

.01660

.18800

.15150

.19000

.05520

.03900

.19500

.05330

.00740

.02830

.17000

log a

-11.12

-11.12

-10.94

-11.66

-11.19

-11.23

-11.20

-11.47

-11.19

-11.13

-10.42

-11.23

-11.49

-11.42

-11.13

-10.61

-10.87

-11.37

-11.24

-11.34

— 11.05

-11.04

-10.98

-11.49

-11.52

-11.10

-11.16

-11.32

-11.07

-11.22

-11.39

-11.28

-11.20

-11.15

-10.80

-11.00

-11.22

-10.48

-11.36

-11.14

-11.70

-11.27

-10.98

X

+ .62

+ .28

+ .22

+ .21

+ .34

-.16

• .05

+ .10

+ .21

+ .56

+ .86

-.01

+ .37

+ .18

+ .54

+ .16

-.13

• .42

+ .31

+ .06

-.11

+ .33

+ .50

+ .14

+ .16

+ .44

• .69

+ .23

+ .50

+ .43

+ .44

+ .12

+ .13

-.01

-.11

+ .04

+ .24

+ .10

+ .41

+ .15

+ .01

+ .67

+ .03

-.07

W

2.5

2

00

0

0

0

I

0.5

4

0

0.5

0

0

0

1

1.5

1

1.3

0

0

Q

2

0

0

0

0

Q

3

0

2

2

0

0

0

0.50

0.5

0

1

1.5

0

1

0

0

0

B

2.5

0

00

1.3

0

00

0

0

0

2

3

0

0

0

2

3

2

1.3

0

ou

0

Q

0

0

0

0

0

Q

0

0

1

0.5

0

0

0

0

2

0

0

1

0

0

1

0

0
52 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 418 Super-Schmidt meteors: Trajectories.—Continued

Trail No

4394

4454

4464

4472

4505

4507

4513

4534

4542

4574

4596

4618

4622

462*

4645

4657

4659

4677

4679

4683

4701

4702

4952

4962

4964

4966

4974

5006

5022

5045

5047

5063

5079

5083

5101

5112

5124

5176

5180

5195

5231

5237

5257

5273

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

6 2

5 2

52

5 2

5 2

5 2

5 2

5 2

52

52

52

52

5 2

5 1

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

5 2

Date

> 17.31692

) 19.36752

) 19.*336*

> 20.25706

) 20.37880

) 20.38*72

) 20.39**8

1 25.28963

> 25.33709

) 26.22639

) 26.36991

) 27.28448

» 27.29697

» 27.30209

> 27.40903

) 27.46457

1

 27.46431

> 28.383*0

1

 28.39461

> 28.41338

) 30.48305

) 24.14407

10 19.44153

10 21.20082

10 21.20117

10 21.22682

10 21.27695

10 21.3*780

10 21.4005*

10 21.4850*

10 22.13*63

10 22.26372

10 22.31903

10 22.33811

10 22.377*6

10 22.*3**9

10 22.*7095

10 23.*2685

10 23.4*002

10 23.4819*

10 2*.27733

10 2*.30020

10 24.38896

10 2*.*2539

Sh.No

120

20

9 0

2

2

8 0

8

2

8 0

8

8

8

8

2 0

2

17

2

8 0

17

Appare

a

11

8 9

3 5 0

2 8 2

3 5 9

16

2 6 7

3 0 1

8

2 3

3 2 6

3 5 7

1 0 7

3 4 *

6 2

6

16

260

3*0

110

2 5

3 1 3

6 2

3 3 9

2 9 2

J 3

9 *

9 5

4 1

1 2 6

11

1 0 3

9 6

9 3

9 5

9 4

3 6

4 4

4 2

4 2

9 9

3 2

4 5

1 6 1

8

2 9

4 8

5 9

3

4 0

3 1

4 2

6

5 2

5

4 7

3 2

3 7

15

5 0

42

20

3 6

4 *

5 6

2

16

4 5

2 4

5 9

5 7

1 *

2 5

4 3

4 5

6

5 2

4 7

4 *

2 0

*

3 5

2 3

5

3 2

1 7

3 3

i t radiant

5

• 2

• * 3

• 10

• 57

- 1

• 0

• 58

• 72

- 3

• 7

• 54

- 2

• * 6

- 0

- 5

- 5

—*

• 85

• * 8

• 5

• 70

• 7

• * 6

• 28

• 6

• 6

• 16

• 11

• 84

• 0

• 26

• 15

• 16

• 15

• 16

• 9

• 12

• 19

• 12

• 33

- 6

• 19

• 36

17

5 9

16

4 3

8

15

2 9

18

* 2

16

34

3 2

4 9

5

4 2

2 4

30

16

5

5 3

2 7

31

18

4 4

2 8

12

2

12

3

17

38

5 6

3

4 6

4 3

0

3 0

3 9

3

4 8

2 9

35

4 8

sin (I

.17 4

.25 0

.35 5

.01 6

.52 5

. 6 36

.083

.156

.307

.177

.005

.298

.203

.529

.114

.317

.387

.149

.433

.414

.288

.564

.058

.246

.12 1

.199

.185

.442

.197

.321

.252

.205

.278

.317

.739

.304

.370

.149

.306

.230

.636

.360

.239

Cos Z,,

.857

.622

.551

.667

.722

.820

.193

.641

.793

.667

.641

.817

.277

.774

.756

.372

.501

.484

.669

.589

. 787

.866

.949

.601

.801

. 311

.692

.H49

.611

.653

. 306

.584

.688

.803

.937

.535

. 795

.783

.572

.498

.777

.924

.410

V

-

33.85

69.05

21.89

2 3.50

25.66

29.03

19.30

31.78

23.86

28.62

22.41

20.50

67.87

18.57

58.85

23.79

18.16

41.15

67.16

30.01

31.62

11.49

21.65

15.92

26.29

67.05

68.17

30.13

42.42

16.26

70.64

67.83

67.27

67.40

67.51

27.88

30.47

31.88

28.92

67.83

28.61

32.87

63.05

M

• 0.8

• 0.0

-0.9

• 0.8

• 1.9

• 2.0

-0.3

-1.8

• 1.2

• 1 .9

• 2.0

• 1.9

• 0.3

• 0.9

-1. 1

• 0.8

-0. 5

-1. 2

• 1.5

-2. 1

• 1.4

• 0.0

• 1.7

• 1.4

-0. 5

-0. 3

-0. 6

-1. 2

• 0.3

• 0.1

- 1 .0

-1. 1

-2. 4

-1. 3

-2.3

• 0.4

-0.8

-0.6

• 0.9

-0.6

• 0.8

-1.7

-0.8

"B

97.5

111.6

99.9

101 .6

101.4

99.5

90.3

104.7

98.1

103.3

94.3

98.4

113.8

95.2

111.5

100.9

109.0

114.2

99. 7

101.3

n.i

97.0

92.5

101.9

117.7

115.5

100.5

99.9

86.5

118.9

118.4

117.6

116.7

114.9

101.4

102.3

93.4

102.1

116.7

102.0

102.4

113.1

96.2

111.6

99.9

100.9

100.2

98.6

90.3

104.5

98.1

102.1

94.3

97.8

113.6

95.2

109.2

100.9

ion. 3

114.2

99.4

101.2

77.2

97.0

92.5

101.2

116.7

115.4

100.0

99.9

86.5

118.4

118.4

117.6

116.0

114.9

101.3

102.3

93.0

102.1

116.7

102.0

102.4

113.1

"2.5

95.3

114.0

98. 7

100. 1

96.5

95.8

90.3

104.5

95.1

99. 1

91.9

94.9

115. 1

93.0

112.5

99. 3

109.5

114.5

97.8

102.8

75.1

96.9

91.2

98.6

118.0

101.1

101. 1

85.8

121.3

123.3

120.1

118.2

115.2

101.9

93.3

102.1

120.8

100.7

102.1

118.2

"HI.

85.6

103.8

76.2

91.6

92.6

92.3

90.2

86.9

88.5

95.4

88.0

87.8

108.6

86.9

96.7

87.2

96.6

105.1

89.N

K'l.S

73. 0

• 9. 1

aa.o

B9.4

101.3

107.1

»•>. 1

93. 9

83. 0

109.8

109.2

106.8

111.3

96.8

86.2

84.2

81.7

93.0

102.8

88.6

82.1

108.4

"ED

84.2

101.0

73.8

87. 7

89.2

86.7

88.4

84.9

86.9

88.5

dl.5

85.2

106.6

82.8

9J.0

82.9

92.4

97.3

83.8

81.9

69.7

Ml. 7

at.*

B7.0

101.5

99.6

78.1

88.9

79.9

107.1

101. 3

96.2

98.2

90.7

80.5

80.1

80.9

86.8

99.*

85.1

79.0

10*.6

°E

83.8

101.0

73.8

87.7

86.8

86.5

87.2

84.9

86.9

88.2

81.5

85.2

106.6

82.8

91.6

82.8

91.8

96.2

81.K

82.4

69. 7

80.7

83.1

*>.O

101.5

98.0

78.1

88.9

79.0

107.1

103.3

96.1

98.1

90.7

80.1

80.1

78.7

86.8

99.4

85.1

79.0

104.6
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 53

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

Vis.A Vis.B log a

4454

4464

44 72

4505

45C7

451 1

4534

4574

4596

4622

4t?4

4645

4657

4659

4677

4679

4683

47C1

4702

4952

4S62

4S64

4966

4S74

5C06

5022

5C45

5047

5063

5C73

5C79

5083

5 I C 1

511 2

512 4

5 176

5180

5195

5231

5237

5257

5273

e,(

2 7 .

1 1.

3.

t .

U .

l.<

1C.<

12 .

i

s.<

?7.

S .

1 1.

H .

S.

3 .'

f .(

t.

7 t

2/.

e.

1 1 .

•»•

is.

I 7.

e .

•>'

2 p

23.(

12.

t.

13.

13.

3.

7

5 . c

23.(

4.,

6.'

15.

B.(

1 1.

1 1.

4.

1C.

26.

P.

17..

7.

7.

10.(

2 i

6.

6 .

6 .

23.

e.

10.<

8.

4.(

1 7.

11.

12.(

11.

4 .

) 16.'

12.

! 6.

13.

) 15.

: 5.

> 8.

1 0.

G

;

2.

1.

•

2.

•

1.

1.

1.

4B

25

27

c; i

K2

5 5

fl4

CC

HO

92

i'

6H

45

1 1

fb

tl

4C

92

7H

T,

82

CO

72

77

37

90

44

7 )

55

8?

3tf

46

3 4

3S

50

9C

6C

95

52

77

78

34

16

137

34

31

i 3

5 9

41

5C

21

53

2)

9',

44

4'i

2/

4 5

0

i )

4C

46

41

41

21

42

24

37

2B

IC4

1 7

26

2C

22

85

53

25

45

31

46

43

15

25

13 i

129 '

31 C

27 C

29

59

36

49

22 ,

46

22

85

47

47

20

54

38

42

43

53

26

43

19

42

21

32

32

106

23

25

20

24

66

53

30

55

27

42

41

20

.4

. 3

.6

.9

. s

.5

.4

.6

.2

.0

. 3

.9

.j

.2

.4

•2

. 7

. l

.0

. <,

.5

_ 2

. •;

. 1

. i

•1

.4

.9

.9

.4

.0

. 1

. 5

• C

.8

g 3

. 2

. 2

. 9

B 7

• 3

•2.3

0

• 2.5

• I

• 1.8

• 1

• 1.5

• 1

C

• 1.8

-1

• 1.5

• 2

• I

• 0.5

• 1.5

• 1

• 1

-I

• 1

• 0.5

0

•1

• 1

• 2

• 1

• 4

• 1

• 1

0

• 2.5

• 2

0

• 3

• 3.5

• 1

• 1

C

0

G

• 1.5

• 2

• 2

• 1. 5

• 2

• 2

• 1.2

• 3

• 1

0

• 1.8

C

• 1.5

• 2

• 2

• 2

• 1

• 2

• 1

-0.6

-1.9

-0.9

-2.4

-1.6

-0.9

-1.6

-0.4

-0.7

-1 .6

-0.9

-0.8

-0.5

-1.9

-1.2

-1.4

-o.s

-0.2

-1.6

-1.3

-2.5

-2.1

-2.0

-0.5

-0.9

-1.9

-2.1

-2.1

-1.0

-2.3

-2.7

-1.2

-1.2

-2.2

-2.8

• .388

-.964

-1.172

-.328

• •331

-.954

-.782

-.670

-.654

-.124

-.161

-.548

-.107

-.142

-.753

• .475

-.995

-.309

-.784

-.819

-.002

-.511

-.025

-.235

-.055

-.471

• •290

-.221

• .319

• •107

-.120

-.015

-.401

-.474

-.122

-.652

• •257

0.0120

5.5139

0.3958

0. 1349

0.0565

1.4204

1.3*17

0. 1814

0.0981

0.3190

0.0136

0.7296

0.0697

1.0912

1.0137

0.2286

0.04,8

0.1369

1.1240

1.6012

0.9039

0.8523

0.1679

0.0659

0.0194

0.8716

0.1550

0.7231

0.0194

4.9070

0.0387

0.1356

0.0 355

0.0859

0.7748

0.7231

0.2518

0.2905

0.0484

0.1937

1.0589

.01100

.00198

.85400

.06130

.02090

.00875

.22000

.21400

.02810

.01520

.04940

.00211

.11300

.01080

.16900

.15 700

.03540

.00740

.02120

.29800

.24800

.14000

.13200

.02600

.01020

.00300

.13500

.02400

.11200

.00300

.76000

.00600

.02100

• 005 50

.01330

.12000

.11200

.03900

.04500

.00750

.03000

.16400

-10.94 •.SI

-11.48 ^.07

-11.01 ^.23

-11.33 ».12

-11.16 ^.34

-11.15 ^.32

-11.27 *.ll

—11.29 +.29

-11.06 ^.20

-11.28 -.03

—11.12 ••61

-11.11 ^.63

-11.00 ••01

-11.36 +.34

-11.2

-11.4

-11.1

-10.9

-11.3

-11.2

-10.8

. -.05

•> •1.0 6

> ^.12

I +.37

b ^.04

( ^.97

1 ••OH

-11.27 -.34

-10.92 ^.24

-10.91 ^.37

-11.24 +.73

-11.04 *.45

-11.31 -.12

-11.20 +.60

• .17

-11.18 +.53

-11.04 +.02

• .60

-10.96 ^.33

-11.73 +.14

-11.40 -.31

-11.26 -.02

-11.41 •.68

-11.30 *.O2

-11.03 *.*l

-11.22 ^.17

-11.15 *.26

0

0

1.7

1.5

0

0

1

1

0

0

0.5

0

1.5

0.3

0.7

2

1

0.3

0

3

00

I

I

0

0

0

1

0.5

0

0

3

0

0.7

o

2

0

0

1

0

0

0

1.3

0

0

0

0

0

0

0

4

0

0

0

00

0

0.3

0

1

0

3

2

0

0

3

1.5

0

00

OQ

0

0

0

1.5

3

1

0

0.3

0.7

1.3

0

0

0

2

0

0

0

0.3

0. JQ
54 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 41S Super-Schmidt meteors: Trajectories.—Continued

5289

5332

53*6

5170

5*50

5*72

5511

5551

5557

5572

5601

5605

5640

5644

5648

5688

5759

A062

6093

6095

6105

6218

6275

6329

6376

6398

6429

6433

6437

6491

6546

6795

6802

6811

6842

6882

6904

6915

6932

6949

6959

6961

6971

6992

6998

5 2

5 ?

5 2

5 7

5 2

5 2

5 2

5 2

5 2

5 2

52

52

52

52

52

5 3

5 2

5 3

5 3

5 3

5 3

53

5 3

5 3

5 3

5 3

5 3

5 3

5 3

53

53

5 3

5 3

5 3

5 3

5 3

53

S3

5 3

5 3

5 3

5 3

5 3

5 3

1 0

11

11

11

11

11

11

12

12

12

12

12

12

12

12

3

12

1

1

1

1

1

1

1

2

2

2

2

2

2

3

3

3

3

3

3

3

3

3

3

3

3

3

Date

24.49407

7.0902H

11.21208

12.18972

15.48622

19.50249

21.44139

9.25420

9.27326

10.21182

11.19612

11.21585

12.21300

12.22909

12.23334

20.39372

13.14203

10.13459

13.39400

13.41927

13.46463

16.44630

20.3166?

23.38956

5.14883

10.2 7808

12.47257

12.49419

12.50608

18.40527

21.46448

12.22319

12.27608

12.30740

13.38101

14.30065

14.44660

18.21645

18.34978

18.43249

18.47712

19.22288

19.31853

19.39518

19.43246

Sh.No.

2

13

17

4

log

100

110

Appare

a

1 5 9

1 7

5 6

3 4 1

1 5 2

I SO

6 7

1 3 3

6 8

3

1 0 8

1 0 9

1 0 9

no

1 1 0

2 6 5

110

5 8

2 5 0

2 2 0

2 4 2

2 1 0

1 9 8

1 2 0

1 4 5

142

175

2 3 6

2 1 7

1 5 9

2 5 4

130

234

2 1 7

2 1 8

1 4 0

2 9 4

172

2 39

1 8 5

30 7

1 2 3

1 7 6

1 7 4

1 7 6

5 3

4 1

5 1

20

8

2

3

2 5

4 7

18

4 9

31

1 2

2 7

3 7

2 6

2 8

5 3

1 6

1 7

4 5

4 5

17

52

3 5

sz

3635

24

11

51

2 7

5 8

12

5 7

3 7

5 6

4

28

6

2 4

5 9

15

5 4

10

nt radiant

b

• 7 41

• 41 42

• 15 4

• 23 57

• 22 47

• 67 54

• 21 56

• 31 40

- 7 24

• 51 12

• 33 7

• 32 44

• 32 39

• 32 10

• 32 49

- 5 54

• 31 9

-23 57

• 43 19

• 41 44

• 35 58

- 0 49

• 29 21

•15 34

• 13 24

• 38 29

•10 3

• 9 55

-29 36

• 49 2

•9 5

• 78 35

*22 35

-21 26

-24 9

• 61 1

- 0 46

• 30 6

• 6 58

• 23 34

-4 4 50

• 26 51

• 71 8

- 6 28

sin Q

.223

.375

.274

.409

.435

.194

.287

.261

.192

.146

.301

.366

.318

.390

.438

.125

.271

.191

.279

.122

.144

.113

.297

.412

.760

• 412

.657

.101

.226

.157

.207

.274

.238

.013

.111

.346

.176

.566

.442

.276

.282

.675

.450

.378

.519

.797

. 790

.8 76

.8H5

.712

.750

.518

.767

.788

.579

.658

.657

.705

.722

.450

.362

.629

.2 34

.619

.551

.675

.494

.810

.486

I«14

.856

.468

.894

.690

.690

.446

.171

.512

.815

.101

.928

.71 1

.520

.159

.988

.821

.489

v

»

61.40

21.04

28. 75

15.58

71.71

46.75

11.00

60.76

22.67

17.19

16.66

36. Id

37.13

35.56

36.21

68.64

16.41

15.33

4 3.50

79. 73

4 3.95

72.78

61.60

72.70

31.67

35.40

66.06

71.07

22.69

64.45

17.39

54.84

61.25

5 7.90

12.72

59.86

20.36

27.07

48.71

20.12

21.60

24.68

30.25

M

pm

• 0. 2

• 1.1

• 0. 7

• 1. 3

-1. 3

-1. 2

-0.2

• O.fc

-0. 6

• 1.4

• 0.4

-2. 7

• 0.9

-0. 4

-0. 7

-5. 7

• 1.0

• 1.2

• 0.7

-0. 3

• 0.7

-1. 4

-I .1

• 1.7

-O. I

-0.1

-0.7

-0.6

• 0.4

-0.6

-0. 1

• 0.9

• 0.9

• 0.5

•2.2

• 0.8

• 2.2

-0.5

-0.5

• 0.8

• 1.9

• 2.1

• 1.3

h

1 10.5

92.8

102.3

75.8

127. H

104.7

104.9

112.6

99.5

97.7

100.7

101. )

101.4

99.7

107.1

114.4

100.8

84.6

107.9

95.0

101.8

115.2

113.0

95.8

102.2

97.4

113.2

115.8

90.3

108.0

85.7

109.0

100.4

109.6

78.3

110.)

91.8

101.4

109.4

94.0

86.6

99.8

104.3

110.5

92.5

107.)

75.6

177.8

104.7

104.5

112.6

99.5

97.5

100.7

101.)

101.2

98.8

107.1

114.4

100.8

84.6

107.6

95.0

100.7

1 IS.2

I 13.0

95.7

101.4

97.4

111.2

115.8

90.)

108.0

85.7

109.0

100.4

78.2

110.)

91.8

100.7

109.4

94.0

85.9

97.5

104.0

"2.5

115.1

92.4

100.4

74.8

125.9

105.3

105.4

113.4

98.3

89.4

100.5

101.4

100.0

99.2

107.8

115.3

100.6

84. t

107.8

95.)

100.9

115.9

114.6

9).8

107.7

92.9

114.5

117.8

90.8

108.3

85.8

109.4

100.7

110.6

73.7

117.2

90.3

99.4

110.9

91.9

84.3

90.8

107.5

107.8

87.2

87.7

71.9

89.1

92.0

81.9

104.8

82.2

80.2

91.0

82.1

92.6

88.7

H9.0

84.1

94.0

• 7.0

106.0

• 9.5

96. >

100.8

103.9

• 6.)

9).4

85. 7

97.5

106.6

*0.9

94.5

84.0

107.9

96.9

101. 7

68.7

105.1

88.5

82.9

96.6

91.)

81.0

87.4

96.1

"BD

98. 7

77. 7

83.8

67.)

b7.2

89.5

80.8

100.7

78. 7

77.8

88.5

74.6

90.6

84.6

04.4

7(1.6

92.1

80.0

107.8

87.2

85.9

96.)

96.4

M4.4

89.2

78.8

90.8

100.8

74.7

90.4

87.4

99.5

92.3

67.4

100.1

D3.5

76.9

91.1

90.1

78.6

1)2.8

90.8

h

98.7

77. 7

83.8

67.)

87.7

85.4

80.8

100.2

78. 7

77.8

88.5

74.5

90.6

84.2

83.7

78.61

92.1

11.*

107.8

• 7.7

85.9

96.)

96.4

84.4

88.6

78.8

90.8

100.8

74.7

90.4

87.4

99.5

97.0

97.4

67.4

100.1

83.5

76.6

91.1

88.1

78.6

82.7

90.1
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 55

TABLE 1.1.—Basic physical data for 418 Super-Schmidt meteors: Trajectories.—Continued

Vis .A Vie .B log i

5289

5332

53*6

5370

5*50

5*72

5511

5551

5557

5572

5601

5605

564C

56**

56*8

5688

5759

6062

6093

6095

61C5

6218

6275

6329

6376

6398

6*?9

6*33

6*37

6*91

65*6

6795

6802

6811

66*2

6682

690*

6932

69*9

6959

6961

6971

6992

9.2

9.0

9.7

5.a

11.c

11.3

1*.8

1C.2

* .3

8.7

11.2

2C.7

8.C

6.2

9.3

37.1G

I*.C

3.7

11.3

11.*

1*. *

12.1

12.9

5.2

10.8

12. 7

5 . 5

7. 7

11. *

e.5

1C.3

2.e

n. c

7 . *

12. 7

7.C

15. 5

1*.7

17.3

2.5

6.0

9.7

ICO

11.3

5.1

13.9

ICO

12.2

8.2

8.5

5.1

1C.6

21.8

6.2

S.6

10.5

39. 8G

1C.9

5.0

1C.3

10.2

1*.O

l*.l

6.5

3. 7

13.6

IC.5

S.4

10. 1

8.2

15.2

16.7

18.5

2.1

7.6

.35

.85

.83

.65

. 6 *

.60

1.05

.*C

1.22

1.15

.58

1.1*

.**

1.16G

.67

.51

.69

.*2

.55

.65

l.*C

.*M

.*U

.28

.39

.37

• *2

1.12

.56

.61

1.30

.73

1.9C

.36

.67

2 . *

1.6

2.5

2.1

6.1

*.5

3.C

1.9

3."*

2.0

2.9

5.9

2.2

3.5

3.7

8.5

2.0

2.2

2.2

3.2

2.3

3.8

3.6

2.0

3 .*

3.5

3.C

2.5

U*

1.7

1.7

I .*

1.1

2 -*

3.6

2.6

2.6

1.7

1.3

•1 ^2.5

•2 +1.5

• 2 ^2

• 1.5

• 2.5

• 0.5

• 3

• 1

• 0.5

• 1. 5

• 2

-0.9

-1.4

-1.6

-1.5

-1. 5 -1. 8

•2.5 -1. *

-1. 2

•0.5 -1. 6

-1.0

-1.8

-1.5

-1.3

-3.3

-1.1

-1.2

-3.5

-3.3

-1.9

-0.5

-2.1

-0.9

• 2.5

• 2.5

-1.0

-3.5

-0.6

-1.5

-1. *

-1.5

-0.2

-2.0

-1.7

-1. *

-2.2

-1.1

-0.8

-.58 2

-.671

-.658

-.955

• .719

-.05 7

-.16 8

-.80 3

-.00 1

-.76 9

-.615

• .880

-.960

-.*1 *

-.155

•1.909

-.83 1

-.96 7

-.72 1

-.36 0

-.6*9

-.171

-.129

-.960

-.239

• .940

-.611

-.356

.*35

.661

.883

.875

-1.0*0

-.6* *

-.56 7

• .001

-.16 2

-.071

-1.291

-1.08*

0.0207

0.3725

0.1916

0.6231

0.2893

0.1756

O.*72O

0.01*2

1.8337

0.7683

0.0988

3.2928

0.0*33

0.17*3

0.3022

5.1007

0.0626

0.6521

0.0*60

0.3*09

0.0553

0.0351

0.0652

0.1956

0.3738

9.4717

0.1130

0.0310

0.0258

0.7038

0.0275

0.5*88

0.0161

0.0119

0.0207

1.0266

0.0213

0.1698

1.06*7

0.1233

2.2210

0.1098

0.1188

.00320

.05770

.02970

.04650

.0*480

.02720

.07310

.00220

.28400

.11900

•01S30

.51000

.00670

.02700

.04680

.79000

.00970

.10100

.00713

.05280

.00856

.00543

.01010

.03030

.05790

1.46700

.01750

.00480

.00400

.10900

.00426

.08500

.00250

.0018*

.00320

.15900

.00330

.02160

.02630

.16490

.01910

.3*400

.01700

.01840

-11.36

-11.2*

-11.30

-10.9*

-10.99

-11.30

-11.40

-11.21

-11.32

-11.08

-10.79

-11.33

-11.35

-11.11

-11.01

-11.88

-11.24

-11.23

-11.74

-11.36

•11.29

-11.29

-11.08

-11.60

-11.25

-11.50

-11.43

-10.79

-11.25

-11.97

-11.09

-11.38

-10.93

-11.06

-11.24

-11.48

-11.97

-11.03

-11.37

• .58 0

• •01 0

• .05 0

• •54 2

•.37 40

•.16 1.5

-.10

• .41

• •22

• .00

• •23

• .44

• .84

• 1.06

• •36

• •26

• •07

• .48

-.03

• •05

• .11

• .14

• .60

• •74

• .15

• •69

• .59

• •31

• •12

1.7

0

••09 0.3

• .08 4

• •52 0

• .63 1

-.08 2

• •07 0

•.37 0.3

-.11 0

0

2

2.3

1

0.3

0.3

1.5

1.3

0

0

0

1.5

• .07 0

•1.01 1.5

•.08 00

• .04 0

-.07 0
56 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

Trail No. Date Sh.No. Apparent radiant sin Q 008 Zj, v^ M p m ^ H ^ H ^ H ^ H ^

7002

7022

7026

70*0

7044

7046

7052

7067

7069

7073

7075

7097

7158

7161

7169

7184

7188

7190

7210

7216

7240

7272

7277

7331

7313

7339

7367

7372

7388

7392

7454

7474

7476

7478

7480

7494

7496

7499

7520

7522

7524

7534

7560

7562

7592

53

53

53

53

53

53

53

53 '

53 '

53 '

53 '

53 '

53 <

53 '

53 '

53 '

53 '

53 '

53 '

53

53

53 '

53 '

53

53

53

53

53 <

53 '

53

53

53

53

53

53

53

53

53

53

53

53

53

53

53

53

( 19.44747

1 20.35965

) 20.38008

> 20.45639

) 20.47410

1 21.35019

1 21.38915

> 3.13834

. 3.19325

• 4.17184

. 4.17230

. 7.28372

. 9.37394

. 9.38246

• 10.14076

. 10.27490

• 10.33836

. 10.35115

• 11.18466

. 11.20551

. 11.34984

• 13.38363

. 13.40978

t 15.27683

• 15.28568

. 15.32599

. 16.13411

t 16.15595

> 16.30122

. 16.33582

. 21.44645

> 5.28417

> 5.30743

5 5.30847

> 6.15238

> 6.28495

> 6.29001

> 6.29997

> 7.2 7400

> 7.27581

5 7.28445

i 7.3195S

3 8.26788

> 8.27766

> 9.33792

210

262

223

190

228

158

252

173

219

205

173

21B

193

315

45

197

232

710

111

194

197

216

250

218

212

220

179

187

204

282

346

239

241

233

198

216

232

2 34

204

239

2 74

241

251

225

160

46

2

58

45

34

54

22

10

9

10

13

20

59

31

11

13

2

39

59

17

39

55

a

30

24

44

57

7

19

17

11

43

28

4

6

48

35

27

36

20

3

36

43

22

-12

• 66

• 37

• 37

• 30

• 0

• 26

• 28

• 48

-8

• 54

• 8

-3

• 32

• 55

-2

• 29

• 27

• 38

-23

• 3

• 0

-28

• 34

-9

-35

-8

-6

-2

• 64

• 25

-20

-14

-26

-7

-11

• 67

-6

• 3

• 66

• 53

-11

• 27

-2

• 35

13

24

5

58

28

13

0

55

57

12

39

39

9

56

8

31

37

32

41

40

40

24

8

51

25

44

13

45

19

55

40

46

23

17

10

20

48

49

18

8

54

42

2

0

16

.392

.316

.778

.238

.544

.439

.318

.387

.322

. 170

.694

.269

.366

.272

.052

.006

.430

.831

.301

.020

.409

.450

.154

.485

.267

.131

.028

.224

.359

.275

.307

.160

.171

.195

.064

.151

.331

.132

.593

.390

.305

.164

.401

.114

.155

.660

.652

.970

.806

.981

.658

.814

.832

.638

.366

.878

.819

.686

.319

.388

.813

.959

.989

.784

.461

.819

.815

.481

.948

.721

.366

.612

.626

.820

.643

.323

.546

.655

.513

.683

.720

.810

.761

.854

.807

.727

.708

.850

.818

.414

31.40

27.29

39.99

22.15

44.95

18.72

54.40

18.58

27.65

34.14

18.04

32. 71

23.07

49.19

18.00

23.12

38.93

29.49

13.71

31.89

21.89

30.92

60.68

25.65

31.46

44.63

21.94

21.12

23.51

27.56

47.21

36.83

33.77

31.95

18.91

21.45

13.67

28.11

18.13

21.03

36.11

35.05

37.75

26.43

13.25

• 1.3

• I.I

• 0.8

• 0.6

-0.9

• 1.1

-0.3

• 0.5

• 0.7

• 1.7

• 1.8

• 0.0

-0.7

-2.0

• 1.2

• 0.6

-1.3

-1.6

• 1.5

-1.9

-0.6

-0.9

-0.6

• 0.6

• 1.3

• 1.2

• 1.0

• 0.7

-0.7

-0.2

• 0.1

• 0.8

• 0.2

• 1.4

• 0.8

• 1.4

• 0.7

• 0.8

• 1.5

• 0.0

-1.8

• 1.1

• 0.2

• 1.1

• 1.5

89.8

100.8

101.0

89.1

108.1

95.2

110.9

86.5

90.3

96.0

86.4

103.9

88.0

113.9

89.1

106-0

106.2

80.5

106.8

86.6

104.2

111.8

86.9

104.6

108.3

94.8

96.5

87.5

93.8

99.OG

104.5

105.4

103.6

95.2

90.2

81.4

100.9

92.4

85.4

110.0

92.7

106.0

100.0

91.7

87.3

100.8

101.0

88.5

108.1

95.2

110.9

86.3

90.3

95.2

85.7

103.5

88.0

113.6

88.8

105.9

104.4

80.5

106.8

86.4

104.2

110.4

86.3

104.6

108.3

94.8

94.6

87.2

93.8

98.7

103.9

105.4

102.7

95.2

90.2

81.4

100.6

92.4

84.8

107.6

92.3

105.3

99.2

89.5

99.9

100.3

87.7

109.0

93.7

86.2

89.1

95.3

83.9

103.7

88.0

113.8

86.3

105.9

103.4

79.2

106.0

86.2

103.8

112.5

85.8

103.6

109.1

93. 1

96.5

87.5

92.9

104.5

105.2

103.5

93.0

89.6

81.4

99.0

89.3

84.2

109.9

91.6

105.4

98.3

83.3

94.4

95.3

84.3

96.2

86.6

84.9

83.0

93.5

80.8

93.7

84.0

94.0

85.5

97.5

83.1

74.1

88.9

83.8

82.2

99.5

78.9

94.2

104.2

87.5

90.2

R4.5

86.7

91.6

96.1

90.8

97.0

85.9

85.1

79.0

86.4

83.8

76.9

98.0

87.9

96.6

85.6

79. 1

8 8. 1

83.5

80.9

92.8

84.0

76.8

81.7

87.0

77.6

86.7

81.7

91.3

76.3

91.7

79.9

72.1

82.8

79.2

81.1

95.2

75.9

90.2

102.1

84.4

87.8

80.8

83.0

B9.2

91.4

84.9

91.4

83.3

81.1

77.8

84.9

78.5

75.0

91.1

81.9

91.0

81.6

79.1

86.4

83.0

80.0

92.8

83.9

76.5

78.7

87.0

76.8

86.7

R0.9

90.9

80.8

76.3

89.7

79.4

71.7

82.8

79.2

81.1

95.2

75.9

90.2

102.1

84.4

87.1

8 0. B

82.4

88.6

91.4

84.9

91.4

83.3

81.1

77.8

84.6

78.5

74.2

87.9

81.9

91.0

81.6

88.0
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 57

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

Vis.A Vis.E

7002

70 2 2

7C26

7C4C

704 4

7046

7C52

7C67

7069

7C73

7075

7C97

7158

7161

7184

7188

7190

7210

7216

7240

7272

7277

7331

7333

7339

7367

7372

7388

7392

7454

7474

7476

7480

7494

74S6

7499

7520

7522

7524

7534

7560

7562

7592

5 m

4 .

5 .

4 m

7.

5.C

I C .

3.

6.

4 .'

35.

2 .

5.

5.

5.

22.

4.

1C.

e.

4.

5.

e.

6.

3.

3 .

7.

12.

8.

7.

7.

5.

2.

3.

4.

7.

e.

5.

5.

2.

4.

7.a

7.6

2.4

) 3.7

3.7

7.6

5.9

5.3

10.4

14.6

) 2.8

8.8

5.3

> 36.8

• 4.5

5.3

2.7

) 3.2

26.2

• 4.4

i ..2.C

11.3

' 5.1

> 7.4

l R.a

7 8.6

I 5.8

) 4.2

1 8.1

7 9.9

3 10.5

: 13.6

7 8.3

1 5.1

5 2.3

1 6.4

. 4.6

D 7.0

9 12.4

3 7.0

1 6. /

? 6.4

9 5.1

.52

.74

.48

.53

• 3 5

.94

.28

.65

.70

.72

.63

.65

.46

1.49

.7C

. 44

.93

.85

1.64

.42

.93

.56

.47

.64

.38

.79

.74

.36

.66

.69G

.65

. 94

. 94

. 60

.33

.78

.93

. 69

.87

. 46

. 48

.87

22

27

28

2 2

5C

15

37

30

22

31

36

25

78

38

23

51

4 8

97

26

56

30

24

38

20

4 6

23

21

29

37

37

47

55

37

21

38

53

35

31

27

27

37

13

24

42

28

25

53

16

30

30

33 (

31

37

25

86

33

22

57

48

94

24

57

28

28

36

24

46

30

2C

35

25

36

58

46

28

21

39

52

37

38

25

28

49

10

•

>.

•

).

'•

,.

j .

(.

, .

; .

•

u

' • •

2 .

>_.

• 2.5

•i

• 2.5

0

0

• 1.5

• 1

) *2

. *2

) +3

> +3

> ^2

) 0

7 *1.5

1 *i

) +2.5

I +4

2 ^2

I +4

> •!

• 2

• 2

• 1.5

• 3

• 3

• 2

-1

• 2

• 1

0

• 2

• 1

• 3

• 1

• 3.5

• 2

• 3

• 1.5

• 3

0

• I

• 0.5

• 2

• 1

• 3

• 1.5

• 3.5

• 1

0

• 1.5

0

• 3

• 2.8

-

-

-

-

_

-

-

-

-

-

-

-

_

-

-

-

_

-

-

-

-

-

-

-:

_

-

-

-

-

-

.5

.5

.0

.9

m 2

.3

.5

.8

.0

.2

.6

m 2

.9

-C

j

.0

.2

.9

).6

.0

>.C

r m 2

i.2

).2

) . 1

).a

.2

1.7

'. 1

3.6

>, 2

.5

. 7

.0

) . 7

-2.2

-.961

-.905

-.750

-. 797

-.794

-.921

-1.122

-.517

-.411

• •510

-.755

-.195

• •088

-.836

• •522

-.460

• .000

-.362

-.880

-.857

-.8B3

-.762

-.716

-.582

-.530

-.378

-.609

-.319

-.664

-.899

-1.000

-.734

-.846

-.447

• -152

-.935

-.653

-.683

0.0355

0.2537

0.5675

0.0200

0.5081

0.0600

0.2731

0.1750

0.6392

0.5604

0.2912

0.2195

0.9820

1.2332

2.1500

0.6779

0.7005

0.0394

0.1653

0.0936

0.0297

0.3409

0.4139

0.4152

0.2964

0.0820

0.0994

0.2583

0.6831

0.2686

0.8781

0.1769

0.5301

0.9304

0.6127

0.0609

0.0859

0.2376

.00550

.03930

.08790

.00310

.07870

.00930

.04230

.02710

.09900

.08680

.04510

.03400

.15210

.19100

.33300

.10500

.10850

.00610

.02560

.01450

.00460

.05280

.06410

.06430

.04590

.01270

.01540

.04000

• 02120

.10580

.04160

.13600

.02740

.0B210

.14410

.09490

.00944

.01330

.03680

— 11. I"

-11.41

-11.02

-11.12

-11.46

-10.34

-11.10

-11.09

-10.86

-11.45

— 10 • 8C

-10.92

-11.13

-11.33

-10.83

-11.30

-10.79

-11.40

-11.24

-11.31

-11.18

-11.05

-11.12

-10.80

-11.16

-11.18

-11.69

-11.25

-11.34

—11.24

-11.06

-10.93

-10.93

-11.32

-11.10

-11.34

-10.86

-12.02

-11.21

-11.37

-.0 8

• .08

• .00

• •57

• •48

• •19

• •2 1

• 1.4 0

0 . 5

0 . 5

•.8 1 0. 3

-.01

• .36

• .16

••14

• •23

• .21

• •06

• •35

• •07

• •77

• .34

-.02

• .87

• .25

1.2b

• •64

• .19

• .74

• .12

-.03

• .14

• .32

• .12

• -38

-.04

• •02

• .74

-.02

• •35

• .11

• •09

1.3

Ou

0. 70

2

1.7

0.5U

1

1

1.5

0

0

0

0

0

0.5U

0.7

0.3

1.5

0

0.5

0

1.5

0

1

0

0

2

2.1

0.3

1.3

0

0

1

I

2

0

0.30

0

0.5

0

0

0

0

0

0

I

0.3d

0.5

1

0

0

ou

0

0 0

lu

0

0

2

2

0.3

0

0
58 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABU: 1.1.—Basic physical data for 41S Super-Schmidt meteors:

Apparent radiant sin Q

Trajectories.-

«BD "2.5

-Continued

"ML "ED

7607

7635

7637

7664

7666

7726

7734

7742

7744

7750

7754

7758

7787

7820

7838

7841

7871

7873

7882

7902

7929

7944

7946

8012

8017

8054

8068

8075

8083

8089

0106

8108

8110

R113

8127

8143

8147

8149

8153

8168

8187

8189

8192

8215

8224

9.37370

12.24694

12.24918

13.16918

13.18491

4.20432

4.24505

5.17470

5.17704

5.21477

5.25789

5.28705

8.28658

9.23606

9.34633

9.38816

13.35828

13.36281

13.41612

16.35285

20.39857

6.30795

6.31R27

15.25842

15.26933

16.28712

16.38349

16.41267 20

16.43128

20.36831

21.39199

21.40291

21.41963 3

23.42250

3.19528

4.21589

4.22409 1

4.25930 1

4.29693 7

5.24897 5

5.33668 5

5.34042

5.35035

5.43212

5.45574 7

308 51

236 21

238 14

206 23

258 5

261 7

213 13

299 7

235 12

223 33

249 10

309 43

305 42

2 34 32

241 1

343 13

271 45

322 11

246 19

317 35

340 16

2 74 9

261 51

295 1

282 18

22 29

50 6

321 58

357 39

283 38

324 25

335 26

312 9

30 35

301 19

284 12

315 26

310 0

36 53

340 2

343 39

299 8

344 0

55 24

36 42

• 68 6

-8 32

-21 42

• 0 46

• 57 14

-23 31

-6 42

• 44 56

-12 51

-12 56

-7 11

• 4 2

• 41 5

• 43 25

• 35 48

-8 17

-27 35

• 11 6

• 28 56

-4 35

-4 57

-8 2

• 26 37

• 2 58

- 3 59

• 5 45

• 50 45

-17 15

• 67 0

-12 11

- 6 21

• 56 0

- 1 13

-14 17

•5 31

-13 51

• 82 15

• 56 38

.293

.108

.009

.113

.410

.071

.411

.298

.110

.183

.432

.141

.370

.255

.212

.106

.274

.238

.125

.004

.015

.414

.798

.087

.186

.198

.218

.399

.103

.099

.321

.350

.325

.401

.228

.726

.150

.223

.280

.232

.036

.542

.169

.277

.411

.682

.679

.509

.791

.440

.360

.721

.382

.625

.701

.757

.461

.736

.982

.880

.426

.485

.764

.650

.661

.639

.736

.894

.837

.565

.451

.104

.780

.864

.825

.637

.824

.594

.760

.832

.994

.664

.763

.492

.598

.654

.778

.675

.601

.866

31.58

29.70

31.36

18.28

14.55

30.76

15.19

42.39

19.76

16.83

22.01

61.82

45.68

18.92

16.25

70.57

26.06

63.03

19.62

60.17

69.42

22.20

18.49

30.09

21.77

54.13

65.67

37.57

65.99

31.38

29.91

44.11

31.05

70.85

26.80

23.67

27.52

24.91

60.10

42.99

41.61

21.65

25.48

43.62

59.70

• 0

- 1

• 1

. 4

. 7

• '

1 0 0

9 8

8 9

. 4

. 2

. 8

1 0 0

9 8

8 9

. 4

. 2

. 8

9 9 .

9 8 .

8 8 .

2

3

0

9 4 .

8 5 .

8 4 .

0

3

1

8 7 .

H O.

7 7 .

2

6

7

8 6 .

8 0 .

7 7 .

8

6

7

• 1.2

• 1.9

• 0. 9

• 1.4

• 1.7

• 0.1

-0. 3

• 1.0

-0.2

• 0.6

-0.4

• 1.0

-0.2

-1.8

• 0.5

-0.7

-0.6

-1.5

• 0.5

-0.3

-0.9

-0.9

• 1.5

-0.4

• 1.4

-2.2

• 1.8

-0.4

• 1.7

• l. l

-1. 3

-1.1

• 1.0

• 1.3

-0.2

96.9

81.1

107.9

85.9

87.2

90.4

111.1

108.0

B5.4

112.7

99.8

111.1

91.5

110.8

112.9

99.2

88.1

102.8

96.2

111.5

109.8G

97.6

113.5

105.6

98.1

106.7

99.4

117.11

97.6

98.6

101.5

98.5

111.9

99.7

102.5

94.1

90.6G

100.8

109.3

96.9

80.1

107.6

85.9

87.2

89.6

110.4

107.4

85.4

111.7

99.0

110.2

91.5

110.0

111.8

99.1

87.7

102.4

94.9

110.5

109.7

97.2

110.8

104.8

98.1

104.

99.A

117.C

97.6

98. t

101.;

97. <;

m.s

102.!

92.S

90. t

100.8

96.8

79.0

107.5

85.2

85.9

88.7

113.2

106.5

85.3

113.9

98.3

117.0

90.0

111. 8

113.0

100.8

H8.2

102.5

93.7

112.3

97.4

112.5

103.5

97.8

106.2

98.4

118.5

96.4

96.7

100.8

97.2

114.1

98.2

101.8

89.1

101.7

110.1

92.1

78.0

99.0

78.1

81.3

82.6

100.9

95.6

95.8

83.4

98.9

91.7

87.5

64.0

81.5

88.8

104.1

107.2

86.0

94.5

94.5

89.3

95.0

89.2

102.2

90.5

86.6

97.9

91.1

99.8

89.0

94.8

86.8

89.1

93.8

100.3

89.1

73.4

96.4

74.1

77.9

78.5

95.7

91.4

76.7

98.1

85.6

91.0

78.S

95.9

90.9

HO. 1

49.)

79.1

85.3

96.5

104.2

80.6

91.7

83.1

84.6

86.8

85.6

94.8

86.5

82.3

96.1

87.8

96.4

89.9

82.4

83.6

86.2

89.1

73.4

95.4

73.7

77.9

77.8

95.5

90.1

74.8

97.9

85.6

90.9

78.1

95.7

90.3

79.8

49.3

79.1

84.9

96.1

101.9

80.6

91.7

83.1

84.6

86.8

85.6

94.8

86.•>

82.3

96.1

86.3

96.4

84.3

89.5

82.4

83.5
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 59

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

Vis.A Vis.I

7637

7666

7726

e

4

p

.e

.7

1C.

4 .

1 1 .

2

1

1 . 1C

. 6 2

.7(1

5.4

3.6

77*2

77',',

7750

7754

7758

7787

7820

7838

7841

7871

7873

7882

7902

7929

7944

7946

8012

H017

SC54

8068

8075

aces

8089

H1C6

8108

8110

8113

H127

8143

H14 7

814 9

815 3

816 8

8187

8189

8192

15. 3

5 . 7

3 . 5

4.4

15.fl

e.c

7 . 1

4 . 7

11. 1

12. 2

1C.2

7 . 3

8 . 2

14. 4

8 . 1

19. 7

1C.3

S . 1

14. 7

21.4G

e . 2

5 . 1

11. 8

S .4

7 . 6

1C.4

7 . 8

5 . 7

4 . 1

1.9

2 . 3

13. 3

9 . 1

e.4

4 . 9

4 . 2

11. 2

5 . 9

6 . 1

15. 7

9 . 8

3 . 4

3 . 9

15. 0

17. 0

11. 8

9 . 1

1C. 7

16. 8

I C C

13. 5

13. 1

9 . 4

7.H G

12.O G

1C. 2

7.6

9 . 4

11. 2

4 . 1

11. 9

7 . 4

5 . 4

3. 1

2.9

3.C

15. 4

1C.2

7.6

4 . 1

5 . 1

1C.3

.78

1.C2

.8C

.77

.55

.53

1.17

.79

.49

1.14

.42

1. 10

.3H

. 5 1

1.21

2.5 5

.97

.94

.60

.81C

.59

.35

52

1C3

• 1.5

- 1

• 1.5

• 2

• 2. 5

• 0.5

• 0.5

-1. 9

• 0.0

-2. 0

-O.I

-0. 6

-1. 8

-1. 3

-0. 6

-1. 2

-2. 1

-2. 6

-0. 5

-0. 7

-0. 2

-1. 1

-1. 0

-0. 7

-0. 1

-1. 6

-0. 9

-l. S

-0. 8

• C.3

-0. 4

-1. 8

-1. 3

-2.1)

-o. ;

-I. I

-1. 6

-0. 7

-2. 4

-1. 5

-1. 0

-2. 0

- 0 . i

-2. 0

• .368

-.81 4

-.69 9

-.00 2

-.77 8

• •100

-.26 5

-.396

-.392

• •030

-.776

-.31 4

-.74 3

• •015

-1.061

-.329

-1.214

-.85 8

• .U89

-.70 2

-I.17 8

-.85 4

-.78 1

1.5618

0.5772

1.36H8

0.0620

0.4778

0.3480

0.8264

0.0446

0.0297

2. 1952

1.3443

0.0239

0.3758

0.0368

0.7044

0.0316

0.0717

0.8U06

11.8413

0.7916

0.3422

0.1569

0.0387

0.1530

0.0284

0. 70 31

0.1291

0.1136

0.1240

0.0594

0.0917

0.7231

0.05H8

0.1840

0.1130

0.1433

0.0568

0.1440

0.1743

0.0403

0.0194

.01850

.03400

.24190

.08940

.21200

.02010

.06500

.00960

.07400

.05390

.12800

.00690

.00460

.34000

.20820

.00370

.05820

.00570

.10910

.00490

.01110

. 12400

1.83400

. 12260

.05300

.02430

.00600

.02370

.00440

.10890

.02000

.01760

.01920

.00920

.01420

.11200

.00910

.02650

.01750

.02220

.00880

.02230

.02700

.00624

.00300

-11.04

-10.97

-10.95

-11.12

-10.54

-11.26

-11.25

-10.89

•10.94

-11.13

•11.38

-11.16

-11.2*

-11.37

•11.25

-10.93

-11.10

-11.29

-11.53

-11.17

-11.47

-11.55

-11.2*

-10.07

-11.25

-11.73

-11.U

-11.06

-11.29

-11.02

-11.31

-11.43

-11.10

-11.01

-11.26

-10.79

-10.93

-11.39

-11.17

•10.56

•10.90

• •14 0

• •11 0

• .03 3

-.1 7 0.30.

• .46

• •28

t . 34

• .33

».3O

t.8 5

• .1 5

• •1 7

• •4 9

•.4 5

• .26

• .42

• .06

• -21

• -3 0

-.0 1

• .36

• •02

-.0 7

• .1 3

• .0 2

• -2 3

t.0 4

• .4 0

0.3

0.5

• .3 1

• .0 4

• -3 3

-.8 5

2.3

00

•.5 4 0.3
60 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

nt radiant sin Q

8238

8240

8244

8254

8294

8307

8344

8368

8394

8401

8413

8415

8417

B447

8463

8469

8476

8510

8546

8572

8576

8609

H640

8645

U648

8658

8668

86 79

8719

8726

8766

8793

8817

8819

8881

8891

8917

8943

8945

8951

8974

8976

8990

9015

9030

8 6.21211

8 6.22121

8 6.24351

8 6.29543

8 7.39845

8 8.19278

8 8.39184

8 9.21638

8 10.22697

8 10.24674

8 10.30711

8 10.30810

8 10.32681

8 11.42992

8 13.45529

8 13.24211

8 13.28005

8 13.42525

8 14.29511

8 14.43341

h. 43670

53 12 14.

53 I? 13.

53 12 15.

,3091

14920

.8317

53 8 10.44060

53 8 10.45569

53 8 11.4680ft

53 8 14.19444

53 8 14.29057

53 9 30.19335

53 10 2.28006

53 10 2.35018

53 10 2.15251

53 10 6.24826

53 10

53 10

53 10

53 10

53 10

53 10

53 10

53 10

i.29615

7.39307

>.19222 9

».19547 2

9.23348 9

9.31756

.31647

9.47638 2C

a

343 19

298 19

264 18

342 5

271 40

h

48 36

280 15

289 19

307 7

23 50

34 14

30 25

152 29

112 46

130 41

46 50

314 S7

46 10

49 36

47 28

6 23

345 3

119 12

24 53

269 51

309 59

13 5

278 23

32 4

-14 43

• 35 48

• 25 52

-13 31

• 22 5

333 58 -13 37

348 18 -13 15

319 7 -0 39

272 37 •O 31

42 51 +58 47

279 45 ^64 29

274 38 -8 33

338 32 O 11

287 48 ^32 51

45 46 +58 3

• 58

-22 18

• 1 0

-35 11

• 48 24

-42 16

• 32 21

• 1 21

• 56 56

-3 32

• 57 14

• 57 57

• 56 45

-2 59

• 38 34

• 36 36

• 44 26

• 33 32

• 72 3

• 3 8

• 48 33

• 9 52

53 10 10.29028

53 10 10.39572

24 13 - 1 20

121 26 ^66 35

39 1 M2 13

32 37 +8 14

19 11 *13 38

.088

.670

.061

.087

. 183

.407

.004

.497

.266

.0d2

.403

.207

.095

.219

.269

.13 8

.38 5

.25 5

.041

.310

.086

.148

.061

.560

.260

.501

.270

.223

.224

.028

.287

.202

. 132

.152

.424

.087

.206

.32 6

.74 5

.221

.084

.349

.279

.986

.885

.598

.330

.697

.719

.794

.365

. 753

.479

.861

.418

.155

.421

.551

.834

.33 3

.73 3

.21 9

.<>84

.804

.820

.377

.866

.204

.471

.662

.956

.329

• 97S

.330

.623

.699

.669

.615

.831

.454

.713

.878

.797

41.26

28.77

16.50

41.72

13.73

41.23

27.99

14.52

59.93

26.29

14.12

29.18

20.83

60.52

• 0.5

-0.8

• 1.8

• 1.6

• 0.5

• 0.7

• 0. 5

• 1.0

-1. 6

• 1.6

• 1.5

-1.1

• 1.2

-0.1

103.7

102.0

89.2

102.4

83.4

101.3

101.3

100.9

8 0 . 7

115.7

102.8

80.7

88.2

96.1

113.0

103.7

102.0

87. 9

102.4

83.3

101.0

101. 3

100.9

80.7

115.3

102.8

80.6

88.2

96.1

112.8

17.74

18.79

64.21

52.79

61.91

55.74

36.20

58.59

60.46

22. 78

60.80

60. 13

61.10

24.01

26.59

68.89

45.45

17.02

32.72

20.63

20.20

31.06

25.66

57.96

26.95

30.33

24.07

-t. 5

• O.B

-0.4

• 0.5

-1.2

-1.6

-3.5

-0.8

-0.9

• 1.2

-2.5

-2. 0

-3.6

-0.4

• 1.2

• 0.7

• 0.3

• 0.0

-0.2

-1.9

• 0.6

• 1.6

-0. 1

•1.2

84.2

90.0

112.8

112.8

107.8

111.20

102.2

112.?

113.7

98.3

119.7

99.40

118.2

101.6

101.8

113.4

101.9

96.5

104.7

87.5

103.8

102.2

103.5

88.1

112.4

100.2

103.5

99.6

84.0

89.7

1 12.8

107.0

110.7

102.2

111.5

112.9

98. 3

118.9

99.2

118.2

101.1

101.0

113.4

101.9

96.5

103.7

87.5

103.5

102.2

103.5

88.0

112.0

99.2

102.7

96.9

104.6

101.4

87.4

100.4

83. 3

100.7

100.7

100.1

76. 7

116.5

99. 7

80.6

H8.3

93.9

114.2

.326 60.59 -2. 6 117.5 117.5 119.1

83.9

8R.2

112.4

115.0

108.5

108. I

114.9

113.7

97.8

118.2

119.9

100.0

97.9

119.5

101.1

93. 7

105.2

86.0

102.H

98.2

102.5

87. 5

115.0

97.7

100.8

95.9

96.0

85.6

80.0

95.9

82.9

92.9

94.3

88. 7

72.8

98.0

88.4

80.2

87.7

85.9

109.4

95.6

80.2

83.7

102.2

105.4

97.9

100.5

68.6

93.5

100.6

92.0

90.1

98.4

93.6

105.4

90.8

81.1

84. 7

78.9

96.3

90.9

97.0

84.1

103.8

93.2

82.5

88.1

"ED

92.5

81.0

72.6

92.0

d2.0

88.4

86.9

69.4

96.2

86.8

75.0

81.2

03.6

107.5

91.4

02.0

re. i

71.0

102.1

91.2

96.8

64.1

91.9

93.9

92.5

83. 3

94.4

90.9

81.5

84.0

103.0

84.2

79.2

87.7

76.4

95.9

85.2

98.8

79.4

102.5

83.3

75.8

79.1

92.5

81.0

72.6

92.0

80.6

88.8

88.4

86.9

69.3

96.0

86.8

75.0

01.2

83.5

106.9

91.4

82.0

77.4

70.8

95.6

102.1

91.2

96.8

64.1

91.9

93.9

90.3

81.S

94.4

90.9

81.3

83.6

102.3

84.2

79.;

87.7

76.4

90.6

85.2

91.3

79.4

102.5

83.3

75.8

79.1
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 61

TABLE 1.1.—Basic "physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

nB

£U Vis .A Vis.B C.I.

8238

82*0

8244

8254

8294

8307

8344

8368

8394

8401

3413

8415

8417

0447

J46 3

8469

34 76

8510

8546

8572

8576

S6C9

8640

8645

8648

8658

8668

8679

8719

8726

8766

8793

8817

8819

8881

8891

8917

8943

8945

8951

8974

8976

8990

9015

9030

17.7

3.1

2.9

6.0

4.7

It.2

5.2

7.6

7.3

27.5

2 . 9G

6.4

2.4G

16.7

IS • 8

41.3

9 a 0

K . 2

13.8

3.7

11.7

9.5

34.OC

9.4

6.7

6.4

11.8

13.3

12. 4G

26.4

5.0

5.8

13.3

6.2

3C.7G

13.2

e.e

1C.3

9.1

11.6

4.4

10.9

9.5

S.8

ICC

15.8

5.8

3.8

6.C

5.9

i a . e

6.6

9.2

3.9G

26.7

8.4

6.4

3.4

14. 8G

18.3

4C.3

5.5

1C.3

16.9

5.9

12.9

1C.3

31.6G

15.2

6.2

5.}

12.3

6.7

7.7G

24.0

8.1G

4.1

14.9

4.4

32.5G

13.1

7.3

8.5

5.9

10.6

4.5

10.9

8.4

13.6

9.3

1

1

1

1

1

1

1

1

1

3

1

1

1

1

.95

.75

.17

.42

.64

.02

.46

.70

.C3

.90

.82

.85

.2a

.50

.65

.33

• 85

.93

.89

.32

.60

.37

.18G

.10

.43

.40

.97

.72

.40G

.96

.30

.73

.49

.38

.48G

.85

.78

.10

.90

.33

.42

.38

.90

• Cb

.C9

53

2ft

31

23

20

50

26

42

58

53

j 3

46

13

89

3C

79

5 2

49

110

19

35

2C

67

41

24

23

42

41

24

59

74

36

26

24

173

47

48

26

49

19

24

22

46

6C

54

40

44

54

17

0

50

25

40

30

53

4 3

45

17

60

j5

78

47

104

18

30

21

68

63

20

23

37

29

15

49

59

39

21

23

130

48

39

0

18

25

22

20

44

58

53

2.5

3.7

1.5

1.4

3.1

2.4

2.3

2.1

2.8

3.8

1.9

4.3

1.9

4.5

5.0

2. 7

3.0

1.7

3.6

4.1

5.9

2.9

4.0

1.9

5.3

4.4

5.6

3.8

2.1

1.2

2.0

3.2

2.6

2.9

1.6

1.6

1.7

5.4

1.7

1.4

3.6

2.0

• 2

• 1

• 3

• 4

• 2

• 1.5

• 1

0

0

• 1.5

• 2

C

• 2

• 1

-1

0

0

0

0

-2

• 3

• 3

• 1

• 1.5

• 1

• 2

• I

• 2

• 3

• I

i 1

• 2

• 1

• 2

• 2

• 1

0

• 2

• 1

• 1

0

• 0.5

• 1

• 2

-1. 5

-2

• 2

0

• 2

-1

• 1

• 2

• 2

• 1

H

• 1

• 1

• 2

• I

• 3

• 1.5

• 2

-0.9

-2.4

-1.1

-3.0

-0.8

-1.0

-1.0

• 0.0

-1.4

-0.6

-2.5

-0.4

-3.5

-1.6

• 0.0

-1.7

-2.5

-0.2

-2.0

-1.1

-0.9

-0.9

-1.8

-1.8

-1.6

-1.2

-1.0

-0.8

-1.1

-1.2

-0.6

-0.8

-0.3

-0.8

-3.8

-0.6

-0.9

-1.8

-0.5

-.392

-.150

-.746

-1.145

-.711

-.485

-.919

-.673

-.628

• .403

-.HUB

-.626

-.466

• .834

• •065

-.292

-.561

-.182

• •571

•1.007

-.296

-.222

-.555

• •478

•1.147

-.010

-.883

-.461

-.645

• •170

-.18H

-.626

-.318

-.885

-.264

-.238

-.743

-.852

-.176

-.591

0.1162

0.6224

0.8716

0.0200

2.2598

0.1433

0.0349

0.2008

1.7058

0.2370

0.16 72

0.9620

0.2002

0.8071

0.6179

0.5398

4.2484

1.6658

0.0200

0.0378

0.0567

0.4358

4.4034

0.0510

0.0549

0.5146

0.2705

1.2913

1.4882

0.1453

0.0213

0.0491

7.4379

0.3B03

0.5740

1.8724

0.0910

2.1307

0.7186

0.0187

0.1524

0.4662

0.3893

.01800

.09640

.13500

.00310

.35000

.02220

.00540

.03110

.26420

.03670

.02590

.14900

.03100

.12500

.00630

.09570

.08360

.65800

.25800

.00310

.00585

.00878

.06750

.68200

.00790

.00850

.07970

.04190

.20000

.23050

.02250

.00330

.00760

1.15200

.05890

.08890

.2V000

.01410

.33000

.11130

.00290

.02360

.07220

.06030

-11.18

-11.20

-11.08

-11.44

-11.25

-11.20

-11.32

-11.20

-10.90

-11.32

—11.08

-10.56

-10.90

-11.22

-11.49

— 11.18

-10.98

-11.22

-10.87

-11.65

-11.42

-11.59

-11.56

-11.06

-11.43

-11.32

-11.55

-11.25

-11.32

-11.36

-11.08

-11.39

-11.15

-11.14

-14.09

-11.45

-15.67

-10.69

-11.23

-11.40

-11.50

-11.26

• .69

• •15

• .14

• 1.02

• •21

-.13

• .36

• .37

• .18

• •57

• • 35

• •49

-.08

• .46

• •04

• • 29

• .75

• .15

• .78

• .09

• •02

• .15

• .11

• .19

• •31

-.28

• .55

• .22

• •01

• 1.73

• •15

• •12

-.01

• •34

• 1.32

• •09

• 2.46

-.01

• .62

• .03

• •20

• .00

0.3

0.5

00

0

0.5

1

0

0.3

2

0.5

1Q

1

0

1

Q

2

0.5

4

10

0

0

0.3

2

4

0

0.7

2

i

1

3

2

0.5

0

1U

2.5

0.3

2

0

0

0

1

0

00

0.5

0

0.5

0

0

ou4

0

1

0

0.5

0

Q

0

1Q

0

0

Q

2.5

0

0

0

0

0

0

0

0

3

0

0

0

0

0

00

ou00

0

1

4

0

4

0

0

0

0

0

225-636 O-67—5
62 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 418 Super-Schmidt meteors: Trajectories.—Continued

Apparent radiant sin Q "2.5 •ED

9062

9087

910*

9130

9147

91*9

9170

9172

9238

9240

92*6

92S2

9257

9265

928*

9331

9335

9375

9379

9*11

9*16

•Ml 8

9*51

9507

95*7

9611

9627

9631

9656

9660

9709

9719

9725

97*2

97*9

980*

9815

9833

9880

9888

9900

9917

9925

99*5

9951

5

S

5

5

5

5

5

5

S

5

5

5

5

5

5

5

5

5

5

5

10

10

10

11

11

11

11

11

11

11

11

11

11

u

11

11

11

11

12

12

53 12

5

5

5

5

5

5

12

12

12

12

12

12

53 12

5 12

53 12

53 12

53 12

53 12

53 12

5

5'

5<

5

5

5'

5<

51

54

54

51

12

3

3

12

. 1

> 1

1 1

1 1

1

• 1

1

12.**075

16.*6267

2O.*7562

2.120*8

2.29009

2.30611

3.20197

3.21307

7.37*03

7.37850

7.*3*75

7.*6139

7.*8135

9.255*7

10.36*21

13.35062

13.359**

26.17665

1.13503

*.**6*8

7.39528

7.*0209

9.37006

11.3957*

12.35211

13.31978

13.36039

13.36283

13.*3186

13.*3706

13.52675

1*.3*826

I*.37895

l*.*0185

l*.*0912

9.*7776

8.29651

29.2**03

1.3185*

l.**056

2.27567

3.21**6

3.32581

3.*2157

3.*5117

2

2

2

2

17

17

17

16

20

t

l(

t

>

10

1*0

36

* 3

285

91

68

5B

20

55

52

55

37

55

5*

60

62

101

5*

22

122

80

105

109

111

11 1

111

112

112

113

128

114

113

1 1 *

113

1 1 *

252

2*1

9 *

107

36

94

80

126

232

166

20

*5

* 0

30

16

10

26

5*

17

* 3

*5

1 *

58

23

3

1 *

* 7

57

* 6

2

1

57

11

* 6

25

38

29

39

25

* 3

13

22

12

4 1

6

50

* 9

1 8

5 6

1 6

3 9

2 8

1 7

5 7

5 5

• 2

- 1 9

• 12

• 32

• * 3

• 50

- 1 9

*22

• 1 *

• 13

• 15

• 16

• 22

• 22

- 1 6

• 23

- 1

• 1 *

• * 7

• 2

• 16

• 32

• 33

• 33

• 32

• 32

• 31

• 32

• 32

• 1

• 32

• 31

• 32

• 32

• 32

- 1 5

• 16

- 2

- * 0

• 7*

• 80

• *

- 6

• *9

• 28

3 0

2 6

1 0

* *

* 9

2 6

5 6

*2

10

37

39

5

26

50

9

46

44

26

5

55

0

6

8

12

37

17

54

26

25

52

59

56

19

8

23

42

51

38

57

59

32

23

53

18

21

.186

.328

.225

.258

.321

.516

.095

.265

.472

.460

.568

.357

.289

.387

.003

.097

.149

.230

.429

.066

.085

.205

.234

.293

.189

.351

.171

.232

.315

.036

.154

.355

.336

.405

.271

.072

. 2 3*

.176

.039

.171

.255

.173

.058

.262

.249

.3*2

.357

.651

.776

.7*3

.907

• 322

.976

.906

.881

.765

• **8

.612

.933

.639

.978

.73*

.823

.957

.866

.8*1

.993

.997

.999

.98 7

.950

.993

.99*

.969

.859

.7*3

.984

I . 000

.995

.991

.612

.345

.785

.285

.423

.669

.874

.750

.450

.989

62.23

19.80

30.30

17.98

58.79

4H.46

33.83

25.10

28.35

26.20

29.34

19.84

30.40

30.53

26. 34

30.75

58.52

21.96

19.63

60.39

25.61

36.30

35.23

35.39

36.26

36.92

36.61

36.2 7

36.04

58.66

35.89

36.43

36.10

36.76

36.23

72.78

59.73

24.94

25.97

18.93

23.87

16.44

44.57

41.45

60.40

• 0.2

• 0.2

-0.1

• 1.4

-0.1

-1.9

• 1.3

-1. 7

• 0. 2

• 0. 3

• l. l

• 1.7

-1. 2

• 1.0

-1. 2

-1.9

-1.5

• 1.0

-0.3

-0.9

-0.4

-0.9

• 0.0

-0.4

-1.0

-0.8

-0.8

-0.2

-1.3

-0.5

-0.2

• 0.9

-2.4

-1.0

-2.5

-3.8

-2.3

-0.2

-0.1

• 0.5

• 0.2

• 1.8

-1. 2

• 0.*

• 0.0

112.6

88.8

100.9

92.5

111.0

95.5

105.0

102.9

100.6

9H.0

102.7

86.2

103.7

100.0

92.3

105.3

109.9

88.5

99.9

111.*

100.2

98. I

101.5

98.6

100.5

100.2

101.0

98.4

102.9

111.5

99.5

101.3

92.20

98.0

100.3

117.5

103.8G

88.6

93.3

96.5

93.8

90.9

106.3

101.8

108.5

111.9

88.8

100.3

92.5

110.2

94.6

105.0

102.9

100.6

97.9

98.7

86.2

103.7

99.9

91.4

104.9

109.2

88.1

99.9

111.4

98.3

98.1

101.5

98. 5

99.5

100.2

99.8

98.4

102.9

109.0

98.8

100.3

92.2

96.8

100.3

112.5

103.5

88.4

93.3

96.2

93.8

89.7

104.2

101.8

108.5

116.0

88.7

102.3

90.0

113.8

94.7

104.4

102.2

99.4

98.3

100.9

H4.6

103.8

98.7

93.0

105.2

112.6

87.9

96.6

115.5

101.8

100.2

102.2

99.9

101.9

100.2

100.7

99.6

105.8

110.5

98.*

100.2

101.7

100.5

117.7

88.6

93.9

96.2

92.5

87.7

107.3

102.*

1 12.4

104.0

88. S

8*.2

85.2

97.1

87.2

97.i

82.9

87.2

8*.6

86.1

81.2

79.9

88.0

80.5

8*.3

92.0

85.5

89.6

93.2

82.9

83.3

86.9

90.3

83.0

89. 1

88.9

8*.O

85.6

92.1

90.3

87.0

70.*

81.2

8*.I

97.0

100.1

86.7

86.9

85.1

82.6

77.8

98.5

95.8

95.5

101.9

86.3

82.7

81.7

90.7

78.6

9*. 3

77.1

82.6

81.0

8*.7

79.1

75.9

a*.1

7*. 7

78.2

88.5

79.8

83.6

85.5

76.2

78.0

«3. 2

82.0

80.7

83.9

8*.7

80.5

83.5

89.6

86.*

8*.9

59.*

79.5

70.6

93.3

96.2

78.9

80.7

77.5

76.3

75.1

91.0

93.7

91.5

101.5

8*.9

82.4

81.3

90.7

78.6

94.3

77.1

82.6

80.3

84.7

79.1

75.6

84.1

74.7

78.2

88.5

74.4

82.1

85.5

76.2

77.4

82.1

81.6

80.7

80.9

83.6

79.4

80.9

88.9

84.7

83.6

59.4

78.5

70.6

93.3

96.2

78.9

78. 7

77. 01

76.2

75.1

91.0

93.7

91.5
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 63

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

Vis.A Vis.E

9C62

JC8 7

1 I M

9130

9147

9149

9170

9172

9238

9240

9246

9252

S257

9265

43 3 1

9335

9375

9379

9 41 1

9 4 U

9 418

9451

95C7

9547

961 1

9627

9631

9656

9660

97C9

S719

9725

9742

9749

9804

9815

9833

9880

9888

99C0

9917

9925

S945

9951

6.5

6.8

lea

8.2

11.5

5.6

12.2

7.4

t.3

7.8

6. 1

7.4

19. 7

4.R

7.6

1C.6

9. 1

t.9

fi . 4

4.6

5.C

6. 7

5. 3

7.4

8.C

t.O

t.2

5.5

6.8

5.8

5.6

12.1

5.4

5.C

12.9

1C.9G

4.4

19.C

23.2G

14. 1

6.3

5. 1

S.8

5.4

16.3

5.1

13.9

6.2

12.C

4. 7

14.0

6.3G

5.4

7.2

4.3

5.9

14.0

6.5

7.8

12. )

4.1

6.2

8.4

6. 1

5.6

5.2

5.1

7.2

7.6

4. 1

6.4

5. )

7.B

3.5

5. 7

13.1

5.5

8.5

9.6

11.2G

5.0

16.7G

24.9C

11. 4G

7.2

7.a

8.8

5.0

.52

.61

. 96

.88

. 47

. 39

. 86

1.07

.72

. 79

. 81

.81

1.51

.57

.92

.50

.81

. 93

.50

1.C5

.5d

.5h

.4n

.55

.55

.4H

.51

. 63

.45

.56

.50

.95G

.54

. 84

.54

.380

.50

1.99

2.57G

1.14

1.17

.46

.45

.29

C

2 2

3a

4 9

28

19

52

65

41

41

2S

4 4

8 4

34

54

30

2 8

52

2 7

51

29

28

27

28

29

26

30

33

23

29

25

54

28

50

27

22

29

ICO

105

61

66

23

28

14

28

22

55

42

25

23

47

42

28

33

36

35

85

34

48

27

20

42

27

61

30

26

26

30

28

18

30

33

20

2 1

27

29

48

20

20

25

74

143

57

57

21

21

16

.5

1. 3

j ^ I

>.H

• . 8

.3

3.0

? . 2

'.6

.8

.9

. 3

> a i

..8

. 1

> . 3

t.9

i B \

'.6

i.O

'.6

S.C

i.C

3.6

i.6

? • 4

S.4

).2

B.3

> . 2

3 . 7

. .9

i. I

i. 7

.4

>. 5

?. 7

'.8

.9

.9

.9

? B I

• 2

• 2

• 1

• 1

• 4

C

• 3.5

• 3

• 3

»3

0

• 2.5

• 2

• 1.5

• 1.5

• 2.5

• 1

• 1.5

• 1 .5

• 1.5

• 1

• 1

• 2.5

• 2

• 1

0

-1

-1

• 1.5

• 1.5

• 3.5

+ 1.5

• 3

• 2

• 1

• 1

• 1.5

• 1

• 0.5

• 1

• 1.5

•1

• 2

• 2

0

• 2

• 1

0

• 0.5

• 1

• 3

• 2

• 2

• 1

• 1

C

• 1

• 1

• 0.5

• 1.5

• 1.5

• 2

0

• U.5

• 1

• 3

• 2

• 1

• 1

• 3

• 2

• 2

-0.8

-1.2

-0.6

-1.0

-2.6

-2.3

-2.2

-2.4

-1.9

-1.5

-1.0

-1.5

-1.3

-1.5

-1.4

-1.8

-1.0

-1.7

-1.1

-2.0

-1.4

-1.3

-0.6

-1./

-1.3

-1.4

-0.3

-1.2

-1.5

-2.6

-0.8

-2.1

-1.?

-2.9

-1.9

-2.2

-l.l

-0.6

-0.9

-1.6

-2.4

-I.a

-1.2

-.443

-.206

-.818

-.444

-.009

-.631

• -374

-.627

-.448

-.654

-.923

• •357

-.796

• a 1 9 1

• .368

• .046

-.567

-.267

-.146

-.216

-.070

-.557

-.402

-.208

-.295

-.424

-.406

• .017

-.424

-.508

-.814

-.143

• .583

• .776

• .337

-.698

• •059

-.033

-.317

-.788

-.206

-.630

-.686

0.0303

0.5101

0.4746

0.5520

0.0355

0.1756

0.1241

3.0410

0.2189

0.4223

0.1821

0.3209

1.7381

0.1162

1.7 362

1.6690

0.1130

0.5527

1.4773

0.0659

0.7851

0.3603

0.1298

0.1788

0.2615

0.2034

0.1537

0.1711

0.4455

0.0374

0.1382

0.0646

0.2989

1.6400

0.3151

0.2034

0.2712

1.3798

2.9700

0.7496

0.8710

0.1427

0.0671

0.0187

.00470

.0/900

.07350

.08550

.00550

.02720

.01922

.47100

.03390

.06540

.02820

.04970

.26920

.01800

•2689C

.25850

.01750

.08560

.22880

.01020

.12160

.055B0

.02010

.02770

.04050

.03150

.02380

.02650

.06900

.00580

.02140

.01000

.04630

.25400

.04880

.03150

.04200

.21370

.46000

.11610

.13490

.02210

.01040

.00290

11.17

11.00

11.32

10.96

11.30

11.41

11.25

11.01

11.26

11.33

11.34

11.04

11.55

1 1.3(1

11.03

11.32

11.49

11.17

10.68

11.44

11.36

11.10

11.34

10.50

11.18

10.89

11.30

11.20

10.80

11.37

11.43

10.86

11.90

11.41

11.37

11.16

11.11

11.12

11.29

11.14

11.18

11.13

11.43

11.65

• .14

• .64

-.28

• .19

• .03

• .60

-.10

• .27

-.09

• .08

• •39

• .25

-.05

• •10

• .16

-.08

• .11

• . 14

-.01

• •03

-.14

-.07

• •29

-.06

• .16

• •23

• .09

• •07

• •47

-.02

• .45

• •25

• .18

• -16

• •15

-.06

• •29

• •33

-.08

-.08

-.06

-.09

• •36

• .44

• .27

0

0.3

0

2

0

3

0

3

0

u

oa

I

0.3

0

2.5

2

1

0.3

2Q

0

0

1

1

0.3

1

2

1.5

0.5

2

1

1

1

2C

2

3

2.5

2

0

2

10

1

0

1

0

0

0

3

0

OQ

0

0

0

0

0

0

0

1

0

0

0

0

0

2

3

0

0

0

0

0

0

1

0.50

0

1.5

0

2

O.b

0

0

0

0

0

0.3

3

0

0

0

1.5

1
64 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.1.—Basic physical data for 418 Super-Schmidt meteors: Trajectories. —Continued

Sh.No. Apparent radiant sin

9953

9955

9974

9983

9985

9997

10006

10012

10064

10070

1009*

10098

10106

10127

1017J

10218

10222

10240

10247

10252

10255

10273

10279

L0281

10342

10358

10365

10380

10384

10394

10414

10439

10447

10478

10480

10531

10555

10566

10583

10587

11816

11818

11825

11856

11862

54

54

54

54

54

54

54

54

54

54

54 '

54 '

54 '

54 '

54 <

54 '

54

54

54

54 '

54

54

54

54

54

54 <

54 '

54 <

54

54 '

54 '

54

54 '

54

54

54

54

54

54

54

54

54

54

54

54

3.45659

3.45699

3.48882

3.49569

3.50371

3.52012

4.45827

4.53118

9.42393

11.37924

10.47485

. 6.23252

. 1.37265

» 28.45642

27.16305

5.30805

5.33948

1 5.45765

6.42134

6.48481

> 6.49676

6.37011

8.44085

i 8.4 7246

) 26.27791

. 1.30207

. 1.34746

. 2.34276

. 2.37276

» 2.42132

• 5.19665

. 5.38519

i 5.41316

t 6.26447

t 6.29420

t 7.46231

• 12.42529

. 30.25718

i 4.39391

) 4.39369

> 3.15099

5 3.17971

i 3.23657

5 3.43132

5 3.45107

10

10

10

10

10

10

10

no

6Q

19

228

224

228

229

231

227

230

176

118

114

317

230

190

240

139

168

227

178

182

251

329

250

186

166

155

198

178

210

207

164

143

207

202

177

165

267

197

252

3

298

156

116

209

214

335

11

10

48

19

10

57

2

15

46

53

55

58

48

49

36

53

57

2

13.

5

38

58

21

19

0

21

56

55

15

23

54

54

28

21

25

22

28

0

31

7

45

42

17

20

•48

+ 51

• 48

• 48

• 48

• 48

• 48

• 23

• 8

• 14

• 32

• 16

-22

-I

• 23

• 7

-9

-20

-1

• 28

• 35

• 48

-0

- 1

• 65

• 4

-23

-19

-15

• 38

-20

-13

-19

-24

- 3 8

• 30

• 53

• 0

• 65

-47

• 35

-14

-11

-1

35

13

38

28

53

56

8

50

19

8

11

12

55

52

32

11

1

14

18

19

57

55

39

20

29

26

30

23

21

43

15

57

27

13

51

58

40

45

24

30

33

43

24

33

.299

.228

.224

.230

.167

.353

.277

.984

.356

.365

.174

.256

.253

.198

.395

.234

.108

.311

.117

.134

.259

• 173

.357

• ^ 74

.612

.024

.270

.030

.020

.004

.2 34

.014

.133

.209

.333

.337

.161

.419

.156

.175

.004

.474

.127

.61 1

.651

.706

.722

.730

.797

.608

.972

.758

.872

.689

.553

.490

.693

.875

.903

.450

.397

.744

.954

.269

.674

.716

• 3 76

.815

.875

.465

.615

.658

.554

.585

.653

.491

.545

.982

.92 3

.215

.833

.161

~.639

.665

.369

.420

43.15 *0.4

43.25 +0.7

43.14 -

43.07 -

1.0

1.3

42.40 -0.4

43.72 »l.l

43.30 +0.4

64.63 - 1.0

29.01 -0.6

26.03

49.31 -

45.71 -

30.71 -

37.55 -

0.2

2.6

2.9

0.2

1.8

17.07 U. 4

27.44 0.4

67.90 -0.3

39.51 +0.9

34.49 +0.1

55.28 - 1 .6

20.66 -0.6

37.10 -0.2

20.56

13.15

29.43

25.04

45.93 -

2.4

• 1. 3

• 1. 1

1.3

0.2

33.38 -0.1

15.11 • 1 . 4

17.03 -0.9

34.71 •0.5

33.85 -0.4

23.71 1.7

51.07 -0.9

26.18

68.98

36.63

19.87

3.2

-1.2

-2.0

1.1

15.58 -0.1

22.96

20.73

66.76

• 0.3

• 1.0

-0.7

100.6

104.0

104.8

102.4

101.1

100.6

103.0

114.6

91.8

103.1

112.0

95.7G

97.4

89.3

82.9

101. 8

115.5

106.2

90.6

109.1

89.3

99.0

8S. 1

78.5

103.2

99.0

94.6

107.2

90.5

95.2

104.9

100.9

91.1

108.9

109.5

117.2

107.9

93.4

93.9

99.2

90.8

115.6

100.6

104.0

103.9

101.7

101.1

100.6

103.0

114.4

91.8

103.1

109.3

94.5

96.5

89.3

82.7

100.5

105.9

90.6

108.3

89.2

87.4

78.3

99.7

9B. 1

94.6

104.6

90.5

95.2

104.9

100.9

90.8

108.1

108.0

116.5

107.9

92.8

93.9

99.2

89.5

115.6

102.1

104.0

104.3

103.7

102. 1

100.2

104.0

114.0

91.8

100.4

112.4

97.9

96.0

89.5

81.7

100.6

118.5

106.2

92.6

112.0

89.5

100.0

84.5

77.7

100.9

98.8

95.3

112.6

87.6

93.9

105.6

101.4

90.5

109.4

107.0

119.8

107.3

93.2

91.6

98.2

89.0

119.6

95.4

100.5

91.7

89.2

91.6

94.0

96.5

101.7

H9.6

79.3

85.5

85.0

84.7

87.0

80.6

89.8

104.1

95.5

84.4

91.9

87.2

91.5

81.5

69.9

88.9

92.5

89.3

86.3

84.2

72.9

84.8

89.7

86. 7

99.5

84.1

107.3

91.7

89.8

82.5

88.1

82.1

102.1

90.8

94.2

86.7

87.2

87.5

88.7

90.6

91.4

79.6

71.5

81.8

78.3

81.3

81.9

72.8

85.9

89.9

79.0

89.7

85.5

74.9

68.4

81 .8

86.3

85.3

78.3

80.5

61.4

81.6

85.3

83.5

85.0

78*0

82.7

103.6

87.7

88.0

73. 1

83.7

80.9

100.7

89.9

94.2

86.3

87.2

87.5

88.7

90.2

91.4

79.1

71.4

81.3

77.9

79.9

81.9

72.8

85.9

101.1

89.9

78.7

89.7

84.8

84.6

74.2

85 •]

68.3

81.4

85.4

84.9

78.3

80.1

61.4

81.6

85.3

83.4

92 • 4

85.0

76.ft

78.1

103.4

87.5

86.6

73.1

83.7

80.5

99.7
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 65

TABLE 1.1.—Basic physical data for 413 Super-Schmidt meteors: Trajectories.—Continued

9953

9-355

9974

9983

9985

9997

IC006

10012

10064

1CC70

1C094

1C098

1C106

10127

1C218

10222

1C240

10247

10252

10255

10273

10279

102P1

10342

10358

10365

10380

103e4

10394

10414

10439

10447

1C478

10480

10531

10555

10566

10583

10587

11816

11818

11825

11856

11862

6.4

6.5

13.0

1C.4

8.2

6.8

11.4

2.1

5.4

3.9

21.5

15.5G

15.8

3.0

4.5

13.9

16.C

4.3

7.5

t . 5

9.1

7.2

5.6

5.2

8.7

9.6

5.5

11. 4

4.5

26.5

8.4

11.2

3.5G

8.9

e.o

3.3

7. 1

26.6

e.o

23.3

8.3

8.2

e.7

14.4

7.0

6.6

10.3

5.2G

5.9

6.0

9.7

2.8

5.3

6.5

17.7

19.OG

16.5

3.4

5. 1

12.1

15.5

5.0

6.9

5.1

6.5

6.5

5.0

3.0

9.6

8.6

5.6

13.6

2.7

31.8

10.4

10.9

7.9

7.8

e.2

2.7

8.0

2C.1

7.5

15.1

4.2

1C.7

6.9

14.0

.42

.36

.62

• 5C

.45

.35

.50

.37

.58

1.46

.92

.71G

1.15

.29

.65

.47

1.04

.47

.37

• 9 1

.59

.97

.9C

.98

.B6

1.17

.34

1.34

1.29

3.84

1.04

.94

.61

1.22

.48

.60

1.30

l.CO

.67

2.16

2.19

1.C3

1 .32

.58

15

20

34

29

27

21

3C

21

32

78

56

36

59

18

35

27

62

27

0

4 3

36

53

4fl

57

42

6C

20

68

47

131

50

54

15

31

29

23

53

50

33

72

117

59

65

33

20

21

31

16

21

19

23

23 '

32

73 4

50 '

38

57

16 '

33

25

58

28

23

32

29

38

44

51

40

44

18

73

55

158

59

51

35

31

27

26

64

47

40

38

0

.6

.5

. 7

.6

.8

.2

.3

.5

. 7

.8

. 7

.2

.9

m 7

.9

.8

.0

1.8

7 . 4

.4

>.7

>.9

'.4

.8

? . 4

>.. 1

>.4

.!

>.8

>.9

• • 6

.2

J.C

).O

J.8

1.0

).2

.0

t.4

58 2.9

64 2.2

34 2.4

• 3

• 1

• 0.5

• 2

• 2

• 1

»1

• 2.5

-0.5

-0.5

• 2

• 1.5

• 2

• 1

• 3

• 4

• 2.5

• 0.5

• 1.5

• 2.5

• 1

• 3

• 1

• 1. 5

• 4

• 2

0

0

• 1. 5

• 3

• 2

0

• 2.5

0

• 3

0 -C

• 2 -<

0 -(

_c

• 1 -C

0

• 2

• 1

-I

— 1 — t

0 -C

• 6.5 -

• 3

• 2

• 2 -(

• 1

• 2

• I

• 1 •(

• 2 -(

-1 •(

• 2.5 -

• 2.5 -

• 2

• 2

• 3 —'

• 2 -(

• 2.5 -

• 2

-

• 1 -(

0

• 3

• 1

• 2 -(

• 2.5 -

0 •(

.5

.9

.0

.6

.9

.3

.1

.6

.4

.2

.0

.9

.8

.3

.4

.4

.3

.8

.8

).5

.1

).6

. 7

.4

.5

.3

# 3

.7

.5

.0

.6

m 7

.5

.8

.8

B 3

.6

.2

.5

.2

.3

-.733

-.142

-.095

-.50 3

-1.019

-.657

-.514

-.487

-.116

• -578

• .654

-.243

-.112

-.685

-.469

-.612

-.067

-1.044

-.672

-.732

-.638

-.584

-.574

• •040

-.870

• •602

-.058

-.176

-.191

-.708

-.126

-.477

• •849

• •048

• •105

-.261

• .339

-.421

-.521

-.202

0.0486

0. 1795

0.2014

0.0826

0.0740

0.0549

0.0228

0.2718

0.9330

0.6457

0.9814

0.3997

0.2970

0.2085

0.024S

0.1117

0.1233

0.1040

2.1242

0.1711

0.2169

0.2344

1.7497

0.1814

0.3377

0.0575

0.6101

0.9265

20.7255

0.4500

0.3525

1.0330

0.3667

0.1123

1.2390

7.8415

0.0678

0.5217

1.4327

6.5728

0.6521

0.6850

0.0420

.O07S3

.02780

.03120

.01280

.00371

.00850

.00353

.04210

.14450

.10000

.15200

.06190

.04600

.03230

.00380

.01730

.01910

.01610

.32900

.02650

.03360

.03630

.27100

.02810

.05230

.00890

.09450

.14350

3.21000

.06970

.05460

.16000

.05680

.01740

.19190

1.21450

.01050

.08080

.22190

1.01800

.10100

.10610

.00650

11.71

11.85

11.06

11.28

11.49

11.65

11.12

11.05

10.68

11.64

11.53

11.33

11.10

11.05

10.72

11.23

11.38

11.13

11.40

11.24

11.06

11.34

10.87

11.20

10.86

11.83

11.54

10.88

11.45

11.58

11.14

11.12

11.40

11.51

10.93

10.71

11.16

11.09

10.91

11.07

11.01

10.82

11.01

• .61

• •55

• .BO

• •35

• .39

• .16

-.04

-.04

-.32

• .12

-.15

-.04

• .61

• -17

• .63

• .29

• •04

• .18

• •07

•.22

• .27

• 1.22

• .37

• .26

• .49

• .37

-.23

-.04

-.10

-.04

-.20

• •12

• •71

• -08

• •16

-.05

• •25

• .40

• .93

-.17

• •10

• .48

• .09

0.5

0

1.5

1.5

0.5

0

0

00

0

OQ

1

3.5

10

2

1

0.5a

0

0

0

i

I

0

00

1

1.5

0.5

00

1

0

20

1.5

0

0.5

1. 7

00

0

1

3C

0.5

3.5

3U

ou

2

1.5

0

1

0

1

I

0.5

0.5

1

0

OU

0

0

0

3

0

0

1

0

0

0.5

0

2.5

0

0

0

C.5

0

0

0.5

0

0

0

0

0

0. 1

2

0

2

2.5

0

0

00

0

0

0

0
66

11973

12342

12361

12363

12399

12504

12577

12714

SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

1.1.—Basic physical data for US Super-Schmidt meteors: Trajectories.—Continued

VOL. 10

5 6.29583

5 31.35359

1.18112

1.18437

2.23660

5.26538

11.41127

29.26276

arent radiant sin Q

a 5

267 8 *25 13

242 16 -15 14

222 20 -35 39

103 20 +48 11

236 24 +35 30

115 20 *65 47

271 45 -12 30

276 58 -0 21

266 .779 44.93 -0

264 .587 23.04 +1

088 .349 22.62 •O

044 .252 18.93 +0

449 .992 20.07 +0

121 .284 19.32 -0

152 .606 29.65 -0

211 .806 25.92 •O

109.4

92.6

97.1

94.8

93.9

9H.2

101.5

100.0

108.1

92.6

97.1

94.2

93.9

98.2

101.5

100.0

"2.5 "ML

93.1

89.0

88.4

85.1

79.9

89.0

"ED

86.9 86.1

81.3 81.3

B6.0 86.0

84.0 83.6

78.0 78.0

82.5

82.8

83.6

82.5

82.8

83.4

11973

12342

12361

12363

12399

12504

12577

12714

13.2

S.5

18.2

12.6

5.2

29.2

11.7

6.1

14

8

16

9

5

26

11

8

0

7

6

6

6

6

9

2

1

2

2

1

.67

.85

.44

.34

.84

.95

.06

.81

38

50

80

90

47

169

60

47

34

43

74

120

48

172

62

47

3.3

2.2

2.7

2.3

2.9

3.9

S.2

• 1

+ 2

• 1.5

• 1.5

• 2

• 1

• 1

• 1.5

• 2

• 3

• 3

• 1

• 0.5

-I

-0

-I

-1

-2

-1

-0

.4

.4

.1

.0 •

.1

.3 •

.6

177

736

370

067

448

261

109

389

0.1498

0.3022

0.7942

3.B61O

0.9665

5.4170

0.6211

0.4907

.02320

.04680

.12300

.59800

.14970

.83900

.09620

.07600

-11.31

-11.29

-10.91

-11.06

-11.31

-10.97

-11.35

-10.86

-.01

• .73

-.01

-.06

• •19

• .06

• .20

-.28

0

3

3

0

0

3

1

2

Notes on Table 1.1

Meteor No.

3053 No v.t.* Estimated time error ±1

minute.

3072 No v.t. Estimated time error ±1.3

minutes.

3076 No v.t. Estimated time error ±20 s.

3288 No v.t. Common point and ratio of

velocities insensitive to time. Possible

error ±5 minutes. Heights could be

greatly in error.

3334 No v.t. Estimated time error ±0.9

minutes.

3355 No v.t. Time from equalization of

velocities.

3636 On Super-Schmidt film 28 segments in

the middle of the trail are lost in the

shutter hole.

3640 Four fragments became successively detached from the main body and can be

followed on the photographs for short

lengths of time.

3643 No v.t. Time computed from maximum-light segments.

*v.t.-vlsual time, I.e., time from visual observation.

Meteor No.

4141 Visual time given only to ±1 minute.

4181 No v.t. Time from good common

point.

4199 No v.t. Time from good common

point.

4388 Possible error of ± 1 minute in timing.

4394 Possible error of ± 1 minute in timing.

4464 A fragment became detached near the

end of the trajectory and remained

visible for Of 1.

4507 No v.t. No good common point.

Time error could amount to several

minutes.

4596 Trails intersect at 0?26 angle. Solution by direct triangulation, poor because of uncertainty in common point.

4701 No v.t. Time from one good common

point.

4952 No v.t. Time from two common

points; estimated error ±30 s.

5273 No v.t. Time from equalization of

velocities, rather uncertain.

5450 No v.t. Time from end flare, good.
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 67

Meteor No.

6093 Shutter flutter nearly masks deceleration on both films.

6398 A fragment became detached near the

end of the trajectory.

6961 Shutter breaks completely obliterated

by blending in the last one-third of the

trail.

7046 No v.t. Time from a common point,

could be somewhat in error.

7184 Trails intersect at 0?34 angle. Solution by direct triangulation.

7272 No v.t. Time from a good cotaimon

point.

7592 The last two-thirds of the trail appears

completely blended.

7637 Trails intersect at 0?5 angle. Solution by direct triangulation.

8089 No v.t. Time from a good common

point.

8168 Owing to shutter flutter and terminal

blending, no significant deceleration can

be derived for this meteor.

8224 Large shutter flutter makes even velocity somewhat uncertain; no decelerations were derived.

8254 No v.t. Time from one good common

point.

8294 The second hah* of the trail appears

completely blended.

8576 No v.t. Time from one common point,

rather uncertain.

8679 No v.t. Time from one fairly good

common point.

Meteor No.

8719 Only the end section of meteor trail was

photographed. Persistent train; the

meteor was reduced for the train program.

8943 Most of the trail is completely blended.

8951 Most of the trail is completely blended.

9172 A fragment became detached toward

the end of the trajectory and could be

followed for 0*3.

9284 Trails intersect at 0?14 angle. Solution by direct triangulation, using a

good common point.

9815 Persistent train; meteor reduced for the

train program.

10106 A fragment became detached in the

second part of the trajectory and could

be followed for 0*2.

10222 Large shutter flutter masks deceleration and makes even velocity uncertain.

10247 No v.t. Time from a good common

point.

10394 Large shutter flutter on both cameras.

10414 A fragment became detached in the

second hah* of the trajectory and could

be followed for 0*3. Another fragment

is doubtful.

11816 Meteor trail runs through shutter hole

on one film.

11818 A fragment became detached in the

second half of the trajectory and could

be followed for 0*3.

12504 A fragment became detached in the

second hah* of the trajectory and possibly subfragmented; it could be followed for 0*70.
68 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations

VOL. 10

Trai l So

2961

3000

102*

3037

1053

10 72

iC74

C 7 6

OSS

1217

1228

12 3*

12 50

U

86.45

85.89

85.92

86.38

88.61

80.61

101.02

101.34

108.03

106.44

109.45

89.14

79.80

74.73

89.30

80.83

75.36

92.13

92.09

94.C9

93.76

86.30

80.70

77.94

87.39

82.74

79.75

77.78

94.35

87.49

94.55

87.41

98.68

99.61

96.76

97.61

83.63

83.97

95.36

88.06

93.01

T

30.845

30.719

30.661

30.618

30.702

29.589

49.503

49.466

68.529

68.498

59.912

15.983

15.296

13.833

15.941

15.431

14.244

36.758

38.786

55.146

55.243

16.638

15.633

14.095

16.709

16.145

15.219

13.828

25.688

24.874

25.681

24.901

47.914

47.947

4C.612

40.528

28.478

28.554

29.075

28.080

28.885

v

-1.9C0

-2.077

-2.664

-1.675

-0.490

-12.790

-2.090

-1.570

-2.002

-1.557

-0.162

-0.267

-0.881

-7.800

-0.102

-0.873

-5.240

-1.436

-1.692

-1.140

-2.002

-0.623

-3.680

-9.160

-0.582

-2.100

-6.300

-9.320

-0.791

-4.910

-0.656

-5.090

-2.510

-1.150

-2.451

-1.706

-2.568

-2.674

-1.448

-6.330

-1.851

p.e.

.169

.129

.205

.069

.045

.710

.100

.150

.125

.226

.008

.024

.044

.28C

.026

.030

.140

.153

• 157

.044

.070

.041

.320

.640

.072

.260

1.C90

1.730

.050

.360

.037

.500

.380

.390

.140

.119

.134

.209

.083

.470

.C85

176CC

158CC

16000

17400

244 CC

0280C

00780

0081C

00146

00103

C0459

98000

3720C

C3000

98000

50300

C58CC

01440

01430

00760

00710

229C0

11000

03100

256CC

159CC

08300

02700

C344C

C078C

03500

0075C

C0398

00493

C0244

00278

0108C

C117C

01590

00327

0124C

• .02

• •12

• .12

• •04

-.2 8

• 1 .0 9

- . 11

-.1 6

-.0 1

• .2 6

• .05

-1.2 0

• .25

• 1.52

-1.20

• .02

• 1.22

-.53

-.52

-.14

-.11

-.49

+ .24

• .92

-.75

-.06

• .44

• 1.01

-.38

• •72

-.41

• .74

• .18

• .01

• .05

-.06

• .20

• .14

-.46

• .75

-.13

-11.07

-10.66

-11.53

-11.17

-11.07

-11.71

-11.31

-10.64

-11.21

-10.60

-10.79

-10.78

-10.70

-10.97

-11.26

-11.32

-11.1 2

-11.3 1

-11 . 10

-11.3 3

-11.2 8

-11.3 0

-11.3 1

-11.4 2

-11.2 7

-11.2 6

-11.2 7

-11.1 8

-11.28

-11.00

-10.73

-11.24

-11.16

-11.13

-11.14

-11.34

-11.24

-11.22

-B.28

-8.26

-8.14 ^

-8.33

-8.82

-7.68

-9.10 <

-9.22

-9.65 <

-9.81

-10.46

-8.31 <

-7.90

-7.23 <

-8.73

-7.87

-7.33

-8.96

-8.H9

-9.46

-9.2 3

-8.19 (

-7.47 <

-7.17 <

-8.21 i

-7.69

-7.26

-7.17 <

-8.74

-8.13

-8.82 <

-8.12

-9.09

-9.40

-9.03

-9.17

-8.49

-8.46

- 8 . 70 <

-8.2 5

-8.6 2

. 0 7

. 0 9

• 03

. 1 ?

. 4 3

. 0 8

. 2 8

.19 <

. 2 4

. 0 3

. 4 8

. 1 2

. 2 0

.12 <

. 2 8

-.10

. 0 6

. 2 8

. 2 1

. 6 2

. 4 1

. 0 1 <

. 2 9

.39 <

. 0 8

• •2 3

• •4 3

. 3 8

• •1 2

• •1 7

. 0 6

. 1 7

• .1 1

. 1 2

. 0 3

-.0 5

-.5 0

-.4 4

. 2 4

• .1 0

>.1 3

. 0 7

. 1 4

. 0 1

. 1 4

. 3 3

. 3 2

. 2 6

. 1 8

. 1 9

. 1 8

-.6 7

. 1 1

. 1 9

. 1 5

. 3 0

. 0 9

• •0 9

-.0 2

• •0 4

-.6 5

. 4 5

. 1 7

. 2 7

• •2 0

. 3 0

• •2 8

• -3 6

• .1 6

• .1 6

• •1 2

• •0 9

• •1 3

• •0 2

. 1 8

-.04

-.08

-.45

-.40

• •1 6

• •1 6

• •0 9

5 . 6

5 . 9

5 . 3

6 . 9

6 . 5

2 . 5

7 . 5

6 . 2

6 . 4

3 . 0

6 . 2

7 . 8

5 . 4

1 . 7

1 . 9

6 . 3

2 . 4

6 . 2

7 . 0

7 . 6

7 . 5

7 . 8

4 . 8

2 . 9

5.5

4 . 4

2 . 1

0 . 9

7 . 6

3 . 6

7 . 6

2 . 7

3 , 2

0 . 7

6 . 2

6 . 6

5 . 6

5 . 2

7 . 8

3 . 1

7 . 6
ATMOSPHERIC TRAJECTORIES OF 413 METEORS

TABUS 1.2.—Bane physical data for 413 Super-Schmidt meteor*: Acceleration*.—Continued

69

Trail No.

3265

1271

1277

3286

1288

3295

1299

3303

3307

1312

1327

1332

1334

1140

1142

• 144

H

100.06

95.IC

95.02

100.41

99.46

81.27

81.70

95.29

94.69

93.28

93.70

80.47

82.14

88.11

82.07

88.62

82.13

84.35

85.65

97.06

96.96

87.24

78.65

84.73

79.20

102.18

96.69

9S.87

81.62

79.28

76.71

74.72

81.84

79.23

76.4C

88.21

89.42

v

41.215

47.214

47.236

5C.449

50.120

20.755

21.060

32.005

31.986

28.718

28.730

17.164

17.310

19.007

17.684

19.071

17.691

15.852

16.002

35.709

35.719

24.265

23.513

24.098

23.376

53.381

62.738

62.609

19.459

19.344

14.000

U.740

14.471

14.344

18.934

18.603

18.729

V

-1.848

-1.226

-1.129

-3.270

-3.120

-0.196

-0.255

-1.442

-1.596

-2.310

-1.280

-2.650

-0.078

-1.076

-10.270

-1.001

-7.230

-2.623

-1.970

-2.160

-2.230

-1.188

-3.420

-1.668

-4.C90

-2.131

-1.C06

-1.715

-0.251

-0.602

-1.789

-45.696

-0.226

-0.605

-1.932

-2.430

-1.566

p.e.

.056

• C79

.054

.070

.320

.004

.007

.201

.184

.110

.130

.110

.080

.089

.880

.053

I.04C

.053

.080

.320

.270

.049

.300

.13 1

• C93

.117

.185

.010

.014

.054

3.290

.010

.022

.060

.540

.096

n

3 2

28

24

25

0

50

28

28

26

24

27

14

24

11

31

11

18

46

24

18

35

18

30

2 4

24

25

60

51

11

7

54

41

27

21

28

m

l

.00782

.01960

.01940

.00771

.C0661

.04550

.04820

.00742

.00680

.00992

.C1C82

.02330

.0307C

.C605C

.01690

.06320

.0174C

.04780

•0551C

.cone

.00328

.0391C

.C1090

.03010

.C0526

IcO542

.44960

.367IC

•2072C

.00840

.45620

.365CC

.1764C

.00810

.0I24C

6

-.10

-.2 0

• •19

-.2 0

-.0 5

-.1 5

-.2 1

-.2 5

-.1 5

-.0 5

-.1 4

• .04

-.2 0

• •70

-.2 4

• .68

-.0 5

-.1 9

-.0 8

-.0 5

-.5 2

• .57

-.1 6

-.1 8

-.5 3

-.4 0

-.7 3

- . 34

• .20

• 1.79

-.7 7

- . 14

• •11

• .24

-.0 1

log o

-11.IS

-11.10

-11.06

-11.4")

-11.11

-10.44

-10.57

-11.15

-11.16

-11.13

-10.98

-11.21

-11.2 2

-11.1 2

-11.1 1

-11.2 0

-11.1 7

-11.4 1

-11.15

-11.15

-11.22

-10.92

-11.18

-11.21

-11 . 16

-11.4?

-10.9?

-11.10

-10.99

-11.29

-10.96

-11.12

-10.91

-IO.H «

-10.81

-9.00

-4.16

-9.20

-8.91

-8.96

-9.12

-8.89

-8.86

-8.55

-8.79

-7.92

-8.26

-7.41

-8.29

-7.55

-?.?5

-7.86

-8.91

-8.92

-8.49

-8.14

-8.17

-9.22

-9.67

-9.44

-8.62

-8.27

-7.86

-6.81

-8.67

-8.27

-7.85

-8.18

l o g pobs

• .31

-.2 4

-.2 8

• •41

• .10

-1.1 1

-1.1 7

• .05

• .0 1

• •2 1

• .02

-.1 7

• .09

• .46

• .10

• •12

• •10

• •29

• .15

• .15

-.2 1

-.5 8

-.2 9

• •25

-.6 2

-.4 5

-.7 9

-.6 1

-.1 8

• .54

-.82

-.61

•". 14

A log Peor r

• •10

-.1 0

-.1 2

• .16

• •25

-t.l l

-.9 4

• •10

• .OH

• !o7

-.1 1

• .17

• •21

• .19

• •10

• •11

• •17

• .17

• .16

-.1 5

-.4 0

-.3 1

• .21

-.4 5

- . 1*

-.! »

-.4 0

-.4 1

-.2 6

-.4 1

-.4 0

-.49

••72

« . 14

P

7 . 5

7.0

5.6

7.a

•>. 1

7.7

7.9

4 . 0

5.4

6 . 1

5 . 1

6.9

0.0

6.1

1.1

7.2

7.4

7.8

1.7

4.4

«.8

1.7

6.2

7 . D

6.2

5.9

9.2

H.I

6.2

I.I

9.2

1 . 2
7 0 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

VOL. 10

Trail No.

1355

1360

1377

J3 79

3386

3393

3399

1405

3407

3411

3416

3424

3450

3463

3487

1497

1567

H

86.19

86.58

88.59

88.73

102.88

102.84

92.14

91.96

89.63

89.49

92.72

91.94

93.11

91.34

91.78

91.19

82.96

91.01

84.89

81.80

89.80

90.90

88.16

90.18

92.21

95.37

95.30

93.29

91.87

96.59

95.52

92.65

92.24

89.83

93.24

92.90

v

33.470

33.593

43.136

43.110

65.212

65.270

24.659

24.561

24.362

24.487

35.877

35.769

42.701

42.375

42.608

26.037

24.880

26.057

25.547

24.227

34.874

23.708

24.150

25.400

25.168

43.114

43.197

42.584

42.270

43.380

43.282

41.471

41.233

27.995

26.774

26.764

v

-9.890

-7.980

-18.200

-17.900

-1.320

-1.540

-2.030

-1.300

-2.127

-1.910

-2.022

-3.266

-3.160

-7.190

-6.810

-0.395

-8.020

-0.374

-3.320

-14.920

-2.840

-4.190

-1.430

•O.COO

-1.518

-0.599

-0.936

-2.340

-13.000

-0.662

-1.400

-4.940

-7.230

-1.750

-0.63 1

-0.919

p.e.

.420

.430

1.300

1.200

.110

.120

.180

.630

.186

.621

.119

.122

.420

.180

.410

• 02C

.340

.048

.270

1.700

.370

.460

1.800

.000

.112

.035

.056

.330

.450

.066

.169

.230

.440

.140

.032

.C44

n

20

16

14

13

23

21

28

17

27

18

24

25

18

25

15

40

16

28

13

9

16

20

9

8

26

29

25

17

14

26

23

21

17

2 3

18

34

m

l

.00460

.OO53C

.00410

.00440

.00353

.00352

.0152C

•C143C

.01320

.0128C

.00730

.00640

.00468

.00259

.00302

.458CC

.09900

.45300

•202CC

.C420C

.00500

.00844

•0067C

•C15C0

.03460

•0343C

.00860

.00490

.0113C

.01010

.00476

.00416

.00806

.C36CC

.03440

s

-.3 6

-.6 1

+ .24

+ .19

-.2 3

-.2 2

+ .01

+ .07

-.2 6

-.2 2

-.1 1

+ .01

-.2 1

+ .27

+ .17

-.8 6

• •63

-.8 3

+ .18

• 1.06

+ .43

-.0 6

+ .05

-.3 1

-.2 9

-.2 4

+ .25

-.4 8

-.3 1

-.1 7

-.0 6

+ .17

-.3 8

-.3 2

log a

-11.70

-11.60

-11.74

-11.74

-11.13

-11.20

-10.95

-10.74

-11.05

-10.98

-11.19

-11.32

-11.25

-11.51

-11.50

-11.07

-11.37

-11.03

-11.26

-11.29

-10.84

-11.24

-10.87

-11.00

-11.19

-11.24

-11.05

-11.24

-11.41

-11.53

-10.91

-10.90

-10.99

log pQbs A log

-8.16 +

-8.24

-8.13 •

-8.13 •

-9.66

-9.59

-8.4 1 •

-8.6 1 •

-8.40 +

-fl.46 •

-8. 8 5

-8.65 •

-8.87

-8.59 •

-8 . 60 •

-8.68

-7.55 •

-8 . 70

-7.86 •

-7.38 •

-8.73

-8.15 •

-8.56 •

-9.31

-9.12

-8.91

-8.24 •

-9.43

-9.12

-8.65 •

-8.49 •

-8.68

-8.87

-8.71 •

"obs

.03

.02

.26

.27

.14

.07

.27

.06

.08

.00

.12

.02

.11

.03

.05

.08

.39

. 1 1

.23

.47

. 2 4

. 4 3

. 1 3

.36

. I B

.13

. 4 2

.39

.16

.07

.20

. 1 9

.10

.03

A log Pcor r

+ .14

+ .15

+ .17

+ .20

-.1 2

-.0 5

+ .29

+ .05

+ .15

+ .07

-.1 2

-.0 4

-.0 7

-.0 9

-.0 3

+ .22

+ .22

+ .18

+ .21

+ .1 T

-.3 3

+ .48

+ .13

-.2 0

-.0 3

+ .06

+ .2S

-.1 6

-.0 3

+ .16

+ .25

-.26

+ .10

+ .20

P

8.3

B.I

5.4

5.6

6.3

6.3

5.6

0.0

6.4

0.8

6.8

7.0

3.9

5.9

5.7

8.4

4.4

5.6

5.0

2.0

3 . 1

5.1

0.0

0.0

5.5

7.4

7.3

4.0

6.0

6.1

4.9

7.7

6.6

5 . 1

7.6

8.2
ATMOSPHERIC TRAJECTORIES OF 413 METEORS

TABLE 1.2.—Basic physical data for 41S Super-Schmidt meteors: Accelerations.—Continued

71

Trail No.

1573

(60*

(610

1612

4629

1633

3636

36*0

36*3

3651

3655

3657

3663

H

90.60

90.66

98. *6

98.55

92.31

91.83

103.73

9*.*2

93.62

92.50

86.98

91.27

86.19

91.61

8*- 70

79.37

88.78

79.*7

81. 5C

7*.*3

71.06

68.08

79.2*

73.97

69.69

9*.l*

93.86

86.37

85.**

92.57

85.51

91.56

85.87

102.21

101.68

9*. 39

88.30

9*. 85

88.1*

v

36.710

36.783

30.903

30.836

*1.18*

*0.861

58.616

33.686

33.5*0

23.837

23.**2

23.706

23.297

23.301

22.76*

20.9*0

23.198

20.983

15.*8*

I*.937

l*.O59

U.*92

15.*02

I*.81*

13.135

26.818

26.836

25.095

25.052

26.532

25.900

26.*83

25.920

55.667

55.535

30.153

29.527

30.232

29.*19

v

-0.5*9

-0.632

-1.189

-1.0*5

-6.900

-7.1*0

-1.118

-2.092

-2.170

-0.721

-2.591

-0.813

-2.870

-0.523

-2.*08

-ll.** 0

-1.069

-9.120

-0.299

-1.823

-*.510

-8.256

-0.52*

-1.823

-8.650

-1.133

-l.*87

-0.385

-0.733

-0.837

-*.6l0

-1.197

-3.700

-2.6*0

-*.58O

-0.868

-5.180

-0.931

-5.190

p.e.

.039

.C35

.08*

.108

.170

.250

.067

.102

• 35C

.063

.075

• C52

.180

.012

.032

.220

.018

.520

.00*

.030

.17*

.139

.013

.0*5

.1*1

.105

.155

.023

.063

.032

.2*0

.056

.220

.100

.670

.020

.1*0

.062

.160

n

37

16

23

21

2*

20

2*

30

25

25

16

25

59

19

21

36

18

71

31

21

19

61

31

21

37

28

35

29

*5

21

*1

21

17

1 *

* l

22

30

22

•

•

•

•

•

•

* .

2 .

1 .

3.

2 .

*

•

•

m

l

0628C

06300

0256C

C259C

0050 7

00*61

00362

00562

00*7*

03*50

020CC

C319C

C1660

185CC

ll*CC

03050

16200

0319C

55000

37000

01CCC

11800

96000

11000

53CCC

01160

OHIO

C1970

01590

0*1 AC

01520

03950

01680

00279

00253

0306C

Cl*30

03170

01350

5

-.7 1

-.7 2

-.1 7

-.1 8

-.3 *

-.2 2

-.2 0

-.0 2

• •12

-.6 *

• •05

-.* B

• .19

-.7 1

-.0 3

• .80

-.* *

• •77

-.8 5

• .08

• •62

• 1.63

-.5 1

• .16

• •9 *

-.1 2

-.0 7

• .0 0

••1 7

-.5 6

• •* 0

-.* 6

• •3 *

-.2 7

-.1 6

-.3 9

• .30

-.* 5

• •3 *

log o

-10.9*

-11.00

-10.9*

-10.89

-11.65

-11.48

-11.I*

-11.25

-11.19

-11.17

-11.23

-11.OT

-11.01

-11.29

-11.*3

-11.53

-11.* *

-10.S6

-11.0*

-11.3*

- 11.00

-11.Cl

-11.01

-11.2 *

-11.0*

-11.13

-10.3*

-10.61

-11.28

-11.29

-11.36

-11.2*

-11.36

-11.5*

-11.33

-11.*8

-11.38

-U.* *

1 0 8 POb8 A

-9.12

-9.06

-8.77

-8.82

-e.*9

-B.*8

-9.63

-8.81

-8.8?

-8.71

-8.22

-8.67

-8.20

-8.59

-7.98

-7.*2

-8.30

-7.51

-8.02

-7.29

-6.97

-6.8*

-7.79

-7.30

-6.72

-8.78

-8.67

-9.11

-8.86

-8.72

-8.10

-8.57

-8.18

-9.25

-9.02

-8.86

-8.17

-8.82

-8.18

logp^ A to

-.56

-.50

• .* ?

• •3 7 <

• .2 1

• .1 8

-.0 5

• .0 6 <

-.0 2 <

• .00

• •0 * <

-.0 6

-.0 1

• .05

• .09 <

• .25

• .10

• .16

-.1 9

• •0 *

• •15

• .10

- . U

-.0 0

• •32

• .07

• .15

-.9 0

-.7 3

-.0 0

• .0 *

• .06

-.0 1

• .2 2

• •* !

• .0 1

• •20

• !t 7

corr

.32

.25

. * 0

. \b

. 23

.C3

.10

.05

.05

.04

.02

. 0 0

. 1 *

.12

. 1 9

.17

.05

.02

.0?

-.27

.06

.07

>.O8

. 1 *

• .20

-.9 0

.87

-.3 6

.01

.01

.06

. 2 7

• * 2

• .1 3

. 1 9

>.I 6

P

8.2

8.2

7.0

5.*

8.3

7.9

7 . 0

6.*

2.6

7.2

6.1

7.8

4.6

9.1

7.2

3.7

* . 6

3.*

» .*

6.7

* . *

1.5

8.7

6.*

3.2

6.0

5.1

6.*

5.1

8.9

*.R

8.6

5.0

8.1

3.8

8.*

5.8

7.7

5.6
7 2 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

Trai l No.

»784

(786

1813

1847

1861

1877

l P 86

-103

4125

4136

4138

4141

H

92.95

92.72

84.60

84.61

93.90

94.17

92.19

92.37

98.90

98.40

92.24

88.68

90.32

86.04

95.58

90.60

85.97

87.39

86.93

78.01

75.27

73.48

81.75

77.99

75.26

73.32

80.66

76.32

81.13

76.48

79.11

79. 2t

99. 19

98.80

104.52

105.44

81.31

77.62

80.10

v

37.349

37.290

21.103

21.073

22.597

22.611

58.480

58.690

52.165

52.149

25.683

25.470

28.622

27.840

28.930

28.608

27.799

18.703

18.649

16.583

16.158

15.389

16.738

16.600

It.17 7

15.046

18.317

17.624

18.348

17.631

18.217

18.206

53.427

53.061

68.527

68.566

16.741

15.783

16.603

v

-2.150

-3.84 0

-1.336

-1.545

-0.819

-0.676

-16.640

-26.410

-1.086

-1.014

-1.25 2

-2.048

-1.848

-4.385

-0.606

-1.497

-4.32 0

-1.69 0

-2.55 0

-1.01 0

-3.26 0

-15.790

-0.18 6

-0.856

-2.33 0

-17.730

-0.603

-7.51 0

-0.724

-5.85 0

-1.508

-1.45 0

-2.754

-1.900

-3.05 0

-2.89 0

-1.03 9

-7.78 0

-2.039

I

1

2

1

1

p.e.

.210

.170

.C3C

.C32

.023

.039

• C20

.400

• C44

.035

.C3C

• C59

.079

.182

.027

.043

.245

.320

.260

.130

.390

.240

.062

.110

.260

.320

.136

• 48C

.140

.440

.034

.042

.087

.230

.260

.340

.C83

.C80

.C37

n

18

17

39

39

66

63

10

11

30

28

46

35

24

20

41

31

19

26

24

20

14

9

27

19

15

10

18

11

20

13

29

33

21

?2

24

18

22

9

31

°1

.01280

.01170

.C534C

.05360

•0243C

•0265C

.00106

.oouc

.03230

.03140

•C221C

.01680

.0274C

.00970

.04200

.02S4C

.00940

.01280

•0115C

.63300

.292CC

.03400

.85000

.63100

•29CCC

.02500

.0434C

.0112C

•C4650

.01230

•0323C

•0335C

.00920

.0089C

.00183

.00207

.153CC

.04700

.12100

-

•

-

-

-

• 1

-1

• 1

•

-

-

•

c

.13

.05

.03

.02

. 10

.03

.13

.17

.39

.35

.25

.02

.01

.66

.54

.05

.68

. 14

.04

.37

.32

.40

.20

.37

.32

.52

. 31

.68

.40

.62

.01

.03

.41

.36

.04

. 17

.63

.48

.75

log o

-10.99

-11.2 0

-10.58

-10.64

-10.88

-10.8 5

-11.75

-11.97

-11.32

-11.24

-11.2 7

-11.20

-11.40

-11.2 8

-11.4 0

-11.34

-11.7 5

-10.9 7

-11.08

-11.07

-11.07

-11.17

-11.1 1

-11.0 0

-10.88

-11 . 12

-10.6 0

-11.1 1

-10.71

-10.97

-10.87

-10.86

-1 1.55

-11.35

-11.4?

-11.54

-11.04

-11.44

-10.94

log p A 1(

-8.77

-8.53

-8.28

-8.21

-8.66

-8.73

-8.64

-8.43

-9.23

-9.26

-8.60

-8.42

-8.50

-8.2 5

-8.93

-8.58

-8.26

-8.28

-8.11

-7.83

-7.41

-7.00

-8.53

-7.91

-7.56

-6.97

-8.53

-7.60

-8.44

-7.69

-9.17

- 8 . 18

-9.03

-9.19

-9.4 3

-9.44

-8.03

-7.28

-7.77

) g Pobs

-.0 2

+ .20

-.2 1

-.1 4

+ .1 7

+ .12

• •05

+ .2 7

-.0 1

-.0 8

+ .09

-.0 2

+ .03

-.0 7

+ .0 3

-.0 2

-.0 8

+ .01

+ .1 4

• 1 1 1 • 1 1 i

- . 77

-.1 5

-.6 4

-.2 3

-.5 ?

-.5 7

+ .2 1

+ .02

+ .21

• •26

-.22

+ .26

-.0 5

A log Pcor r

+ .05

+ .23

-.1 7

-.1 0

+ .2 0

+ .15

+ .05

+ .2 9

+ .06

-.0 2

+ .1 6

+ .0 3

+ .0B

+ .05

+ .0 7

+ .02

+ .04

+ .11

+ .71

-.0 9

-.0 8

-.1 5

-.1 7

-.7 3

-.1 7

-.6 0

-.4 7

-.4 3

-.5 2

-.5 1

-.4 9

+ .27

+ .0 2

+ .16

+ .24

+ .11

+ .10

+ .11

P

5.3

7.3

6.9

7.0

6.7

6.3

6.R

7.0

8.4

8.3

8 . 0

7 . 0

? . l

4 . 2

8 . 8

7 . 3

4 . 2

2 . 3

? • 0

5.0

3.4

1.0

1.0

5.0

4.0

1.4

1 .6

3.7

2.5

7.0

7.2

8.5

5.0

5.W

5.4

7.2

H.O
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 73

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

Trail No.

4143

4147

.151

.153

'•181

'•199

4216

4229

4289

M i l

O 1 J

H

81.04

77.86

79.92

92.98

91.41

81.66

74.94

71.82

81.99

75.96

72.43

75.89

78.41

78.48

103.24

90.66

85.48

90.90

85.46

89.47

89.14

95.55

93.81

87.99

94.33

92.57

88.CO

91.67

92.50

88.69

102.65

101.72

97.63

98.37

85.29

79.03

85.33

84.17

84.10

79.95

76.57

74.78

V

16.815

16.018

16.689

29.824

29.533

22.656

22.288

20.772

22.668

22.383

21.444

22.348

22.600

22.554

70.875

20.496

19.767

20.523

19.728

20.412

20.429

30.463

30.433

29.616

30.353

30.288

29.626

31.787

31.690

31.061

60.355

60.266

33.848

33.854

18.299

U.973

18.295

19.523

19.456

15.150

14.775

14.313

V

-1.133

-7.370

-2.124

-0.996

- 1 . 92 7

-0.108

-3.030

-19.460

-0.460

-1.870

-8.910

-1.190

-0.718

-0.638

-1.174

-0.447

-5.360

-0.521

-5.880

-0.801

-1.018

-0.241

-0.601

-7.310

-0.513

-0.896

-6.990

-2.936

-1.665

-5.860

-1.730

-1.670

-1.311

-0.980

-1.513

-5.330

-1.653

-3.773

-3.950

-0.569

-1.777

-2.830

p.e.

.187

1.500

.072

.C2C

.048

.030

.230

2.300

.036

.210

.510

.250

.104

.052

.260

.051

.420

.013

.016

.028

.CIO

.570

.0 38

.014

.580

.087

.044

.520

.120

.160

.C54

.065

.C34

.160

.073

.175

.220

.032

.152

.200

n

1 9

1 0

2 9

3 8

2 9

37

1 7

10

31

17

13

28

6 4

6 3

2a

22

15

32

15

3 7

4 7

35

4 6

11

2 9

4 0

11

2 7

34

16

2 5

2 1

4 0

3 8

38

21

15

?!

20

4 3

23

21

B

l

.14800

.05100

.11500

.C1006

.00766

.843CC

.29700

.05600

.85400

.384C0

.11900

.37700

.64000

.647CC

.00355

.125CC

.03370

.12200

.0334C

.109CC

.10500

.142CC

•1230C

.03220

.12800

.109CC

.0322C

.00563

.00635

.00255

.00230

.00198

.00940

.01050

.127CC

.02250

.12800

.C34CC

.03110

•122CC

•076CC

.03600

-.5 8

• .44

-.2 0

-.1 0

• .13

-1.06

• .32

• 1.19

-1.1 2

• .14

• .81

-.1 1

-.5 5

• •57

-.4 9

• .57

-.7 5

-.4 2

• .62

-.4 9

-.2 7

• .62

-.0 5

-.1 7

• •50

-.1 9

-.0 4

-.1 2

-.2 4

-.1 2

• .87

-.1 1

• .54

• .59

-.25

• .17

• .63

log a

-11.21

-11.40

-10.91

-11.10

-11.19

-11.30

-11.22

-11.25

-11.06

-11.2?

-11.28

-11.02

-11.18

-11.06

-11.21

-10.80

-11.03

-11.28

-11.00

-11.10

-11.26

-11.49

-11.29

-11.12

-11.31

-11.21

-11.16

-11.25

-11.11

-11.15

-11.17

-10.79

-10.82

-10.1i

-11.00

-10.90

1 0 8 pob.

-8.00

-7.10

-7.76

-8.95

-8.69

-9.01

-7.7?

-7.09

-8.40

-7.90

-7.15

-8.09

-8.25

-8.29

-9.78

-8.60

-7.68

-8.54

-7.64

-8.17

-8.27

-9.20

-8.82

-7.91

-8.88

-8.66

-7.91

-8.62

-8.84

-8.41

-9.53

-9.57

-8.95

-1.06

-7.97

-7.61

-7.94

-7.82

-7.81

-8.24

-7.79

-7.67

^ log pobe a

-.21

• .26

-.05

-.20

-.0 7

-1.1 9

-.1 6

• .07

-.5 4

-.4 7

-.1 5

-.6 7

-.6 5

-.6 9

-.2 1

-.0 4

• .46

• •04

• .49

• .09

• .16

-.24

-.0 0

• .43

-.0 2

• .06

• .41

• •02

-.1 1

-.0 1

-.0 1

-.1 4

• .17

•.1 2

• •15

• .01

• .I d

• •21

• .2?

-.5 1

-.1 2

-.1?

1 0 8 peorr

• .09

• .11

• .08

-.1 5

-.1 8

-.9 0

-.1 8

-.1 5

-.2 3

-.4 5

-.2 9

-.2 1

• .21

• .22

• .26

• .26

• •04

• .11

• .11

• •IS

• .11

• •09

• .08

-.0 6

-.0?

-.0 5

-.1 8

••1»

• .08

• .07

«.0«

• .10

• .??

• •??

-.4 4

-.1 1

-.44

P

1 . 6

1 . 5

7.8

7 . 5

6 . 5

1.0

4 . 6

1.5

7 . 7

4 . 5

3.2

0 . 0

0 . 0

0 . 0

6 . 0

5.3

4 . 6

6 . 1

4 . 1

0 . 0

0 . 0

5 . 5

a.5

1 . 5

7 . 0

8 . 1

1 . 5

7 . 1

7 . 7

1 . 9

7 . 0

s.a

7 . 5

7 . 2

8.2

1 . 4

S . l

4 . 7

4 . 1

1 .{

5 . 1

1 . 9
74 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

A log

79.86

76.51

7*.7*

85.84

81.67

85.31

81.83

106.85

107.25

92.37

86.99

8 4. 36

91.85

87.01

84.42

88.24

83.45

85.65

90.94

90.29

93.65

87.12

91.01

79.87

76.32

74.09

78.74

75.91

74.36

90.15

90.18

106.30

106.20

94.08

85.45

80.72

77.39

74.76

93.43

84.24

79.04

75.48

15.130

14.740

14.255

25.659

25.283

25.613

25.336

64.163

64.122

22.525

21.942

21.091

22.496

21.924

21.126

24.723

24.182

24.500

45.162

44.927

26.553

26.010

26.448

15.507

14.995

14.431

15.372

14.904

14.527

33.805

33.705

21.813

21.549

20.781

19.648

17.137

21.825

21.382

20.355

18.109

-0.667

-2.145

-3.009

-1.136

-2.790

-1.074

-3.210

-0.398

-0.115

-0.737

-3.400

-7.630

-1.021

-3.660

-6.920

-0.983

-3.250

-1.991

-5.260

-7.410

-0.890

-3.940

-1.504

-1.234

-1.722

-4.170

-1.350

-1.873

-3.727

-0.924

-0.879

-0.153

-1.119

-2.218

-6.128

-15.890

-0.209

-1.268

-3.763

-11.343

.036

.156

.128

.046

.140

.066

.160

.C35

.035

.038

.100

.290

.060

.230

.360

.079

.170

.071

.190

• 29C

.050

.250

.077

.042

.089

.155

.041

.109

.190

.071

.130

.012

.C40

.060

.121

.530

.013

.032

.068

.165

.122CC

.C74C0

.03490

.C438C

.02550

.04140

.0263C

.01540

.01690

•1580C

.08740

.04100

•153CC

•0879C

.04170

.0432C

.0145C

.03200

.00465

.00397

•01990

.0096C

.01630

.12400

.0636C

•C233C

.10400

.05690

•0271C

.00650

.00653

25

19

65

58

07

48

04

18

11

63

09

57

56

08

56

63

43

18

23

06

37

29

13

43

22

80

20

30

72

16

16

-11.02

-11.07

-10.93

-11.17

-11.21

-11.09

-11.28

-10.55

-10.02

-11.27

-11.37

-11.37

-11.37

-11.40

-11.35

-11.23

-11.06

-11.21

-11.61

-11.64

-11.24

-11.35

-11.25

-11.11

-11.01

-11.01

-11.04

-10.94

-11.00

-10.88

-10.86

-8.17

-7.71

-7.65

-8.55

-8.22

-8.58

-«.16

-9.95

-13.47

-8.43 •

-7.83 •

-7.56 +

-8.30 +

-7.80 +

-7.60 •

-H.5B

-8.20

-8.31

-8.70

-8.57

-8.80 •

-8.24 •

-8.59

-7.92

-7.85

-7.57

-7.90

-7.82

-7.60

-9.15

-9.17

47

25

30

38

38

46

31

14

64

27 •

43 •

49 +

36 •

46 •

45 •

??

22

16

12

04

01

03 •

00

22

40

27

28

40

28

63

65

38

26

43

37

44

46

36

27

73

41

46

45

49

49

41

16

18

11

01

05

.00

00

02

?8

42

24

.33

.41

.26

.53

.55

7.2

5.6

4.3

8.9

6.1

7.8

6.2

5.0

0.7

8.1

6.7

4.6

8.0

6.1

4.2

7.2

4.7

7.8

7.9

7.3

7.5

5.2

6.8

8.5

5.5

3.7

7.8

5.2

3.6

6.2

3.8

823CC

651C0

44400

24600

03150

81700

60900

34800

07890

-1

-

-

• 1

-1

-

+

.42

.51

.03

.39

.42

.34

.40

.16

.99

-11.44

-11.58

-11.50

-11.61

-11.23

-11.52

-11.59

-11.61

-11.31

-8.85

-8.01

-

-

-

-

-

-

—

r.74

r.33

r.io

i.72

.96

r.52 i

r.i6

-.01

• •1 2

• .0 3

• .2 0

• •2 5

• •0 7

• .0 8

• .1 2

• .2 4

• .1 4

• .21

• .08

• .2 2

• .2 0

• •21

• .15

• .16

• •2 2

7.9

8.7

7.2

5.4

1.9

8.8

8.5

6.4

3.0
ATMOSPHERIC TRAJECTORIES Of 413 METEORS 75

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

Trail No.

4472

4505

4507

4513

4534

4542

4574

4596

4618

4622

624

.645

• 657

H

95.46

94.17

90.12

95.36

94.19

90.45

94.81

94.43

92.67

92.23

89.35

89.46

97.24

91.52

87.53

97.76

91.74

87.77

92.43

91.46

95.22

95.13

88.44

87.29

91.39

87.27

91.73

88.82

109.79

110.24

88.88

84.78

88.24

85.30

101.09

100.69

94.69

87.29

84.64

95.68

89.07

v

23.404

23.357

22.831

23.447

23.383

22.910

25.254

25.218

28.812

28.774

18.902

18.882

31.705

31.424

30.879

31.722

31.492

30.961

23.639

23.538

28.418

28.351

21.719

22.010

20.394

19.661

20.368

20.328

67.813

67.781

18.353

17.809

18.301

17.893

58.699

58.795

23.589

22.915

22.127

23.606

23.176

v

-0.459

-0.814

-4.130

-0.642

-0.844

-3.C30

-1.885

-2.255

-1.925

-2.371

-0.836

-0.788

-0.332

-1.562

-5.410

-0.325

-1.527

-4.250

-1.490

-2.171

-1.292

-0.900

-1.579

-1.697

-0.96 3

-7.660

-0.757

-2.520

-1.053

-0.830

-0.951

-3.655

-1.530

-2.680

-1.574

-2.034

-0.379

-1.58 3

-4.031

-0.326

-1.020

p.e.

.024

.014

.14C

.C28

.019

.250

.C7 8

.11 1

.089

.113

.069

.114

.012

.044

.18C

.013

.036

.180

.049

.083

.C28

.130

.027

.C28

.030

.410

• C35

.340

.275

.230

.016

.173

.C33

.167

.113

.109

.009

.023

• C79

.015

.071

n

41

51

71

43

52

73

34

31

31

27

33

79

43

75

17

40

75

19

35

79

41

36

50

49

46

16

39

20

21

72

53

19

46

22

23

22

50

40

77

35

40

m

l

.043 70

.0387C

.CU5C

.04330

.03830

.0136C

.01180

.01120

.CC487

.00443

•131CC

.136CC

.19500

.138CC

.04900

.19800

.14200

•055CC

.02020

.01770

.00818

.00807

.C281C

.C2420

.01990

.C067?

.02070

.01290

.00112

.00128

.0764C

.02C8C

.06910

.02660

.00679

.00648

.1386C

.C5H3C

.01930

.14510

.08320

5

-.3 9

-.2?

• .64

-.3 8

-.2 7

».55

-.1 1

-.0 6

-.0 9

-.0 1

-.1 7

-.7 1

-1.07

-.7 6

• •5?

-1.0 9

-.7 9

• •46

-.4 1

-.7 3

-.0 7

-.0 3

-.1 2

• •0?

-.1 1

• .63

-.1 5

• .24

-.0 5

-.1 9

-.3 2

• .65

-.7 0

• .51

-.2 3

-.1 8

-.6 6

• .28

• •89

-.7 8

• .01

log o

-10.89

-11.00

-11.03

-11.03

-11.07

-10.95

-11.31

-11.14

-11.1?

-11.17

-11.12

-11.08

-11.32

-11.74

-11.73

-11.37

-11.77

-11.19

-11.70

-11.73

-11.11

-10.94

-11.30

-11.27

-11.18

-11.17

-10.9?

-11.05

-11.05

-11.04

-10.96

-10.88

-11.04

-10.85

-11.77

-11.34

-11.10

-11.2?

-11.21

-11.3 )

-11.24

^

e

 "obi

-8.86

-8.63

-8.08

-8.72

-8.61

-8.19

-8.50

-8.4 3

-8.74

-8.66

-8.26

-8.27

~».O5

-8.42

-8.01

-9.06

-8.43

-8.10

-8.47

-8.32

-8.82

-8.98

-8.3?

-8.32

-8.53

-7.76

-8.63

-8.16

-9.96

-10.04

-8.25

-7.83

-8.06

-7.93

-9.39

-9.29

-8.78

-6.76

-7.99

-8.84

-8.41

08

30

11

11 \

70

17 <

16

21

r.i

b.2

\.t

1 . 6

1.0

• .8

>.6

1.1
76 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

.659

".677

4679

4683

4701

47C2

4952

4962

4964

4966

.974

006

85.26

83.92

83.90

100.31

99.68

92.22

86.68

83.84

91.29

86.19

83.66

105.68

104.80

90.88

91.44

87.38

93.67

89.53

85.44

89.12

88.29

74.10

73.21

71.26

74.23

73.35

71.55

92.14

84.69

92.45

84.59

88.83

84.68

89.02

84.40

94.03

92.19

109.08

108.79

107.43

107.18

22.369

18.082

18.069

41.036

40.996

17.403

17.060

16.237

17.363

16.978

16.016

67.159

67.080

29.623

29.644

29.043

31.613

31.537

30.796

31.570

31.200

11.164

11.019

10.484

11.107

10.995

10.626

21.269

20.658

21.449

20.856

15.751

15.029

15.762

14.853

26.143

26.113

66.968

66.957

68.128

67.933

-3.130

-0.723

-0.688

-0.652

-0.572

-0.217

-1.021

-4.410

-0.288

-1.190

-5.930

-0.577

-0.344

-1.773

-1.499

-4.230

-0.117

-1.362

-13.290

-2.142

-5.C70

-1.283

-1.796

-3.210

-1.100

-1.370

-2.117

-0.839

-0.388

-0.910

-2.100

-0.950

-5.380

-0.627

-4.930

-0.965

-0.684

-0.618

-0.699

-1.330

-1.040

.066

.011

.011

.016

.020

.029

.061

.440

.018

.059

.360

.054

.145

.058

.029

.210

.027

.1 14

1.500

.154

-73C

.048

• 02a

.240

.C42

.022

.032

.107

.405

.079

.275

.062

.770

.045

.550

.042

.057

.018

.033

.190

.470

30

44

47

49

47

56

31

17

56

77

15

22

20

45

54

27

29

19

9

14

16

32

39

16

35

42

2C

?3

17

75

18

34

14

39

14

41

26

41

43

21

19

.02820

•121CC

.12100

.02220

.02 11C

.35800

.21400

•02CCC

.34400

.19100

.013CC

.00523

.00448

.C118C

.01260

.00588

•253CC

.17100

.06800

•161CC

•139CC

.18300

•157CC

.C694C

.18700

.17800

.07830

.11550

.03270

.1175C

•C324C

.10000

.02560

.C933C

.01850

•0165C

•C1280

.00540

.C052C

.00155

.00148

• • 70

-.53

-.5 2

-.23

- . 17

-1.05

-.09

• 1.27

-.8 7

• •02

• 1 .46

-.38

-.10

-.17

• .42

-. 75

-.11

• •51

-.07

• .05

-.45

-.24

• •41

-.49

-.41

• •34

-.69

• •53

-.72

• .53

-.49

• •61

-.39

• •79

-.74

• .01

-.06

-.01

-.04

• •01

-11.21

-11.00

-10.98

-11.24

-11 . 10

-11.14

-11.07

-11.13

-11.02

-10.81

-11.35

-11.37

-11.40

-10.40

-11.03

-11.61

-10.99

-10.89

-10.92

-10.93

-10.87

-10.76

-11.18

-11.25

-10.85

-10.98

-11.15

-10.84

-11.05

-11.06

-10.70

-11.20

-11.24

-11.03

-10.90

-8.05

-8.29

- 8. 31

-9.2 9

-9.36

-8.62

-8.01

-7.67

-8.50

-7.9 5

-7.60

-9.98

-8.6 7

-8.73

-8.3 7

-9.46

-8.45

-7.57

-8.26

-7.90

-7.56

-7.43

-7.25

-7.62

-7.53

-7.43

-a. 37

-a. 34

-8.14

-8.08

-7.49

-8.27

-7.56

-B. 77

-8.96

-9.95

-9.90

-9.81

-9.92

• •07

-.28

-.30

.04

-.08

• .07

>.22

• .34

• .11

• -74

• .39

-.24

-.09

-.10

-.08

-.65

• .02

• •56

• . 17

• .46

-.25

-.18

-.12

-.31

-.27

-.28

• .31

• .37

-.08

• .33

• .60

• •15

• .49

• .07

-.27

• •01

• •04

• .04

-.09

.08

. 31

.30

.02

. 11

.15

.13

.17

.19

.17

.15

-.04

.05

.05

.07

• .12

.06

.74

.41

. 17

. 11

. 10

.22

.19

.2ft

.03

.07

.05

.42

.41

.2?

• .28

• •21

-.23

.00

.00

• .01

. 14

4.1

8.8

8.8

7.9

7.7

4.8

6.7

1.6

8.4

6.3

1 .6

6.7

0.0

7.5

7.7

4.7

1.8

6.0

3.4

3.4

R.6

8.0

4.2

8.7

8.5

5.6

5.5

0.0

7.3

2.9

7.P

2.2

7.6

2.6

8.0

5.6

7.3

7.1

3.6

0.0
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 77

Trai l »3.

022

•C45

0 4 7

.063

.073

S079

,083

5101

5112

5124

5176

3180

5195

TABLE

H

94.51

85.70

80.02

94.25

85.44

80.53

94.56

93.41

83.13

83.04

113.36

112.65

93.89

83.39

78.33

94.55

83.32

78.37

111.22

110.51

107.15

106.34

107.23

107.11

103.36

102.53

95.37

86.70

82.05

95.70

87.25

94.51

85.78

81.56

96.23

87.04

82.38

86.06

86.96

95.97

88.63

1.2.—Basic physical data for 418 Super-Schmidt meteors: Ace

v

29.993

29.448

27.812

29.967

29.356

28.308

42.381

42.117

16.055

15.977

70.666

70.463

20.231

19.900

18.304

20.208

19.841

18.395

67.928

67.746

67.254

67.083

67.305

67.436

67.303

67.255

27.533

26.848

25.635

27.529

26.925

30.352

29.634

28.210

30.277

29.875

28.731

31.804

31.832

28.694

27.700

-0.661

-3.544

-15.060

-0.852

-2.906

-10.460

-1.786

-3.759

-1.656

-1.610

-0.810

-0.472

-0.193

-0.775

-12.630

-0.123

-1.300

-11.630

-1.821

-0.860

-1.105

-2.328

-0.727

-0.796

-2.240

-4.170

-0.713

-2.021

-6.620

-0.697

-1.788

-0.647

-4.350

-14.500

-0.435

-2.970

-5.320

-0.788

-0.497

-0.780

-5.340

p.e.

• C78

.174

.800

.092

.192

.840

.045

.139

.038

.044

.045

.081

.Cl l

.070

.470

.013

.C63

.540

.646

.180

.060

.C71

.776

.252

.200

.14 0

• C4C

• C79

.340

.02 8

.C61

.05 7

.310

2.IOC

• 107

.18 0

2.780

.067

.074

.C53

.580

»

27

15

11

77

15

9

74

71

37

3?

78

32

59

29

16

63

30

13

17

23

26

25

20

20

22

24

45

25

15

44

22

31

13

8

79

15

9

25

30

3?

13

" l

.111X0

.05700

•ooeic

.1160C

.05600

.01310

•C174C

.01180

•0775C

.0698C

.00169

.0015C

.72900

.32900

•0273C

.7350C

.32400

.02780

.C0369

.00330

•0095C

.00790

.00173

.0017C

.00980

.00930

•C990C

.04680

.01310

.100CC

.05100

.09200

.04C9C

.00340

.09720

.05220

.C073C

.02950

.03120

.C3040

.00750

E

-.8 3

••1 4

• 1.20

-.7 9

•.1 5

• .9 9

-.4 ?

• .0 1

-.2 7

-.2 1

-.1 1

• .0 0

•

1.37

•.1 2

. 4 3

.47

1.42

-.2 1

-.1 1

• .0 8

• .2 1

• •35

• •35

-.4 5

-.3 6

-.6 9

• •19

• .9 1

-.6 9

• .1 1

-.6 7

• •24

• 1.49

-.8 3

• .0 5

• 1.14

-.4 9

-.6 0

-.3 4

• .6 9

log o

-11.3 2

-11.4 4

-11.3 1

-11.4 4

-11.3 5

-It.2 4

-11.08

-11.12

-10.70

-10.53

-11.24

-10.95

-11.37

-11.14

-11.25

-11.02

-11.11

-11.33

-10.9?

-10.S7

-11.12

-10.71

-10.75

-11.59

-11.80

-11.54

-11.36

-11.15

-11.4?

-11.35

-11.33

-11.37

-11.2H

-11.31

-11.37

-10.89

-11.15

-11.06

-11.14

-11.3?

derations.-

1 0 6 pobs A

-8.78

-8.13

-7.74

-8.67

-8.22

-7.84

-8.92

-8.71

-7.90

-7.92

-19.04

-10.29

-8.70

-8.20

-7.28

-8.90

-7.9 7

-7.U

-9.55

-9.S9

-9.6?

-9.32

-10.05

-10.01

-9.31

-9.04

-8.69

-8.33

-7.96

-8.70

-8.37

-8.83

-8.10

-7.89

-8.99

-8.24

-8.23

-8.95

-9.14

-8.86

-8.20

-Cont

1 0 8 Pob,

• •10

• .0?

-.0 3

-.0 9

-.0 9

-.0 4

• .08

• •05

• .0?

• •19

-.1 0

• .1 3

-.2 3

• •3 1

-.0 2

-.0 1

• •28

• .55

• .16

• .21

• •45

-.2 2

-.1 9

• •24

• .4S

• .76

-.1 0

-.0 9

• .7 7

-.0 9

• .0 5

• .0 6

-.0 6

• •0?

• .0?

-.3 4

-.7 7

-.8 8

• .1 3

• .1 9

0 9

17

14

0 ?

0 8

16

0 2

15

11

7 0

15

15

74

7 8

0 0

0 1

2 5

6 3

I d

5 . 8

7 . 2

4 . 5

5 . d

2 . 4

8 . 5

7 . 0

8 . 1

1.1

b.n

2 . 8

8 . 0

5 . 1

1 . 9

6 . 9

6 . 5

1 . 9

0 . 8

2 . 3

4 3

4 0

2 6

4 5

0 4

0 4

19

0 6

0 6

0 8

11

07

0 6

0 7

76

\1

4 4

1 1

/^

0 . 6

0 . 6

6 . 9

8 . 3

8 . 2

6 . 3

3 . 0

9 . 1

6 . 6

7 . 3

5 . 4

0 . 9

1 . 9

6 . 2

0 . 0

7 . 0

4 . 5

7 . 5

7 . 9

225-636 O-67—6
78 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 41S Super-Schmidt meteors: Accelerations.—Continued

Trai l No. H v v p.e . n m1 s lo g a log p ofe s A log p Q b s A log

231

237

•257

• 27 3

•289

332

1346

5370

5*50

5*72

5511

96.52

88.73

107.68

108.05

95.3*

93.46

86.71

94.53

92.85

86.81

92.34

89.82

81.11

92.03

109.37

108.84

104.62

104.32

87.03

85.07

86.68

84.87

80.46

95.53

92.91

86.97

95.01

92.75

87.56

71.34

71.28

106.CO

103.79

96.39

97.25

95.49

90.38

85.04

95.81

90.09

84.08

28.722

27.678

67.727

67.841

28.493

28.431

27.307

28.513

28.446

27.517

32.807

32.751

31.596

32.832

62.973

62.896

63.242

63.272

22.799

22.635

22.737

22.574

21.696

28.629

28.510

27.744

28.591

28.491

27.840

15.291

15.287

71.820

71.548

46.607

46.620

30.876

30.643

29.986

30.934

3C.614

29.723

-0.728

-4.750

-0.535

-0.554

-0.597

-1.077

-6.860

-0.717

-1.228

-10.990

-0.458

-0.954

-11.810

-0.345

-2.628

-2.330

-1.990

-2.550

-1.096

-1.773

-1.320

-1.966

-5.690

-0.819

-1.325

-6.200

-0.798

-1.401

-5.620

-1.616

-1.724

-0.178

-0.408

-1.115

-1.232

-0.576

-1.632

-4.489

-0.767

-1.703

-7.800

.C57

.540

.043

.053

.059

.027

1.C2C

.059

.026

1.150

.034

.013

1.140

.025

.458

.281

.190

.330

.044

.026

.048

.C20

.170

.053

.022

.320

.046

.029

.320

.050

.032

• C16

.039

.139

.104

.016

.036

.C85

.038

.078

.28C

16

31

27

17

46

9

33

42

9

33

43

10

41

15

20

21

19

36

49

32

44

20

36

49

18

35

44

18

37

37

35

32

26

26

44

30

23

39

28

17

•C328C

.00780

.00403

.00421

.02190

.0189C

.00324

.02070

.01770

•0035C

.13500

.12200

•0245C

.13400

.00375

.00326

.00156

.00148

.03960

.03250

.03840

.C317C

.00980

.0242C

.C206C

.00654

.02360

.02CJC

.C0838

.04900

.0483C

.C3640

.03300

.C195C

.02100

.05750

.04C5C

.C1850

.05750

•0395C

.C145C

-.42

• •68

-.17

-.11

-.42

-.23

• .91

-.34

-.16

+ .88

-.67

-.45

+ .76

-.67

-.11

+ .01

+ .01

+ .07

-.39

-.15

-.35

-.12

+ .67

-.64

-.35

+ .55

-••>9

-.33

+ .40

-.01

+ .oo

-.64

-.45

-.40

-.53

-.57

-.09

+ .47

-.57

-.07

+ .61

-11.16

-11.29

-10.96

-11.00

-11.05

-11.16

-11.12

-11.07

-11.17

-11.36

-11.12

-11.28

-11.31

-10.97

-11.42

-11.29

-11.34

-11.42

-11.22

-11.26

-11.27

-11.28

-11.31

-11.32

-11.34

-11.23

-11.28

-11.35

-11.26

-10.92

-10.9b

-10. 71

-10.95

-11.19

-11.31

-11.25

-11.38

-11.42

-11.37

-11.39

-11.58

-f1.88

-8.24

-10.06

-10.04

-9.02

-8.78

-8.20

-8.95

-8.73 <

-7.99 ^

-8.99

-8.69

-'

-

c

_<

-'

_<;

r.79

(.12

(.32 -i

>.39

.57 <

).47 <

-8.47

-8.29

-8.39

-8.24

-7.92

-8.87 <

-8.68

-8.15

-8.88

-8.65 <

-8.16

-7.93

-7.90

-10.27

-9.92

-9.19

-9.14

-8.96

-8.55

-8.21

-8.84

-8.54

-8.00

• .16

• .16

-.20

-.15

-.08

• •01

• •04

.07

.01

• •25

.29

-.20

• •01

.45

.66

• .55

• •08

.15

-.21

-.19

-.16

-.15

-.17

.09

>.O7

• .11

.04

• 08

• •14

-.80

-.77

-.52

-.33

-.16

-.05

-.00

-.01

-.11

• .14

-.03

».O2

• -21

• .20

-.18

-.15

.06

.00

-.17

-.06

.01

• .05

-.07

.03

.14

-.22

• .69

• .50

• .0?

• .06

-.20

-.18

-.14

-.14

-.17

• .17

• .13

• •13

• .12

• •15

• •17

-.84

-.82

-.34

-.22

-.15

-.01

-.11

-.07

-.11

• .03

-.08

• .04

6.8

2.9

6.2

5.3

6.0

7.9

1.7

6.6

7.7

2.4

7.3

8.6

2.7

7.3

3.0

4.2

5.6

4.1

8.4

7.7

8.)

7.5

4.2

8.1

8.3

4.2

8.0

8.3

4.8

7.1

7.1

7.2

6.0

5.1

7.0

8.9

7.4

5.0

8.0

7.3

4.4
ATMOSPHERIC TRAJECTORIES OF 413 METEORS

TABUS 1.2.—Basic physical data for US Super-Schmidt meteors: Accelerations.—Continued

79

Trai l No.

5551

5557

5572

• 601

.605

J64 0

• 644

• 648

• 688

•>759

6062

6093

6095

H

106.36

106.14

91.33

83.86

80.94

89.84

84.65

81.14

87.35

82.75

79.88

87.27

82.86

79.80

94.70

94.10

91.29

81.72

77.82

90.66

81.85

77.36

94.52

94.54

91.43

91.86

93.20

93.00

99.18

81.53

99.80

83.03

96.39

9S.61

82.34

82.25

105.21

105.22

88.69

88.22

v

60.652

60.615

22.563

27.039

71.067

77.534

22.160

71.140

It.857

16.410

15.667

16.863

U.425

15.700

36.554

36.540

36.112

35.683

34.964

36.177

35.735

34.876

36.849

36.869

35.509

35.473

36.062

36.024

68.612

66.483

68.647

67.021

36.277

36.120

15.066

15.005

43.438

43.510

29.510

29.467

v

-1.569

-1.245

-0.428

-2.867

-9.679

-0.625

-2.596

-8.377

-0.840

-1.860

-5.165

-0.825

-2.008

-4.630

-0.544

-0.982

-0.285

-2.560

-7.050

-0.305

-2.624

-9.570

-2.690

-4.200

-0.668

-0.668

-0.814

-0.839

-0.136

-18.820

-0.130

-12.280

-0.992

-1.470

-1.884

-2.263

-0.296

-0.428

-1.283

-1.42 6

p.e.

.192

.436

.018

.174

.190

.027

.077

.228

• C39

.149

.263

.054

.140

.217

.058

.080

.009

.110

.210

.014

.091

.410

.300

.360

• C23

.044

.037

.C42

.005

.590

.C05

.740

.074

.136

.047

.058

.102

.098

.027

.041

n

21

20

5?

21

17

42

25

17

43

76

71

47

19

34

31

50

71

17

51

73

16

70

ID

33

1?

42

38

55

13

52

13

•>7

33

34

33

29

27

40

39

m

l

.00117

.00117

.25100

.12860

.C51CC

.73600

.14800

•0567C

-C9310

.05380

.0193C

•C973C

.05490

.01810

.00948

.00840

•446CC

.193CC

.067 30

.43500

•197CC

.0518C

.00334

.00335

.01700

.01780

•C341C

.03350

.74CCC

.C950C

.74400

.18600

.CC58C

.00494

.0605C

.05870

.00306

.00108

.02690

.07170

s

-.06

-.e ?

-.8 8

• .08

• .66

-.6 1

-.0 4

• .61

-.5 6

• .08

• .71

-.5 4

• .07

• .75

-.7 1

-.0 9

-.8 4

• •72

• .86

-.7 6

• •70

• .95

• .00

• .00

-.7 3

-.2 9

-.4 3

-.4 0

-1.2 0

• .86

-1.2 0

• •50

-.1 7

-.0 2

-.1 7

-.1 4

• .12

• -12

-.0 2

• •09

log a

-11.71

-11.09

-11.19

-11.79

-11.19

-11.71

-11.17

-11.39

-11.11

-11.08

-11.05

-11.20

-11.11

-10.86

-10.71

-10.85

-11.07

-11.34

-11.27

-11.08

- 11. 16

-11.46

-11.25

-11.45

-10.97

-10.99

-11.06

-11 . 04

-11.19

-11.87

-11.24

-11.90

-11.17

-11.24

-11.09

-11.15

-10.36

-10.5?

-10.87

-10.9?

1 O g Pob6

-9.68

-9.78

-8.61

-7.86

-7.4?

-8.45

-f .88

-7.47

-8.20

-7.91

-7.58

-8.21

-7.B8

-7.64

-9.39

-9.16

-9.10

-8.27

-7.97

-9.08

-8.75

-7.86

-«.86

-8.67

-9.70

-9.19

-9.02

-9.01

-9.91

-8.04

-9.93

-8.14

-9.20

-9.05

-7.82

-7.74

-9.97

-9.81

-8.69

-8.66

& leg bs

• .09

-.02

• •0 1

• •1 6

• •0 4

. 1 1

. 0 9

. 0 1

. 1 ?

• .0 7

• .0 5

. 0 6

- •

; •:

>0

12

• 1

52

to

14

• .02

•.21

-.58

-.51

-.75

-.76

-.67

-.71

-.64

-.70

-.17

-.09

• •07

• .14

-.1?

10

A log P cor r

• .07

-.0 7

•.1 5

• •on

• •17

• .11

• .IS

• .14

• .07

-.0 1

• .11

• •05

•.0 1

• •04

-.4 3

-.7 6

-.3 7

-.4 0

-.4 1

-.4 1

-.1 6

-.1 6

• •07

• .76

-.3 8

-.3 0

-.7 3

-.24

-.4 4

-.4 6

-.4 1

-.1 6

-.0 5

-.0 1

• •26

• .31

-.4 6

-.1 0

-.7 4

-.2 6

P

4.4

0.7

9.4

6.1

4.2

9.0

7.2

4.4

8.4

5.4

1.6

6.1

1.9

5.5

5.9

6.1

3.5

9.7

6.2

1.7

4.9

5.7

7ll

8.5

7.6

9.7

1.5

9.7

4.4

6.7

5.7

7.7

7.6

0 . 7

7.7

6.7
80 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

log o log p , A log p A log

6275

6329

6429

->433

5437

.491

.802

.811

92.61

92.83

10S.41

106.26

89.90

90.13

95.29

95.58

91.98

77.33

71.94

90.80

76.83

71.08

85.49

85.94

84.57

79.93

77.02

85.26

80.27

77.03

99.63

99.57

84.00

83.93

104.33

103.86

96.33

95.86

74.66

72.6$

69.43

74.40

43.103

43.171

72.773

72.696

22.390

22.355

31.509

31.533

27.299

26.319

24.008

27.285

26.177

23.159

35.230

35.258

22.506

22.066

21.511

22.455

22.095

21.476

64.268

64.250

16.931

16.838

54.723

54.670

60.922

60.338

12.389

12.169

11.464

12.376

-4.810

-4.840

-0.586

-0.727

-2.295

-1.836

-0.755

-0.755

-0.240

-5.902

-18.260

-0.408

-6.370

-22.390

-1.983

-1.719

-1.00 5

-3.270

-4.420

-0.668

-2.560

-5.780

-1.590

-2.520

-5.400

-4.550

-1.560

-1.360

-6.530

-10.790

-0.790

-1.377

-2.755

-1.035

.C80

.C80

.104

.C87

.C50

.083

.036

.C29

.010

.C98

.260

.020

• !50

.740

.046

.058

• C84

.170

.480

.108

.2 30

.3 50

• 22C

.190

• 25C

.29C

.21 0

.52 0

.7 30

.890

.036

.015

.203

.049

•C0324

.00337

.C0402

.00426

.C1770

-0183C

.03465

.03634

1.357CC

.729CC

.16500

1.32600

.682CC

•C91CC

.0101 0

.0112C

• •2?

• . 19

-.4 6

-.5 6

-.1 5

-.1 8

-.1 7

-.2 3

-1.09

• .0 1

• •90

-.9 7

• •06

• 1 .18

-.1 3

-.2 5

-11.75

-11 . 75

-11.07

-11.30

-11.28

-11.20

-11.02

-11.06

-11.13

-11.69

-11.43

-11.30

-11.68

-11.53

-11.12

•11.23

-8.75

-8.74

-10.09

-9.98

-8.2 5

-8.34

-8.94

-8.9 3

-8.78

-7.45

-7.09

-8.55

-7.42

-7.06

-8.79

-8.84

-.03

-.00

-.39

-.22

».25

• .1 8

• .0 3

-.11

• .07

• .08

• .02

• .07

• •06

-.6 5

-.6 7

07960

04500

0217C

0839C

C4800

02170

00267

00265

0442C

C441C

00130

0012C

00098

00088

11010

0814C

04480

10690

-.43

• . 16

• .61

-.52

• •11

• •61

-.23

-.22

-.03

-.03

-.06

• .02

-.06

• •03

-.35

-.02

+ .41

-.31

-11.14

-11.28

-11.27

-11.00

-11.17

-11.39

-11.31

-11.SI

-10.85

-10.72

-11.24

-11. 16

-11.84

-12.09

-10.90

-11.06

-11.13

-10.99

-8.40

-7.95

-7.91

-8.57

-8.0 5

-7.79

-9.60

-9.40

-7.51

-7.58

-9.5 7

-9.65

-9.09

-8.88

-7.94

-7.72

-7.46

-7.82

1 1 1 l 1 1

-.32

-.13

• .51

• .41

• .05

-.06

-.07

• . 10

-.60

-.51

-.44

-.49

01

04

27

06

26

34

28

04

09

08

02

03

04

01

07

54

50

6. 1

6.3

3.4

5.3

7.3

7.7

7.8

7.7

7.9

9.6

7.0

3.3

8.6

6.8

2.5

7.6

8.0

6.8

5.a

3.1

3.5

5.3

4.0

4.0

6.3

7.2

6 . 5

4.4

0.7

5.1

5.6

8.3

7.?

5.3

8.2
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 81

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

o961

t>971

•)992

998

•CC2

C22

72.49

69.37

104.14

105.21

87.47

87.54

93.56

93.50

91.1C

88.40

83.50

79.76

91.68

88.63

84.00

79.92

12.146

11.448

59.672

59.688

20.184

20.200

31.604

31.622

26.987

26.936

26.675

26.025

27.012

26.950

26.691

26.024

82.20

82.18

91.53

90.05

85.98

92.36

90.86

87.06

97.32

97.31

83.31

83.16

95.31

93.99

90.38

95.78

94.45

90.52

21.195

21.201

24.375

24.247

23.520

24.470

24.358

23.792

29.779

29.798

31.031

30.802

27.064

26.962

26.350

26.384

1.425

2.834

1.682

1.413

1.520

1.870

1.528

1.366

0.285

0.586

1.726

6.352

0.288

0.590

1.671

5.405

.C16

.111

.239

.112

• 15C

.130

.C68

.044

• COS

.C04

.C59

.10 2

.C09

-C03

.03 9

• I'll

.0013C

•C017C

.01110

•0113C

.01480

.01460

.1429C

.12990

.07920

•0318C

.1452C

.13120

.08570

.0337C

log o

11.07

11.42

1 1.42

10.(16

10.95

11.06

11.00

11.15

11.26

11.16

11.35

11.18

11.29

11.19

11. 32

1°6 P h

-7.71

-9.61

-9.66

-8.41

-8.32

-8.75

-8.81

-9.02

-8.72

-8.31

-7.86

-9.01

-8.71

-8.32

-7.92

g Pobs A log pe()rr P

-.51 -.46 7.1

102.24

100.13

101.62

99.71

94.86

91.97

92.04

48.649

48.539

48.518

48.430

47.804

20.027

19.998

- 1 .

- I .

- 0 .

- 1 .

- 6 .

- 0 .

- 0 .

1 0 0

6 3 3

8 9 7

6 1 7

2 5 4

4 5 8

3 6 8

.C76

.037

• C32

.021

.240

.cn

• C12

33

4 3

" 3

4 2

19

50

6 8

.01450

.01220

•0139C

.01160

.00420

.29600

.29800

-.5 1

-.2 4

-.4 2

-.1 9

• •56

-.7 9

-.8 1

-11.49

-11.49

-11.34

-11.45

-11.53

-11.34

-11.27

-9.28

-9.13

- 9 . 37

-9.14

-8.69

-8.45

-8.54

>. 19

. 1 8

>.O6

. 14

. 7 1

>.22

. 1 1

2.887

1.692

1.344

1.974

4.885

1.294

1 .799

4.981

1.416

1.338

4. 365

1.689

.381

.348

.058

.042

.384

.042

.032

.259

.C42

.034

.157

.179

-1.082

-1.649

-4.116

.C5P

.C38

.536

•01CIC

•CICOC

.01290

.0U2C

.00530

.01370

.01220

•0069C

.01270

.01270

.C0450

.00430

•C174C

.01360

.00470

-11.10

-10.87

-11.32

-11.36

-11.42

-11.36

-11.40

-11.40

-11.26

-11.23

-11.30

-10.86

-11.02

-11.11

-11.13

-8.19

-8.42

-8.61

-8.45

-8.14

-8.62

-8.49

-8.11

-B. 76

-8.78

-8.75

-8.60

-8.34

-.1 6

-.0 1

-.1 3

-.0 4

• .0 1

-.0 3

-.3 0

-.2 5

-.3 0

-.7 1

-.2 3

-.2 2

-.2 7

-.2 5

• -18

• . 15

• .14

• .04

•-1 1

• .1 »

1.07

1 .011

-.3 0

-.5 3

- . 0 1

• .02

-.0 3

• .OS

• .OS

• .13

•.7H

• .7h

-.4 6

-.8 9

••1 2

• .1H

• . 7 0

• . \h

• .(19

3 . 7

5 . 7

5 . 1

6 . 1.

7 . 5

7 . S

9.J

e.'<

6 . V

4 . 4

9 . 4

«.- *

7 . 7

* • *

7 . *

8.0

3 . B

8 . S

7 . 8

4.f ,

9 . 3

9 . i

4 . 6

7 . 1

R. (

7 . 0

4 . 1

H.b

H . I

S . I

7.' .

7. S

h . '

4 . 7

7 . 7

7 . 0

2.4

H. 1

1 . 1
8 2 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

VOL. 10

Trail No.

7026

'040

7044

7046

7052

7067

7069

7C73

7075

7C97

.'158

/161

'169

H

92.40

91.75

84.ol

84.64

100.39

100.82

88.89

89.55

104.98

104.46

81.56

82.05

86.04

85.87

91.06

82.10

81.45

79.01

81.75

96.31

90.11

95.20

96.33

89.67

94.99

84.86

84.78

105.25

102.74

101.57

96.64

105.78

102.31

100.90

94.79

83.86

82.44

83.81

82.33

v

39.428

39.589

21.517

21.498

44.869

44.858

18.522

18.541

54.075

53.967

18.444

18.459

27.550

27.509

34.119

17.896

17.838

17.071

17.839

32.587

32.074

32.558

32.660

31.911

32.613

22.942

22.904

49.109

49.049

49.009

48.675

49.116

49.037

48.981

48.417

17.812

17.463

17.840

17.434

v

-4.671

-5.495

-3.368

-2.996

-1.470

-1.610

-0.955

-0.80 7

-6.246

-4.185

-0.890

-0.687

-1.495

-1.733

-0.083

-1.293

-2.251

-12.763

-1.638

-0.620

-7.130

-1.029

-0.761

-8.960

-1.334

-1.698

-2.166

-0.280

-0.448

-0.663

-1.438

-0.24 3

-0.499

-0.682

-2.481

-0.894

-2.580

-0.981

T3.340

p.e.

.231

.232

.070

.125

.11C

.14 0

.024

.017

.398

.584

.061

.058

.118

.052

.107

.076

.078

1.C51

.060

.047

.570

.038

.045

.530

.C36

.046

.070

.010

.005

.033

.044

.011

.004

.015

.C45

.016

.140

.022

.230

n

27

28

28

25

22

22

50

53

15

16

37

30

30

30

3 3

26

31

13

31

31

14

36

32

14

37

25

25

59

78

37

31

59

86

44

29

45

20

47

21

m

l

.00205

.C018C

.02370

.024CC

.00853

.00884

.05110

.05540

•002CC

.0018C

.01830

.0219C

.03985

.03951

.00432

.02850

.025CC

.01040

.02660

•C187C

.C0410

.01660

.01870

.C033C

.01620

.05460

.0526C

.07460

.06620

.C614C

.03500

.07610

.06450

.C583C

.02310

.0440C

.0157C

.04300

.01410

s

• •22

+ .31

-.1 8

-.2 0

-.4 0

-.4 6

-.1 4

-.2 3

-.2 6

-.1 2

• .52

+ .41

-.7 9

-.7 6

• •06

-.3 2

-.1 6

+ .49

-.2 3

-.3 5

+ .75

-.2 0

-.3 5

+ .86

-.1 7

-.0 9

-.0 5

-.7 9

-.5 1

-.3 8

+ .17

-.8 5

-.4 6

-.3 1

+ .44

-.0 1

+ .65

+ .01

+ .71

log 0

-11.39

-ll.4!>

-11.04

-11.00

-11.22

-11.31

-11.05

-11.04

-11.55

-11.22

-10.47

-10.36

-11.64

-11.67

-10.90

-11.08

-11.34

-10.98

-10.9H

-11.29

-10.95

-11.07

-11.29

-11.04

-10.7»

-10.1(7

-11.37

-11.37

-11.47

-11.44

-11.34

-11.39

-11.42

-11.38

-10.75

-10.79

-10.80

-10.88

l o s pobs

-8.75

-8.7 0

-8.01

-8.06

-9.16

-9.11

-8.32

-8.38

-8.90

-9.09

-8.49

-8.58

-8.50

-8.44

-10.27

-8.24

-8.01

-7.35

-8.14

-9.14

-8.29

-8.94

-9.05

-8.21

-8.8 3

-B.24

-8.14

-9.64

-9.45

-9.29

-9.03

-9.70

-9.41

-9.29

-8.8 5

-8.33

-8.00

-8.30

-7.91

A log P

obs

-.0 5

-.0 5

+ .0 6

+ .0 1

+ .17

+ .2 6

+ .0 9

+ .0 9

+ .7 7

+ .54

-.6 6

-.7 1

-.3 2

-.2 7

-1.6 8

-.3 7

-.1 9

+ .2 9

-.3 0

-.1 2

+ .23

-.0 1

-.0 3

+ .?7

+ .0 9

-.1 5

-.0 6

• .OS

. 0 6

• .1 3

• .0 2

• •0 3

• .0 7

• .0 8

• •05

-.3 2

-.1 0

-.3 0

-.0 2

A log pc^r

-.1 1

-.1 2

+ .0 9

+ .0 4

+ .3 5

+ .47

+ .1 7

+ .2 1

+ .7 7

+ .5 2

-.7 6

-.7 9

+ .7 4

+ .7 4

-.1 3

-.0 7

-.1 2

-.1 3

+ .02

+ .09

+ .09

+ .11

+ .10

+ .IR

-.0 9

-.0 1

-.0 1

+ .00

+ .08

-.0 3

-.0 3

+ .01

+ .03

+ .00

-.3 0

-.3 2

-.2 9

-.2 6

r

 P

5.5

5.7

7.B

7.8

6.8

6.9

7.6

7.9

7.2

3.8

4.3

4.2

7.4

9.2

0 . 0

8.2

7.7

4.0

7.9

6.7

3.1

7.8

7.5

3.1

7.7

7.4

7.3

9.3

8.7

8.4

6.4

9.4

8.6

8.2

5.2

7.1

4.3

7.0

3.6
NO. i ATMOSPHERIC TRAJECTORIES OF 413 METEORS 8 3

TABLE 1.2.—Basic physical data for US Suver-Schtnidt meteors: Accelerations.—Continued

B log a log po b 6 A log po b a a log p cor r p

Trail No.

'184

1 8 8

'190

'210

'216

7240

72 72

7277

7331

7333

F339

7367

•3 72

a

82.41

81.76

98.74

98.88

94.43

92.00

84.52

76.13

76.22

98.13

94.70

90.31

86.47

97.02

93.93

91.35

85.31

82.74

82.85

95.83

92.48

89.56

84.22

95.81

92.47

89.56

84.23

103.19

102.37

81.65

81.03

97.39

96.83

105.06

105.20

89.49

86.29

89.41

86.88

91.19

91.13

V

22.857

22.786

38.715

38.697

29.438

29.398

28.833

13.402

13.364

31.816

31.740

31.473

30.822

31.810

31.718

31.561

30.416

21.641

21.707

30.841

30.753

30.594

29.790

30.832

30.743

30.579

29.799

60.648

60.609

25.343

25.235

31.244

31.052

44.592

44.425

21.689

21.062

21.711

21.256

21.104

21.013

-1.734

-1.831

-3.090

-2.470

-0.357

-0.718

-5.120

-1.051

-1.20 3

-0.217

-0.512

-1.452

-4.028

-0.302

-0.628

-1.144

-6.142

-2.173

-2.547

-0.458

-1.011

-1.863

-7.962

-0.519

-1.013

-1.760

-7.809

-0.671

-0.705

-2.498

-4.197

-1.414

-1.790

-1.205

-1.296

-1.261

-4.606

-1.370

-4.203

-1.251

-0.665

Y •*- •

.042

.043

.200

.170

.022

.011

.183

.023

.020

.005

.002

.022

.C65

.004

.002

.016

.132

.062

.083

.023

.011

.041

.385

.022

.009

• C3C

.226

.036

.041

.190

.122

• C81

.078

.188

.212

.013

.132

.028

.152

.163

.056

38

33

23

22

41

51

21

48

48

69

97

19

27

69

94

41

23

26

24

40

56

11

17

41

57

31

17

30

28

24

28

38

36

20

24

46

19

46

23

23

10

1

.C2020

.01710

.0195C

.02020

.13110

.U92C

.05740

.11400

.116CC

.29890

.25820

•1754C

.05770

.28760

.2463C

.1985C

.03490

.0454C

.C4760

.09440

.0814C

.C663C

.02650

.09440

.0814C

.0663C

.02660

.004CC

.OO37C

.01670

•0148C

.C0860

.00 790

.C022C

.00220

.033IC

•C116C

.03270

.01600

.C341C

.C336O

0 9

*1

13

17

8 0

5 6

2 2

1 7

1 9

9 4

54

0 5

6 8

8 0

4 5

1 7

9 3

1 2

0 8

8 2

4 8

2 0

4 9

8 2

4 8

20

4 9

28

17

2 7

14

16

0 8

0 6

02

24

55

2 1

36

0 6

0 4

-10.97

-10.91

-11.16

-11.08

-11.07

-11.17

-11.42

-10.77

-10.84

-11.18

-11.28

-11.31

-11.36

-11.24

-11.3 2

-11.3 9

-11.4 1

-10.77

-10.« 6

-11.22

-11.36

-11.4 0

-11.4 9

-11.28

-11.3 6

-11.38

-11.48

-11.1 3

-11.0 6

-11.2 0

-11.3 2

-11.17

-11.2 0

-11.0 5

-11.10

-11.1 5

-11.1 0

-11.1 9

-ll.lo

-10.89

-10.60

-8.37

-8.37

-8.59

-8.68

-9.01

-8.72

-7.95

-7.88

-7.81

- » . 17

-8.82

-8.42

-8.12

-9.04

-8.74

-8.50

-7.99

-8.11

-8.04

-8.99

-8.66

-8.42

-7.90

-8.93

-8.66

-8.45

-7.91

-9.87

-9.86

-8.33

-8.12

-8.86

-8.76

-9.44

-9.39

-8.39

-7.96

-8.36

-7.97

-8.37

-8.64

. 4 8

-.53

• •6?

>.54

-.1 4

-.0 4

• •1 1

-.4 4

-.37

-.01

. 0 7

•.1 1

• .1 0

. 0 4

• .0 9

• .1 2

• •1 3 <

-.1 9

-.1 1

-.0 1

. 0 5

• •0 5

• .1 4

• .0 5

• •0 5

».02

•.1 3

-.3 3

-.3 8

-.4 9

-.3 3

• •24

• .3 0

».24

• .1 0

• •0 7

>.24

t • 10

• .2 8

>.23

-.0 4

-.4 4

-.5 1

. 5 9

.51

.01

• •0 3

• .0 1

. 3 7

-.2 ?

. 0 0

• •05

. 0 6

.01

.03

• •0 7

. 0 8

. 0 3

.18

-.0 9

. 0 8

. 1 2

. 1 0

. 1 3

. 1 4

.12

.07

•.1 2

. 1 6

. 3 0

. 4 1

-.2 9

•.2 3

• .2 *

. 1 4

. 2 3

• .0 8

. 0 5

. 1 0

• •1 4

.34

. 0 5

6 . 7

6 . 2

7 . 6

7 . 7

9 . 3

8 . 9

6 . 1

7 . 7

7 . 8

9 . 5

8 . 8

7 . 3

4 . 2

9 . 3

8 . 6

7.7

3 . 2

6 . 6

6 . 7

8 . 4

8 . 7

7 . 8

4 . 9

9 . 3

8 . 7

7 . 8

4 . 9

7 . 3

7 . 0

6 . 5

7 . 6

b.i

7 . 4

3 . 4

2.8

8.0

4 . 7

7 . 9

5 . 5

4 . 4

5 . 8
84 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

Trai l No.

'J88

'392

,'4 54

".74

4 76

4 7 8

•iSO

/494

7496

7499

/52C

7522

7524

7534

H

83.84

83.96

88.11

87.85

94.84

93.94

91.03

92.16

90.28

97.58

97.86

96.77

94.93

97.00

96.93

89.22

85.64

88.12

85.28

85.56

86.02

79.60

79.56

91.74

92.77

87.05

85.65

82.28

86.75

84.98

80.82

79.62

79.80

100.89

99.31

88.66

86.85

83.96

88.39

86.76

v

23.177

23.240

27.303

27.211

47.083

47.007

46.005

46.598

44.833

36.518

36.542

33.525

33.457

31.678

31.677

18.724

18.203

18.631

18.099

21.163

21.185

13.213

13.248

27.775

27.757

17.025

17.710

17.169

17.837

17.643

16.639

20.838

20.841

35.970

35.911

34.609

34.074

31.594

34.402

33.795

v

-3.638

-2.167

-2.283

-2.210

-1.007

-2.161

-12.413

-7.391

-20.518

-1.46 2

-2.149

-0.831

-1.548

-1.262

-0.985

-0.888

-3.448

-1.323

-4.392

-1.379

-1.194

-3.130

-3.100

-1.762

-1.413

-1.052

-1.521

-3.915

-1.327

-1.S98

-5.237

-1.940

-1.792

-0.739

-1.321

-4.448

-10.068

-33.017

-6.489

-10.343

p.e.

.145

.071

.061

.040

.131

.083

1.194

.234

2.379

.C38

.062

.022

.016

.053

.077

.C16

.191

.022

.157

.059

.057

.220

.2 70

.C67

• C23

.041

.029

.172

.014

.023

.234

.03 1

.036

.03 0

.212

.113

1.489

.32 1

.286

n

21

?0

29

35

31

37

14

25

1C

37

3ft

47

58

42

39

55

23

46

20

37

28

21

21

18

39

42

53

27

39

52

20

35

3 8

19

27

12

17

25

.C284C

.C3O7O

•O3C8C

.0288C

.00810

.0071C

•C029C

•C048C

.00170

•C079C

.00833

.0288C

.02490

.0121C

•012CC

•C6660

.02980

•0588C

• 0243C

.02220

.0245C

.07H 0

.07080

.CI59C

.01760

•062CC

.C533C

.02340

.06020

•04P2C

.01270 .74

11.30

11.09

1 1 . IS

11.11

11.36

11.64

1 1.82

11.85

11.83

11.15

11.34

11.29

11.41

1 1 .28

11.17

11.12

10.96

1 1. 16

1 1.04

10.91

10.94

10.92

10.91

1 1 . 32

11.34

1 1. 16

11.13

1 1 .(I d

11.22

11.15

11.2?

-8.0 1

-8. 2 3

-8.3 5

-8. 3 7

-J. 3 7

-1.0 5

-8.4 1

-8. 5 7

-8. 2 5

-8 . 99

-8.8 2

-8.9 7

-8.7 2

-8. 8 7

-8.9 8

- 8 . J2

- 7 . 82

-8 . 16

-7 . 74

- 8 . 39

-8 .44

-7.4 6

-7.4 7

-8.5 7

-8. 6 5

-8.2 1

-8. 0 7

-7.7 5

-8.1?

-7.9 6

-7.6 9

.09640 -.31 -11.14 -8.02

• 06740 -.39 —10.84 -8.96

.05000 -.05 -10.89 -8.75

.00724 -.52 -11.68 -8.47

.00536 -.12 -11.85 -8.15

.00282 ^.37 -12.36 -7.66

.00698 -.45 -11.79 -8.31

.C0526 -.10 -11.87 -8.13

-.0 0

-.2 2

• .0 0

-.0 4

- . 4 7

- . ??

• .1 8

• .11

• •2 8

• •1 )

• .3 2

• .0 9

• .1 9

• •20

• .0 9

• .12

• • 33

• •n

•• )H

-.2 5

-.2 6

*.2?

• .21

• .OH

• .OH

• .OS

• .Oh

• .13

• •12

• .14

• .OH

- . 33

••4 1

• .5 0

• . 10

• • 35

• .0 6

• -11

-.0 2

-.1 9

• •09

• .03

-.3 3

-.1 9

-.2 6

-.0 9

- .37

• .10

• .30

• .1?

• .23

• .27

• .15

• •2?

*.22

• .24

• •23

-.1 9

- . 19

• .29

• .? *

• .1 2

• .I ?

• .08

• .10

• .14

• . 14

• •15

• .08

-.0 6

• •35

• .45

• .12

• .21

•-2 1

• .13

6 . 7

6 . 9

8 . 2

7 . 9

8 . 0

7 . S

4 . 3

6 . 2

2 . 6

7 . 2

7. 3

8 . 5

7 . 9

7 . S

6 . 0

7. >

5. 3

7 . 5

4 . 8

7. i

1.1

6 . S

5 . 8

7 . 6

8 . 0

8 . 7

H . I

5 . 3

8 . 6

7 . 7

3 . 9

8 . 2

8.3

7.6

7 . 3

7 . 5

5 . 5

7 . 7

7 . 5
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 85

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

Trai l N:..

'56 0

5 6 2

'592

'607

'635

6 1 7

•>64

S66

'726

'734

'74 2

7744

7750

H

84.40

98.28

94.05

89.63

92.02

90.23

84.95

88.2C

88.06

93.98

93.01

91.95

89.26

81.84

87.95

86.60

82.89

85.30

83.56

80.49

82.95

82.91

83.73

82.98

92.91

93.00

76.89

76.77

101.95

102.05

80.77

78.33

76.16

79.85

80.17

81.96

79.75

82.42

v

31.901

37.495

36.935

26.096

26.149

26.027

31.384

31.351

29.480

29.298

31.321

31.241

30.654

31.176

31.094

30.492

17.688

17.465

16.845

17.301

14.411

14.519

14.420

30.593

30.558

15.018

14 • 98 3

42.232

42.214

19.456

19.143

18.488

19.363

19.439

16.577

16.115

16.616

v

-19.S99

-1.926

-8.130

-2.339

-1.189

-1.881

-1.978

-i.ess

-1.537

-2.231

-0.352

-0.583

-3.920

-0.788

— 1 - 358

-5.040

-1.523

-2.063

-3.39 1

-2.170

-1.302

-0.510

-1.342

-1.047

-1.022

—0•770

-1.028

-0.949

-1.057

-2.439

-4.910

-1.490

-1.221

-1.400

-4.218

-1.182

p.e.

1.616

.C82

.490

.C52

.030

.016

.113

.075

.028

• C35

.019

.007

.157

.021

• 01 4

.147

.042

.023

.123

• C28

.059

.130

• C48

• C37

.037

• 100

.C46

.072

.026

.C83

.2 30

• 02C

.C2C

.031

.244

.C17

n

13

2 7

13

37

39

0

24

25

34

37

46

66

23

37

19

38

53

27

42

37

72

3t

4 2

39

41

40

50

32

21

57

52

42

21

44

m

l

.00311

.00819

.00247

.01900

.02420

.00632

.00642

.02U C

.01740

.22020

•189CC

.03480

.160 50

•C235C

.06800

•C1420

.03750

.1465C

.18C4C

.14980

•C111C

.03150

.C0590

.00601

.C453C

.03290

.01650

.C4C1C

.04200

.03150

.01120

•C3360

s

• • 11

-.2 0

-.1 5

• .64

-.0 3

-.2 8

• •23

• -27

-.2 1

-.0 2

-I.0 1

-.5 5

• •77

-.2 9

• •97

-.5 0

+ .72

• .14

- . 3 5

-.7 6

-.3 8

-.0 7

-.0 9

• .03

-.2 0

-.2 2

-.2 0

• .10

• •54

-.0 7

-.1 2

-.1 5

• •58

- .22

log o

-12.1 2

-11.1 6

-11.25

-11.3 4

-11.17

-11.25

-10.8 7

-10.82

-11.10

-11 . 1H

-11.3 1

-11.0 7

-11.0 6

-11.00

-10.9 6

-11.13

-11.06

-10.88

-10.9 4

-10.7?

-10.96

-11.0 6

-11.1 2

-10.60

-11.22

-11.1 9

-11.1 4

-11.3 1

-11.2 3

-11.15

-11.05

-11.0 0

-11.I B

l o g pobs

-7.87

-8.89

- a . 78

-8.42

-8.37

-8.63

-8.75

-8.79

-8.64

-8.50

-B.99

-8.79

-8.20

-8.69

-8.14

-8.03

-7.87

-7.95

-7.81

-8 . 19

-7.80

-8.97

-8.93

-8.18

-9.31

-9.34

-8.33

-8.00

-7.77

-8.20

-8.28

-8.12

-7.77

-8.19

A log p

obs

• . L8

t.2 8

• .3 7

• .4 2

>. 11

.0 4

• •12

-.3 9

-.4 4

• .f

- . 32

-.3 5

-.1 5

-.3 5

-.2 1

• .0 9

-.1 2

-.0 1

• . 12

-.1 9

• .1 4

-.27

-.1 8

-.6 9

• •14

• .1 2

-.5 6

-.4 1

-.3 3

-.5 0

-.5 5

-.0 6

-.2 9

A lo g p corr

• -C6

• .2 6

• • 34

• •3 0

• -O6

• •0?

• .0 2

-.4 7

-.5 3

• .2 0

• -24

-.2 7

-.3 1

-.3 5

-.3 ?

-.2 2

• .0 1

• .06

• .0 1

• •03

• .45

• .4 6

• .4 9

-.1 0

-.6 5

— • 78

• •1 6

• .I")

-.4 4

-.3 9

-.4 6

-.4 2

-.4 6

-.1 7

-.2 0

-.1 8

P

4 . 6

7 . 8

7 . \

7.2

7.4

4 . 5

5 . 5

5 . 9

7. 9

7.2

8 . 6

8 . a

3. 8

8 . 1

7.2

3 . 1

8 . 7

7.2

4 . 0

6 . 5

e . 3

1 .8

8 . 4

7.3

7 . 4

6 . 9

4 - 1

7.8

6 . 3

7.6

6 . 7

4 . 7

7.3

7.5

7.7

4 . 1
86 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

84.C7

84. 11

103.69

103.01

99.49

98.75

86.06

82.39

77.6C

86.49

82.20

77.71

81.02

80.97

104.48

104.83

91.89

88.37

93.32

92.18

87.56

83.90

86.68

83.16

80.75

102.86

103.13

101.32

101.13

89.10

83.53

88.65

83.19

76.44

65.69

59.4C

55.56

51.51

21.788

21.767

45.568

45.247

18.834

18.648

17.889

18.783

18.580

17.878

16.010

15.976

70.430

70.447

25.887

25.356

25.946

25.888

25.054

100.60 62.995

19.385

19.309

18.958

18.261

60.132

60.047

69.365

69.307

21.937

21.257

21.889

21.138

18.373

17.933

17.214

16.169

13.724

-1.195

-1.011

-1.587

-2.880

-0.588

-5.832

-0.479

-1.485

- 4 . 392

- 1 . 126

-1.685

-2.030

-0.892

-0.870

-3.640

-0.514

-0.801

-5.080

-0.525

-1.869

-0.620

-2.037

-5.545

-1.103

-0.938

-1.135

-1.141

-0.740

-4.310

- 1 . 130

-4.590

-0.304

-1.102

-2.837

-5.750

-16.CCO

.C29

.016

.098

.123

.129

.C16

.067

.177

.049

.040

.106

.102

.018

.210

.022

.012

.230

.168

.034

.028

• C79

.137

.207

.191

.054

.029

.006

.075

• C16

.130

.043

.018

.024

.044

.150

.07720

.07870

.00270

•C025C

.28600

.08850

.29160

.22420

.09140

.14310

.14220

•C02CC

.00210

•0349C

•0158C

.03910

.03580

.0117C

.C0340

• 0588C"

.0839C

.04830

.01780

.003CC

.00310

•C087C

.0086C

.08600

.0314C

.08300

.02/70

1.645CC

1.133C C

.7210 0

.44800

.126CC

- . 18

-.2 0

-.3 4

-.3 3

-.0 6

-.1 1

- . 18

• .43

-.3 1

-.2 0

+ .62

-.1 7

-.0 7

-.5 2

+ .10

• -7 1

-.2 1

-.2 3

-.5 7

-.5 4

-.3 5

+ .47

-.3 0

• .54

-.9 4

-.2 1

+ .20

+ .49

+ 1.13

•10.96

-10.90

-11.27

-11.47

-11.12

-11.2 5

-11.2 4

-11.0 8

- 1 1 . 26

-11.1 3

-11.04

-11.2 0

-11.4 6

-11.13

-11.32

-11.19

-11.12

-11.33

-11.47

-11.C9

-11 . 14

-11.02

-11.18

-11.25

-11.1 9

-1 1.43

-11.42

-11.1 3

-11.28

-11.23

-11.26

-11 . 16

-11.38

-11.52

-11.5 9

-1 1.38

-8.30

-8.37

-9.30

-9.05

-8.29

-7.94

-7.42

-8.3 8

-7.91

-7.54

-7.9 7

-7.79

-9.62

-9.9 7

-8.70

-8.18

-8.92

-8.73

-8.07

-8.04

-8.4 7

-8 .02

-7.69

-9.69

-9.75

-9.64

-9.64

-8.50

-7.85

-8.32

-7.84

-8.30

-7.78

-7.40

-7.10

-6.67

1 .6

6.9

7.0

7.4

9.2

8.2

5.1

9.3

8.1

5.2

8 . 3

7.3

4.5

4.7

8.2

7.3

8.8

6.7

4.0

2.4

2.4

8.3

5.0

9.5

7.9

6.2

4.9

2.6
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 87

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

Trai l No.

J C l 2

<C 1 7

:054

068

C 7 5

3 8 3

189

1C6

! 0 8

; ic

H

77.49

65.78

5 8. 94

55.21

51.05

93.62

88.21

82.51

92.89

86.68

82.64

90. 84

89.83

87.44

91.04

90.02

87.21

103.50

107.S9

106.99

105.41

90.68

83.22

91.08

82.54

101.14

102.06

96.19

93.40

90.19

85.97

94.OC

91.23

91.84

95.85

95.78

93.46

92.38

88.58

93.94

92.41

88.50

v

18.400

17.964

17.148

16.027

12.578

29.973

29.641

29.884

29.400

28.375

21. 52 3

21.392

20.840

21.530

21.420

20.738

54.120

54.245

65.377

64.939

37.561

37.455

33.998

65.897

66.352

31.207

31.112

30.916

30.272

31.273

29.569

29.610

43.985

43.976

30.852

30.777

30.190

30.880

30.786

30.167

v

-0.232

-1.C94

-3.151

-6.375

-18.620

-0.825

-2.335

-0.905

-3.633

-10.282

-1.412

-1.752

-3.462

-1.025

-1.606

-5.145

-0.110

-2.220

-0.3?0

-0.597

-18.260

-1.130

-0.561

-0.696

-1.199

-2.192

-8.840

-1.010

-1.789

-1.473

-1.233

-0.856

-1.102

-1.506

-4.800

-0.855

-1.512

-5.550

p.e.

.C09

.C12

.C2C

• C33

.150

.Cl 5

.C33

• C15

.CIS

.169

.032

. 18C

.06?

.039

.109

.018

.4 50

.120

.071

.520

.278

.276

• C21

.019

.080

.770

.C23

.041

.010

.052

.08?

• C55

.C41

.460

.C49

.CIO

.?60

n

72

59

35

23

42

31

41

44

21

19

48

20

35

16

2 1

2 5

26

10

21

16

40

50

28

14

49

41

39

31

31

32

19

18

34

43

20

B

l

1.68300

1 .14C00

.42500

.09060

•1C64C

.07630

.10340

.C653C

.03090

•C3C7C

.01590

.03710

.0318C

.C147C

.01260

•0227C

.00125

•C181C

.01880

•0019C

.00290

.00310

.08320

.05910

.03230

.00672

.06440

.01020

.CUCC

.01178

.01167

.CU7 7

.01012

.00442

.C1237

.C1C37

.00429

:

"

-1.0 5

-.22

• .52

• l.?8

-.8 2

-.22

- . 71

-.0 6

• •47

-.1 4

• .37

- . 18

- . 18

• •42

-.0 3

-1.1 5

• .58

-.5 1

-.5 8

• 1.06

-.2 7

-.1 8

-.5 1

-.0 7

• •17

• 1.18

-.1 6

-.0 2

-.0 9

-.3 1

-.2 9

-.2 0

-.0 7

• •52

-.2 6

-.0 7

• .54

log o

-11.1 0

-11 . Ml

-11.68

-11.51

-11.44

-11.48

- 11.40

-U.5 H

-11.61

-11.19

-11.27

-11.11

-11.19

-11.43

-10.06

-11.48

-10.64

-10.96

-11.98

-11.12

-10.90

-10.95

-10.99

-11.05

-11.40

-10.95

-11.29

-11.29

-11.09

-10.92

-11.22

-11.28

-11.32

-11.15

-11.28

-11.38

l o g pobs

-8.42

-7.7P

-7.06

-6.61

-8.69

-8.2H

-7.71

-8.65

- 8 . 10

-7.73

-S.?5

-8.0 3

-8.46

-8.2T

-7.86

-10.19

-9.58

-9.55

-9.28

-8.04

- 9 . 76

-10.06

-8.84

-8.65

-8.47

-8.07

-8.71

-S.68

-8 .76

-3.17

-9.3 3

-8.91

-8.79

-8.19

-9.01

-8.79

-8.11

A log P

ubs

 A U

-.B9

-.96

-.56

•.11

.OR

• 1 9

.13

. 18

.27

. 1 )

.22

.42

-.82

• .12

-.99

-.6R

-.14

-.37

-.60

.17

.14

.05

.11

• .13

-.07

-.10

-. 19

-. 35

.12

.09

.00

-.18

.09

.05

g

 °cor

.76

.'»0

. 7h

.h?

. 1 1

.04

* 1 t

.30

.0'*

.10

. 1?

.25

.1 7

. It

.24

.11

. > "

. 0 8

. 75

.8'V

. 4 1

.'. r

.41

.64

.09

.OB

.Oi

.14

.Oh

.02

.04

. 4 0

.36

.11

.1 1

.Oh

.Oh

r p

9.6

7. >

6 . 1

7. t

4 . ')

1.2

! . i

5.0

4. I

7.h

7.rt

4 .7

9 . 0

1 .4

0.9

0.0

5. f

1.6

0.0

P . 7

r . i

5.S

? . c

7 . t

7 . 4

5. 7

7 . 8

r. i

3.4

7 .?

7 . 1

4 . 1
88 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

s log o log Po b s Trai l No. A log p A log p

1 13

1 27

1 4 3

1 4 7

1 4 9

1 5 3

.168

1 8 7

•<lfl9

1 9 2

2 1 5

2 2 4

2 3 8

^ 4 0

P>44

54

H

105.79

106.31

92.03

91.05

90.37

90.11

98.79

98.68

92.7 7

92.82

10*.58

104.14

96.18

95.80

87.60

85.42

87.30

87.42

86. 90

94.50

94.29

93.20

99.01

97.22

87.66

93.02

84.61

91.36

84.04

81.99

75.35

96.90

96.04

v

70.620

70.549

26.655

26.511

23.625

23.574

27.344

27.372

24.791

24.819

60.078

60.055

41.475

41.296

21.059

20.565

21.001

25.422

25.244

43.572

43.581

43.604

41.198

41.166

28.485

28.678

27.984

28.635

16.176

16.228

15.066

41.691

41.474

v

-2.860

-3.190

-1.675

-2.222

-0.671

-0.751

-3.070

-0.960

-0.970

-0.750

-0.260

-0.450

-1.870

-2.940

-2.700

-5.070

-2.810

-1.130

-1.380

-0.204

-0.176

-1.009

-0.389

-1.297

-2.960

-0.630

-6.310

-0.967

-0.820

-1.068

-5.140

-2.582

-2.813

p.e.

.14C

.150

.095

.121

.017

.022

• 23C

.400

.140

.160

.140

.C51

.12C

.200

.050

.19C

.080

.210

.240

.088

.111

.032

.011

.059

.13C

.023

.310

.C15

.210

.049

• 26C

.197

.216

n

26

21

31

25

42

37

18

16

31

25

25

32

0

28

26

37

22

34

23

22

30

25

3 0

0

53

40

26

37

17

44

31

40

21

23

17

m

l

.C05C9

.00549

•ooei c

.00672

.08380

.0813C

.00502

.00486

•C163C

.01640

.01C96

.01C39

.00582

.00546

•0114C

.00570

.01070

•C084C

•C0685

.00360

.C0352

.00306

.01127

•ooei a

.05040

.07980

.0229C

-C728C

.09510

•0778C

-C3030

.00168

.00147

11.39

11.47

11.07

11.10

10.82

10.83

I 1.20

10.68

10.81

10.70

10.65

10.86

11.27

11.38

11.20

11.14

11. IB

10.65

10.69

10.49

10.41

1 1.07

10.97

11.31

11.35

11.11

11.18

11.19

11.04

11.07

11.11

11.38

-9.34

-9.28

-8.65

-8.5 5

-8.61

-8.56

-8 .48

-B.99

-8.7 3

-8 .84

-10.13

-9.90

-9.04

-8. 8 5

-8.19

-8.00

-8.18

-8.78

-8. 7 2

-10.11

-10.18

—9 .89

-9.44

-9.62

-9.14

-8.20

-8.81

-7.97

-8.64

-8.18

-8 .09

-7.48

-7.93

-9.08

-9.06

• .39

• •49

+ .02

+ .04

-.07

-.04

+ .73

+ .21

+ .00

-.10

-.49

-.29

-.03

+ .13

+ .12

+ .13

+ .10

-.49

-.47

-1.23

-1.32

— 1.05

-.6 7

-.3 9

-.0 5

+ .11

-.0 6

+ .1 0

-.0 2

- . 16

-.23 .

-.0 9

-.22

-.0 1

-.0 6

+ .34

+ .44

+ .12

+ .0 7

+ . 12

+ .12

+ .83

+ .29

+ .0 7

-.0 3

-.4 2

-.2 5

+ .02

+ .16

+ .10

+ .09

+ .08

-.5 5

-.5 7

-1.3 9

-1.4 7

-1.1 7

-.7 0

-.2 6

-.1 3

+ .07

-.0 0

-.0 3

+ .00

-.1 0

-.2 0

-.1 6

-.2 3

+ .01

-.1 5

7 . 4

7 . 7

6 . 8

6 . 2

8 . 6

8 . 5

5 . 9

0 . 0

3 . 8

2 . 3

0 . 0

5 . 4

7 . 3

7 . 1

7 . 2

5 . 1

6 . 9

1 .7

2 . 0

0 . 0

0 . 0

4 • 4

7.0

7 . 9

6 . 7

7.2

9.1

4 . 4

8 . 7

1 . 7

7 . 6

4 . 3

6 . 7

5 . 9

5 . 5
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 8 9

TABUS 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

log p

413

M5

94.93

96.07

91.76

94.70

95.11

93. 8C

93.43

76.18

73.74

71.35

71.94

105.73

98.39

105.57

98.92

89.06

94.72

77.76

77.78

85.25

84.70

91.03

89.68

85.55

90.50

110.17

110.18

104.33

97.86

94.95

103.94

97.77

89.85

85.02

90.76

81.02

81.21

35.687

35.804

35.381

41.012

41.005

27.840

27.826

14.312

14.078

13.630

13.769

59.892

59.364

59.892

59.385

25.561

26.153

13.928

13.944

28.860

28.707

20.729

20.655

19.882

20.681

60.322

60.464

60.525

60.243

59.900

60.483

60.212

22.016

21.540

22.084

17.639

17.632

-0.806

-0.791

-1.818

-2.830

-2.550

-0.997

-1.163

-0.720

-1.309

-3.488

-2.952

-0.256

-7.609

-0.387

-5.157

-6.410

-0.823

-0.689

-0.740

-2.556

-3.005

-0.373

-0.644

-3.590

-0.416

-0.710

-0.850

-0.366

-1.574

-2.839

-0.38 8

-1.613

-0.902

-3.775

-0.617

-0.795

-0.717

.024

.029

• C97

.180

.120

.C16

.035

.020

.025

• 107

.090

.012

.766

.011

.271

.770

.015

.021

• C23

.394

.387

.006

.004

.C56

.006

.130

• 14C

.003

.024

.118

.002

.017

.CIS

.148

.060

.017

.010

.C1340

.01540

.00590

.00299

.00324

.02040

.01960

.2327C

•1539C

.06630

.08630

•C235C

.00470

.02320

.00618

.00471

.01510

.0639C

.06450

.00748

.00584

.09490

.0849C

.03360

.09100

.CC378

.00381

.07100

.0440C

.02080

.06980

.04340

.06170

.03330

.06540

.42900

.45200

-.18

-.35

• •44

-.09

-.18

-.28

-.23

-.87

-.14

• •47

• •31

-.25

• .83

-.24

• .69

• .65

-.15

• •49

• .64

-.50

-.33

• .43

-.43

-.18

-.19

-.46

• .07

• .56

-.43

• .08

-.45

• .18

-.56

-.27

-.34

-11.21

-11. 34

-11.15

-11.25

-11.32

-11.11

-11.15

-11.01

-10.85

-10.93

-10.99

-10.91

-11.53

-11.09

-11.48

-11.39

-10.96

-10.59

-10.63

-10.83

-10.87

-11.05

-11.20

-11.26

-11.11

-11.03

-11.22

-11.42

-11.48

-11.35

-11.44

-11.48

-11.18

-11.18

-11.08

-10.78

-10.81

-9.15

-9.15

-8.91

-8.95

-8.98

-8.78

-8.72

-7.99

-7.78

-7.45

-7.49

-10.02

-8.77

-9.84

-8.90

-8.11

-8.18

-8.15

-8.55

-8.51

-8.73

-8.51

-7.86

-9.85

-9.77

-9.71

-9.15

-8.99

-9.69

-9.13

-8.46

-7.91

-8.62

-8.05

-8.08

-.24

-.15

-.26

-.06

-.06

• •04

• •07

-.55

-.50

-.32

-.32

-.29

•-41

-.13

•.32

••32

• .03

-.63

-.60

-.43

-.44

-.14

-.03

• .28

-.14

• .18

• .26

-.09

-.01

-.08

-.09

• .00

• •03

• .19

-.05

-.26

-.28

-.31

-.24

-.25

-.02

• .02

• .18

-.34

-.42

-.35

-.33

-.20

-.11

-.04

-.12

• .10

• .10

-.64

-.61

-.34

-.34

• .04

• .07

• •03

• •01

• .21

• .29

-.12

-.06

-.15

-.13

-.05

• .15

• .12

• •09

7.8

8.3

4.6

6.7

7.8

9.4

7.6

5.0

5.7

2.5

8.0

3.7

2.6

7.7

6.6

6.6

2.0

2.6

8.7

8.3

5.2

8.5

3.1

3.9

8.6

6.8

4.6

8.5

6.7

8.6

6.3

6.2
90 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

rail No

.5*6

5 7 2

5 7 6

>6C9

6 4 0

6 4 5

-1648

'658

H668

• 679

1719

•1726

TABLE

H

83.58

80.14

79.28

75.60

73.20

82.97

79.63

78.63

75.38

72.70

107.58

106.68

99.14

98.56

106.14

101.44

99.23

105.65

101.05

98.88

102.53

89.5C

86.0C

73.10

70.00

101.66

99.87

103.41

103.13

95.37

95.25

100.94

101.84

96.79

95.99

105.88

104.45

94.57

105.71

1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

V

18.652

18.445

18.357

17.691

16.730

18.605

18.388

18.241

17.631

16.409

52.724

52.760

61.555

61.315

55.596

55.216

54.816

55.502

55.114

54.719

55.757

36.159

36.175

35.389

37.241

58.353

58.426

60.306

60.445

22.519

22.506

60.646

60.892

60.036

59.720

61.075

61.064

60.263

61.089

v

-0.384

-0.892

-1.189

-2.456

-5.485

-0.425

-0.996

-1.415

-2.757

-6.950

-0.381

-0.566

-4.840

-6.640

-0.557

-1.480

-2.860

-0.521

-1.468

-3.520

-1.570

-0.193

-0.405

-5.890

-37.570

-2.210

-2.160

-1.310

-0.831

-0.815

-0.938

-0.774

-0.228

-1.929

-5.120

-0.212

-0.340

-8.604

-0.132

p.e.

.008

.002

.015

.040

.078

.004

.002

.012

.020

.120

.046

.040

.170

.180

.016

.C85

.140

.023

.118

.240

.480

.018

.012

.170

.770

.160

.310

.110

.098

.032

.053

.026

.046

.C58

.210

.005

.004

.566

.006

»

70

110

51

3 1

2 7

6 5

I d

4 5

3 5

2 5

0

3 5

3 0

20

21

45

26

22

46

26

22

23

4 1

50

19

13

24

2C

23

23

42

3 7

4 1

2 9

2 4

15

53

5 9

17

4 9

m

l

.2082C

.14470

.13190

.0685C

.C285C

.19530

.13690

•119CC

•C6540

.01830

.00337

.00282

•C0495

.00447

.046CC

.07220

.00920

.04420

.021CC

.00780

.02990

.63200

.58500

.22700

.01800

.00559

.00483

.C0522

.00504

.062CC

.C612C

.03570

.0366C

.C0940

.00560

•1555C

.14470

.03840

.1544C

^

-

i

•

A

•

-.62

-.11

-.02

• .4 4

• .9 1

-.4 9

-.05

• .0 7

• •4 7

. 1 2

-.1 3

. 0 3

-.1 1

.02

-.3 3

• .3 1

. 8 0

. 2 8

• .3 5

• .8 8

. 1 0

.10

. 7 8

. 3 0

. 5 7

.38

. 2 0

. 2 0

. 1 6

. 5 5

-.57

. 7 6

. 5 4

. 4 1

. 6 3

. 5 2

log a

-10.8?

-11.1 7

-11.3 ?

-11.32

-11.06

-10.88

-11.2 1

-11.30

-11.38

-11.15

-10.83

-10.84

-11.61

-11.69

-11.49

-11.4 1

-11.3 6

-11.4 2

-11.3 5

-11.4 0

-11.5 8

-11.0 7

-11.1 1

-11.6 6

-11.5 9

-11.61

-11.4 1

-11.14

-10.92

-11.2 8

-11.3 7

-11.5 1

-11.22

-11.46

-10.97

-11.12

-11.70

-10.76

-8.51

-8.19

-A.08

-7.82

-7.55

-8.48

-8.15

-8.01

-7.78

-7.50

-10.02

-9.87

-8.99

-8.87

-9.52

-9.20

-9.01

-9.55

-9.21

-8.96

-9.14

-9.23

-8.92

-7.8 7

-7.35

-9.27

-9.30

-9.54

-9.74

-B.5 3

-8.47

-9.49

-4.28

-8.92

-9.85

-9.65

p

obs

-.5 ?

-.4 7

-.4 2

-.4 2

-.3 0

-.5 4

-.4 6

-.4 0

-.3 9

-.2 8

-. 16

-.OS

• .2 5

• •3 3

• •?4

».2I

.22

. 1 7

• .1 7

.26

. 3 5

-.7 7

. 7 4

. 6 )

-.3 0

• .1 6

-.0 0

• .C2

-.20

• .4 2

• .4 7

-.11

-.22

• .0 8

-.1 1

-.02

-8.43 *.45

-10.05 -.33

A 1Og

 "corr

-.42

-.44

-.40

-.47

-.43

-.46

-.44

-.39

-.45

-.44

-.1 1

-.15

••21

.28

• .1 9

•.1 6

. 1 5

. 1 1

. 1 2

. 1 9

• •30

-.5 5

-.5 7

-.6 2

-.4 8

• •15

-.0 3

• .0 1

-.22

• .60

• .6 4

-.3 8

• •13

• .16

• •05

. 0 9

P

9 . 0

7.5

7.2

5 . 2

3 . 3

8 . 7

7 . }

6 . 8

5 . 0

2 . 7

4 . 5

6 . 3

7.5

7.2

8.3

5.2

3.7

8. 1

4 . 4

3 . 1

0 . 7

6 . 7

9 . 3

5.8

1.6

7 . 6

3 . 9

6 . 3

4 . 6

8 . 8

7 . 9

9 . 2

0 . 0

0 . 0

0 . 0

8 . 8

8.5

3 . 9

8 . 8
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 91

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

766 -

793

! 1 7

6 1 9

B81

H91

111

9 4 3

<)45

9 5 1

9 7 4

93.93

91.14

86.79

83.96

91.08

89.22

84.26

91.08

87.57

88.43

108.40

107.54

92.66

92.61

91.87

90.53

88.61

85.40

82.79

80.47

93.24

91.38

88.62

86.10

83.73

81.46

95.73

91.36

97.31

95.64

90.98

81.86

81.44

100.80

95.45

93.58

88.53

91.68

100.57

101.06

83.44

84.30

23.909

23.832

23.454

22.605

23.891

23.785

22.850

26.077

25.574

25.936

68.775

68.779

45.338

45.348

16.879

16.819

16.684

16.296

15.659

14.652

16.909

16.859

16.716

16.416

15.915

15.179

32.591

32.305

32.635

32.574

32.160

20.413

20.370

19.894

30.807

30.684

29.848

30.513

19.641

19 . 696

25.240

25.312

-0.323

-0.727

-2.613

-7.609

-0.702

-1.265

-6.352

-2.333

-5.626

-4.162

-0.870

-2.310

-1.660

-0.190

-0.304

-0.486

-1.028

-1.610

-2.796

-0.107

-0.207

-0.471

-0.820

-1.393

-2.033

-0.682

-2.010

-0.601

-0.887

-3.070

-1.137

-1.356

-2.430

-0.993

-1.625

-5.920

-2.710

-4.250

-3.460

- 4 . 316

-2.836

.014

.005

.099

.187

.014

.007

.141

.038

.137

.253

.280

.230

.28C

• CIO

.003

.014

.017

.019

.038

.CIC

.C03

.011

.015

.019

.031

.018

.130

.C18

• C12

.140

.C15

• C19

.310

• C55

.029

.140

.24C

.380

.132

.149

5 4

74

2 7

2 0

4 5

5 9

2 1

36

19

2 1

2 6

2 1

2 3

t l

9 0

5 0

39

4 0

34

4 8

6 9

2 7

24

34

33

4 7

2 1

3 8

4 8

21

48

39

26

3 8

4 9

22

18

19

24

22

1

1

1

I

.20180

.17340

.C967C

.03730

.17260

.14440

.0439C

.01200

.00630

.00800

.00153

•C0137

.00464

.08900

.05000

•975CC

.766CC

.50400

.24000

.11500

•C7600

.97500

.82400

.597CC

.3714C

.03660

•C1670

•C4380

.03620

.0148C

.C586C

.05510

.28CCC

.00985

.00837

.00352

•C0691

.31600

.03390

•0729C

-.8 5

-.4 8

• •14

• •71

-.4 7

-.2 2

• •63

-.0 6

• .4 1

- .22

• •26

• •06

• .15

-.2 0

-1.2 4

-1.0 1

-.7 4

-.3 0

• •11

• .58

-1.48

-1 .15

-.7 4

-.4 0

-.0 3

• .32

-.72

• •40

-.4 6

-.2 0

• .47

-.2 9

-.2 1

-1.45

-.3 7

-.1 6

• .48

• •02

-1.3 6

• •36

-.2 8

-11.10

-11.17

-11.26

-11.32

-11.15

-11.21

-11.30

-11.36

-11.28

-11.27

-11.28

-11 . 34

-11.69

-11.13

-11.43

-11.45

-11.51

-11.44

-11.42

-11.33

-11.41

-11.40

-11.52

-11.43

-11.40

-11.25

-10.95

-11.06

-11.00

-11.07

-11.17

-11.03

-11.12

-12.51

-11.29

-11.55

-11.46

-11.50

-12.83

-10.67

-10.71

-8.81

-8.48

-7.9 9

-7.63

-8.49

-8.26

-7.70

-8.43

-8.13 <

—8 .57

-8.24

-10.00

-9.59

-9.20

-8.49

-8.29

-8.09

-7.78

-7.61

-7.42

-8.74

-8.46

-8.11

-7.87

-7.67

-7.53

-9.00

-8.64

-9.03

-8.89

-9 .47

-H.31

-8.24

-7.73 •

-8.JB

-8 .79

-8.3 3

-8.59

-7.45 •

-7.99

-8.06

• .0 2

• •1 2

• •2 5

• •3 8

t.l l

. 18

• •3 4

• . 1 7

. 1 8

* . 15

• .1 4

-.0 9

t.2 6

-.4 8

.26

.28

'.27

.28

• .2 6

.2°,

. 2 5

. 1 2

. 12

.10

.08

. 2 4

-.04

. 5 0

• .1 7 ».2 8

• .2 6 . 3 5

• .3 0 +.3 5

• .3 5 ^.3 5

••3 1 ^.2 6

• •3 3 .22

• -0 3 +.1 7

••1 6 • •2 6

••2 8 +.3 3

• •3 2 +.3 3

•.3 3 +.2 9

• .2 9

-.0 3

-.0 2

.27

. 0 8

. 0 7

• •0 7 •.O l

>.O8

• .1 2

-.4 6

-.4 2

1.6 4 •

-.0 3

. 0 3

. 0 7

-.3 1

. 3 0

).5 l

. 0 6

•.0 1 +.0 7

•.0 5 •.0 6

t.0 5 +.1 0

. 9 0 • ' . 2 1

-.02 ^.04

-.02 . 0 3

9 . 4

8. 7

6 . 5

3 . 6

8 . 6

7 . 9

4 . 4

7 . 3

4 . 8

7.9

5.4

0 . 7

4 . 5

2 • I

3. 1

J . 7

9 . 5

9 . 2

8 . 2

6 . 6

4 . 6

7 . 9

9 . 7

9 . 2

a . 5

7.2

5.7

7 . 9

4 . a

8 . 6

7 . 8

5 . 0

8 . 1

T.H

5 . 1

7 . 5

7 . 7

5 . 0

5 . 6

T.8

7 • 'i

5 . 5

7 . i
92 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

Trai l No.

•1976

?99C

1015

<C10

C 6 2

'087

'IC4

'130

U 4 7

1149

mo

H

107.03

107.29

94.05

91.J5

86 .51

92.23

90.5C

86.31

92.75

89.14

84.67

78.99

91.85

88.25

84.22

79.00

90.01

86.86

82.23

89.64

87.78

82.24

106.87

87.47

87.57

93.06

93.45

89.59

86.09

87.00

84.36

86.77

84.12

100.50

99.71

85.73

86.52

99.86

98.95

96.4?

100.38

V

57.736

57.899

26.760

26.563

26.632

26.489

25.668

30.786

30.714

30.402

28.578

30.850

30.747

30.431

28.844

23.826

23.589

22.654

23.810

23.669

22.598

62.069

19.557

19.475

29.937

29.992

29.737

29.316

17.707

17.383

17.722

17.295

58.608

58.587

48.377

48.260

33.570

33.490

33.105

33.631

v

-1.501

-1.953

-1.054

-1.794

—5.456

-1.243

-2.057

-6.732

-0.410

-1.049

-2.944

-21.400

-0.529

-1.265

-3.046

-16.930

-0.971

-1.933

-6.824

- 1 . 14 2

-1.758

-6.259

-0.943

-2.510

-2.030

-1.224

-0.921

-1.597

-3.285

-1.010

-2.810

-1.260

-3.000

-1.956

-1.895

-2.383

-1.380

-0.810

-1.078

-1.933

-0.858

p.e.

.382

.302

.071

• C26

.499

• C59

.C36

.388

.012

.011

• C71

.910

.015

.011

.C79

.490

.C35

.C83

.163

.024

.C13

.153

.155

.200

.240

.C42

.042

.080

.155

.030

.080

.015

.165

.057

.C72

.129

.147

.052

.033

.236

• C48

n

22

2 0

3 2

4 6

1 6

35

4 4

i e

4 5

6 0

2 4

15

4 3

5 8

2 5

16

4 1

2 9

2 0

4 1

5 3

2 3

2 8

22

22

3 8

4 2

2 6

2 1

4 9

26

4 2

19

2 8

2 5

1 9

2 3

4 2

5 2

24

4 7

m

l

•C0120

.00130

•C172C

•C1300

.01430

.01180

.00540

.C594C

•C5C20

.03330

.00770

.0574C

.04730

.03150

.00790

.0375C

.02500

.00822

•0362C

.02870

.00822

.0O22C

.03750

.04000

.05340

.05450

.03910

.C21CC

.05480

.02740

•C511C

.02420

.00307

.00277

.01900

.02110

.01070

.00920

-0045C

.C117C

11.18

11.32

11.27

11.37

11.53

11.24

11.34

11.59

11. 14

11.27

11.41

11.59

11.20

11.28

11.41

11.51

11.12

11.19

11.28

11.15

1 1. 19

11.24

11.17

11.05

10.96

11.47

11.37

I 1.28

11.11

11.01

10.97

11.08

10.96

1 1. 14

11.26

11.28

11.09

11.17

11.26

11.30

11.22

-J.65

-9.51

-8.75

-8.5 5

-8.70

-8.51

-8.0 8

- 9 . 10

-8.72

- 8 . 32

-7.62

-9 . 00

-8.65

-8.31

-7.71

-8.57

-8.32

-7.90

-8.5 1

- 8 . 35

-7.94

-9. 8 3

-7.99

-8.07

-8.62

-8.74

-8.54

-8.31

-8.24

-7.88

-8.15

-7.87

-9.41

-9.44

-8.90

-9.12

-9.13

-9. 0 3

-S.87

-9.09

• .04

• .20

• •15

• •12

• .09

• •05

• •09

• •16

-.1 8

-.1 6

-.2 1

-.1 1

-.1 7

-.1 8

-.2 5

- . 19

-.0 1

-.0 2

• •0 3

• .02

• .02

-.0 1

-.0 8

• .11

• -29

• .07

-.0 1

-.0 3

• •04

• •02

• .05

• .08

• •01

-.1 1

-.2 1

-.5 7

-.6 1

+ .10

• .1 5

• .1 6

• .1 7

1 . 3

i . i

7 . 7

7 . 4

1 . 9

7 . 8

7 . 1

4 . 3

9 . 1

8 . 3

6 . 8

3 . 3

8 . 9

8 . 1

6 . 6

1 . 5

7 . 9

5 . 4

3 . 7

7 . H

6 . 9

1 . 7

2 . 8

5 . 5

4 . 1

8 . 5

B . 6

6 . 6

5 . 1

8 . 0

5 . 6

7 . 9

4 . 8

7 . 5

7 . 1

7 . 5

6 . 2

6 . 7

6 . 9

2 . 9

7 . 0
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 93

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

Trail No

il 72

91.05

79.70

89.98

94.48

91.49

90.38

89.29

88. 18

90.84

91.64

82.91

82.93

94.68

86.08

81.70

78.36

93.93

86.01

81.67

78.67

91.58

91.84

84.95

82.98

77.68

82.20

94.80

91.53

87.04

81.89

92.79

90.32

82.94

98.77

98.75

83.97

84.51

91.68

90.06

99.61

97.5C

25.084

24.205

25.088

25.095

27.970

27.901

25.955

25.592

29.028

29.060

19.490

19.529

30.249

29.826

29.127

27.486

30.244

29.762

29.085

27.717

30.123

30.308

26.285

26.228

25.733

26.159

30.728

30.651

30.396

29.476

30.523

30.438

29.826

58.320

58.432

21.717

21.783

19.477

19.428

60.299

60.183

-0.133

-10.432

-0.251

-0.116

-1.82 3

-2.450

-1.681

-2.418

-2.577

-1.803

-1.338

-1.040

.004

.382

.C04

.016

35000

0427C

32300

42000

-.46

• 1.00

-.34

-.92

- 10.

- 11.

-10.

-10.

31

20

59

V*

-9

-7

-8

-9

.16

.54

.89

. I 9

-0.428

-1.823

-4.464

-16.417

-0.596

-1.684

-4.923

-13.595

-2.180

-2.591

-0.387

-0.658

-3.395

-0.745

-0.479

-1 .051

-2.916

-8.557

-0.753

-0.957

-3.826

-1.788

-1.810

-1.002

-1.047

-0.639

-0.952

-1.042

-2.177

.028

.C65

.103

.050

.079

.037

.01 3

.C48

.379

.019

.076

.135

.401

.C58

.C81

.013

.006

.109

.015

.016

.007

.089

.401

.C22

.017

.208

.C34

.C89

.179

.021

.031

.120

.080

04 3 2C

C3820

01340

0149C

C2900

02920

2473C

1681C

0278C

2418C

16380

09170

0307C

C1U2

01144

23HC

20100

0595C

18290

22490

19690

14650

C417C

20850

18500

0632C

-.29

- . 15

• •04

-.05

-.15

-.15

-1.05

-.27

• .94

-.95

-.19

• .29

• .89

-.21

-.24

-. 79

-.47

• •55

-.33

-.83

-.50

-.12

•- 72

-.62

-.40

• .49

-11.29 -R.39

-11. 3< -8.24

-11.38 -8.47

-11. K -8.6 1

-11.07 -8.30

-10.96 -8.41

-11.79 -8.86

-11.5 -8.28

-11.53 -7.51

-11.8

-11.4

-8.72

-8.31

-11.57 -7.91

-11.5

-11.3

-11.4,

-11.1

-11.0

-11.1

-10.9

-I 1.1

-11.3'

-11.4f

-11.2

-11.2<

-7 .59

-8.60

-8.53

-8.79

-8.58

-8.0 3

-8.54

1 -8.84

-8.52

-8.11

) -7.80

-8.65

-11.26 -8.56

-11.02 -8.10

C632C

C6660

1781C

1330C

00 72 0

0062C

-.45

-.55

-.55

-.14

-.38

-.20

-11.12

-11.13

-10.72

-10.65

-11.32

-11.51

-8.40

-8.38

-9.35

-8.22

-9.59

-9.29

. 49

. 17

. 14

.1?

. 15

. 18

3.6

3.0

B. 1

6.6

8.0

6.8

•.14

• .10

-.28

-.39

• -0?

-.U6

-.05

•.17

• . 10

-.10

-.02

•-11

• .US)

•.19

-.51

-.5 1

- .5 3

-. 5 7

• .04

•. 1?

• .1 9

• .1 6

• .04

- .01

-.08

-.07

- .06

-.27

-.19

• .?<•

• -24

-. 15

-.2?

6.9

7.1

6. )

7. 7

9.6

7.9

6.0

3 ./

9.5

7.S

5.B

3.4

7. )

8.0

9. 3

8.6

4. 7

8.1

9. 3

a.7

7.5

4 . 0

9.0

8.S

4.5

8.0

B.O

h . 4

1.1

8.8

7.6

5.0

1.6

225-636 O-67—7
94 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

VOL. 10

log a log PQ b s A log Po b s A log p

89.07

83.91

90. 43

86.66

84.00

79.49

89.41

86.84

92.4C

90.47

89.98

90.24

90.19

90.05

92.06

91.68

92.18

89.92

89.40

89.08

92.84

93.22

99.25

99.06

92.52

92.25

92.39

92.53

78.85

69. 36

63.46

80.11

71.19

63.51

87.60

88.20

87.70

85.31

76.40

25.368

24.901

25.417

25.221

24.959

23.969

36.183

36.071

35.158

35.067

35.341

35.336

36.132

36.174

36.857

36.822

36.434

36.510

36.132

36.158

35.972

36.057

58.535

58.424

35.726

35.620

36.378

36.314

35.813

34.834

32.015

35.929

35.195

32.081

36.525

36.616

36.157

36.124

35.347

-1.083

-2.355

-0.819

-1.60 3

-2.898

-6.64 6

-0.841

-1.559

-1.058

-1.121

-0.240

-0.585

-0.781

- 1 . 132

-0.632

-0.970

-1.612

-1.042

-0.935

-1.097

-0.260

-0.402

-1.400

-1.888

-1.984

-3.250

-0.906

-0.838

-1.449

-7.940

-31.500

-1.259

-5.860

-30.400

-1.571

-1.757

-0.473

-0.974

-8.859

.020

.148

.054

.C16

.169

.247

.085

.056

-C62

.103

.116

.133

.054

.042

.C52

.052

.129

.469

.073

.057

.133

.101

• C5C

.112

.076

.C64

.028

.090

.770

.024

.050

.530

.135

.103

.C14

.009

.143

.08990

.05690

.0956C

-1 1.36

-11.2 2

• 1 1.44

-R.45

-8.17

-8.57

.05780

.0117C

.04410

.03500

•C1540

.01360

.01440

.C1520

.02930

•029CC

.02010

.01930

.0176C

.01320

•0168C

.C164C

.C0390

.00380

•C154C

.01490

.0054C

.C055C

.29100

.15CCC

•C57CC

.30700

.18100

.0577C

.03140

.03270

.20750

.17440

.05530

-11.1 2

-11 . 14

-11.3 3

-11.1 7

-10.11

-10.4 9

-11.0 6

-11.2 1

-10.7 9

-10.92

-11.27

-10 . 70

-11 . 17

•11.22

-11.34

-I 1.46

-11.3 1

-11.4 7

-10.8 6

-10.8 3

-11.50

-1 1.85

-12.14

-11.51

-11.81

-12.13

-11.32

-11.42

-10.S7

-11.02

-11.64

-8.0 7

-7.91

-8.9 7

-8.74

-9.00

-8 .99

-9.66

-9.27

-9.06

-8.91

-9.21

-9.05

-8.8 3

-9.06

-V.07

-9.00

-9.52

-i .39

-8.74

-8.5 3

-9.25

-9.28

-8 .46

-7.79

-7.26

-8 .51

-7.90

-7.27

-8.76

-8.71

-9.00

-8.71

-7.90

-.0 2

- . 16

-.0 3

-.0 5

-.2 3

-.5 1

-.4 9

-.3 0

-.4 4

1.16

-.7 4

-.5 4

-.4 0

-.5 5

-.4 1

-.1 4

-.5 6

-.6 1

-.5 7

-.0 3

-.1 0

-.0 6

-.0 5

• .00

-.0 5

-.5 0

- .46

-.1 0

-.3 0

-1.1 1

- . 70

-.4 2

-.2 9

-.4 5

-.1 1

-.0 5

-.5 0

-.5 5

-.5 1

8.6

6.1

8.0

7.9

6.2

1.1

6.2

7.9

7.0

5.8

0.0

1.5

7 . 7

6.4

7.0

6.9

0.0

6.4

7.1

5.7

3.1

8.5

8.3

5.8

5.9

8.3

5.9

1.7

8.5

6.5

3.7

6.6

7.6

9.0

8.3

4.6
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 95

TABLE 1.2.—Baric physical data for 413 Super-Schmidt meteors: Acceleration*.—Continued

Trail Ho.

1804

IS 15

1833

(880

1888

1900

9917

9925

9945

1951

H

87.51

84.52

75.64

102.85

100.93

99.62

100.08

83.57

84.13

88.93

86.93

83.85

85.76

83.61

88.39

84.91

82.40

80.21

90.89

86.29

83.73

81.37

79.21

88.10

84.98

80.08

85.85

83.75

79.63

85.18

81.04

77.51

82.06

84.25

80.12

77.25

81.94

97.15

98.30

97.73

97.89

100.05

98.82

V

36.160

36.090

35.112

72.414

72.577

59.203

59.539

24.810

24.841

25.767

25.650

25.328

25.570

25.293

18.598

18.233

17.723

17.169

18.740

18.428

18.021

17.477

16.791

23.754

23.592

22.990

23.584

23.444

22.863

16.038

15.518

14.705

15.693

15.878

15.408

14.685

15.657

44.339

44.351

41.172

41.278

60.317

59.827

V

-0.629

-1.185

-10.127

-3.215

-2.473

-7.290

-3.059

-1.311

-0.938

-0.342

-0.526

-0.896

-0.733

-1.091

-0.493

-1.28S

-1.670

-2.067

-0.311

-0.935

-1.547

-1.845

-3.095

-0.569

-1.074

-2.795

-0.806

-1.335

-3.240

-1.299

-2.097

-4.640

-1.907

-1.012

-2.404

-4.590

-1.711

-4.150

-3.188

-2.155

-2.401

-5.558

-4.254

p.e.

.C26

.CIO

.218

.C83

.070

.154

.115

.087

.084

.009

.005

.027

.011

.061

•C12

.014

.033

.043

.006

.C15

.028

.030

.059

• 027

.009

.067

.020

.010

-09C

.027

.037

.153

.010

.037

.068

.187

.015

.125

.135

.093

.271

.403

.539

n

38

48

19

27

20

22

20

29

25

68

ICO

53

74

40

55

48

38

34

77

50

40

37

31

37

61

31

42

57

26

39

33

25

66

38

28

20

57

23

21

28

21

14

16

" l

.20510

.16110

.0464C

.03260

.02710

.00570

.00830

.01C9C

.C125C

.17310

•1326C

.0686C

.10260

.06500

.32800

.22000

.13800

.0835C

.3720C

.27100

.17600

.109CC

.06650

.09730

•0776C

.02810

.08380

.06880

.02380

.09910

.066 30

.02770

.07560

.09740

.05720

.02460

.07450

.C0740

.01070

.00590

.C0610

.00173

•0015C

8

-.62

-.24

• .65

-.30

-.10

• .65

• .45

• .45

• •37

-.63

-.21

• .33

• .03

• .36

-.40

• •04

• •28

• .65

-.63

-.16

• .21

• -51

• •77

-.71

-.30

• •50

-.41

-.16

• •59

-.44

• .01

• •59

-.11

-.34

• .13

• .65

-.09

• .30

• .03

-.12

-.16

-.17

-.03

log a

-11.07

-11.04

-11.61

-11.31

-11.03

-11.38

-11.09

-10.36

-10.66

-11.18

-10.95

-11.16

-11.06

-11.24

-11.22

-11.20

-11.30

-11.33

-11.19

-11.32

-11.32

-11.23

-11.50

-11.26

-11.25

-11.07

-11.15

-11.23

-11.12

-11.32

-11.22

-11.05

-11.28

-11.17

-11.18

-11.04

-11.22

-11.20

-11.16

-11.35

-11.42

-11.73

-11.52

108 pob.

-8.88

-8.63

-7.86

-9.04

-9.18

-8.76

-9.09

-8.65

-8.78

-8.87

-8.72

-8.57

-8.61

-8.49

-8.34

-7.96

-7.89

-7.84

-8.53

-8.08

-7.90

-7.87

-7.68

-8.66

-8.41

-8.12

-8.53

-8.33

-8.08

-7.96

-7.78

-7.5?

-7.81

-8.07

-7.74

-7.54

-7.86

-8.72

-8.78

-8.97

-8.9?

-9.07

-9.20

Alo8«>ob. l

-.58

-.57

-.45

• .48

• .20

••52

• •22

-.67

-.75

-.45

-.47

-.56

-.45

-.50

• .03

• •13

• .0 0

-.1 1

• .05

• •12

•.1 0

-.05

-.0?

-.31

-.31

-.40

-.36

-.33

-.39

• .15

•.01

• .Cl

•.06

-.03

-.02

-.02

-.00

• •37

• •40

• .16

• .22

•.24

.0?

> * *

 poorr

-.4 4

-.4 8

-.5 0

• .4 1

• .14

• .2 8

• .04

-.7 9

-.8 5

-.4 5

-.4 3

-.4 9

-.4 0

-.4 2

-.0 5

• .0 8

-.0 2

-.1 1

-.0 5

• .0 6

• .06

-.0 6

-.0 1

-.3 5

-.3 3

-.3 7

-.3 8

-.3 4

-.3 5

• .16

• .0 6

• •1?

• .10

-.0 1

• .0 4

• .0 8

• .04

• •2 1

• .3 3

•.21

• .29

• .23

-.03

P

9 . 0

8.0

4 . 3

8 . 2

6 . 7

4 . 3

$ . 1

4 . 6

4 . 4

9 . 0

7.9

5.6

6 . 9

5.5

8.5

6.9

5.9

4 . 3

9.0

7 . 7

6.2

4 . 9

3.8

9 . 1

8.2

4 . 9

8..5

7.7

4 . 5

8 . 6

7.0

4 . 5

7 . 5

8 . 3

6.5

4 . 3

7 . 4

5 .8

6 . 9

7.5

5 . 4

7 . 0

4 . 3
96 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

Trail No.

4953

S955

,9 74

9983

,985

SS97

1C006

10012

1CC64

UC70

1 :094

1 3098

101C6

1U127

10173

1C218

H

96.23

98.65

99.35

95.28

95.30

94.37

91.43

94.18

93.89

94.52

94.39

96.75

95.97

102.25

102.84

85.74

85.43

91.74

84.21

78.70

73.94

89.76

83.35

79.30

75.76

99.58

91.00

85.52

85.40

86.46

88.89

85.47

86.08

77.84

77.03

93.08

93.67

V

42.654

42.987

42.895

42.937

43.089

43.098

42.931

42.804

42.223

42.114

43.018

43.082

42.983

43.035

64.461

64.450

28.820

28.807

25.937

25.607

24.632

21.160

25.911

25.467

24.773

23.177

49.218

48.878

48.180

45.342

45.457

30.697

37.240

37.161

16.966

16.965

27.175

27.264

V

-7.607

-0.880

-4.471

-2.912

-0.633

-0.485

-1.511

-3.940

-3.140

-2.420

-7.703

-7.093

-2.035

-1.509

-2.260

-2.585

-0.816

-0.604

-0.401

-2.048

-6.969

-26.692

-0.721

-2.403

-5.611

-16.340

-0.567

-2.387

-7.660

-1.872

-1.385

-0.479

-5.610

-3.C40

-0.573

-1.107

-1.690

-1.879

p.e.

.27 3

.229

.242

.288

.027

.017

.061

.036

.C90

.170

.3 74

.337

.059

.152

.284

.184

.077

.111

.014

.047

.108

.930

.025

.C83

.178

.529

.032

.085

.370

.032

.013

.016

.270

.380

.C27

.032

.036

.C44

n

15

2C

20

21

34

31

29

16

27

21

21

19

30

23

21

23

32

32

59

40

30

19

53

35

25

17

35

23

15

3t

38

57

18

16

35

35

35

33

m

l

.00450

.00650

.CC491

.00531

.01660

.01670

.02100

.01230

.00862

.00824

.00192

.00187

•005CC

.00420

.00180

.00205

.00960

.00880

.12220

.08660

.04750

.OICCC

.U40C

.08120

.05230

.024CC

.08550

.05330

.0193C

.10010

•11570

•0433C

.01470

.O2O3C

.04670

.04000

-C189C

.02040

s

-.C2

-.4 4

-.2 7

-.3 8

-.1 7

-.1 8

-.3 1

• .19

-.3 2

-.2 6

-.0 3

-.0 1

-.1 5

• •01

-.0 2

- . 14

+ .53

+ .58

-.7 4

-.1 7

+ .31

• 1.13

-.5 7

-.1 1

+ .25

• •70

-.7 7

-.0 6

+ .62

-.2 9

-.5 0

-.3 7

+ .33

• •10

-.1 1

+ .03

-.1 5

-.2 3

log a

-11.79

-11.C7

-11.81

-11.61

-11.00

-10.89

-11.22

-11.3 1

-11.51

-11.3 0

-11.67

-11.62

-11.25

-11.00

-10.98

-11.13

-10.bb

-10.46

-11.15

-11.53

-11.67

-11.61

-11.35

-11.54

-11.63

- 1 1.78

-11.53

-11.6 1

-11.37

-11.32

-11.38

-10.^2

-11.16

- 10.94

-10.5 6

-10.83

-11.13

-11.25

l o g pobs A lo g pobs

-8 .49

-9 .38

-8.71

-8.89

-9.39

-9.51

-8.9 8

-8.63

-8.77

-8.89

-8.62

-8.66

-9.05

-9.51

-9.4 3

-9.01

-9.15

-8.86

- 8 . 19

-7.71

-7.22

-8.61

-8.12

-7.80

-7.39

-9.32

-8.75

-8.38

-8.70

-8.82

-9.08

-8.3 3

-8.55

-8.4 7

-8.21

-8.55

-8 .49

+ .36

-.37

+ .49

+ .37

-.45

-.57

- . 12

-.01

• -C8

-.06

+ .26

+ .21

+ .00

-.22

-.04

+ .09

-.85

-1.0?

-.21

- . 16

-.09

+ .08

-.12

-.15

-.14

+ .02

-.05

-.16

-.24

-.57

-.60

-.67

-.19

-.37

-.9 1

-.71

• .21

+ .32

A lo g p

corl

+ .38

-.09

+ .63

+ .56

-.32

-.43

-.01

-.07

+ .20

+ .03

+ .23

+ .18

-.02

-.23

-.09

+ .03

-.63

-.78

-.08

-.09

-.09

-.02

-.01

-.10

-.n

-.0 2

-.2 1

-.2 2

-.2 0

-.63

-.6 7

-.4 7

-.2 6

-.39

-.7 7

-.6 8

+ .27

+ .40

. P

7.2

1.7

7.3

5.9

7.7

7.8

8.2

5.0

8.2

7.2

7.2

7.1

7.7

4.9

4.3

6.9

3.3

1.8

9.2

7.7

5.7

2.4

8.9

7.5

6.0

3.7

8.3

7.3

4.4

8.1

8.7

8.4

5.6

4.0

7.5

6.9

7.7

7.9
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 97

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

p

corr

1C222

102*10

10247

10252

1C255

10273

10279

K28 1

10342

103 58

1C365

10380

1038*

10394

104 14

97.76

99.25

97.56

93.03

84.45

84.83

99.20

87.28

87.86

81.05

81.62

89.74

89.42

73.22

73.23

91.49

90.62

85.93

90.90

86.71

93.06

89.51

89.28

95.76

92.29

85.25

95.35

81.65

91.14

84.84

85.39

86.62

76.47

69.26

63.58

88.46

39.246

39.330

39.220

38.486

34.122

34.221

55.090

20.063

20.231

20.270

20.348

26.349

26.375

12.896

12.894

29.369

29.339

28.877

29.101

28.590

24.942

45.062

45.199

33.272

33.107

32.372

33.134

31.244

32.956

14.361

14.443

16.798

It.047

14.404

11.039

16.829

-1.261

-0.774

-1.246

- 4 . 182

-2.974

-3.053

-2.280

-2.589

-1.104

-1.204

-1.530

-0.730

-0.740

-0.910

-1.017

-0.911

-1.310

-6.120

-1.59 8

-4.350

-0.495

-11.293

-11.694

-0.831

-1.190

-3.330

-0.666

-10.210

-1.442

-1.484

-1.219

-0.271

-1.345

-2.962

-6.212

-0.203

.013

.019

.014

.215

.096

.C90

.140

.C27

• C9?

• C16

.043

.C22

.C22

.012

.019

.022

.028

.220

.C27

.170

• C38

.224

.368

• C16

.012

.100

.021

.190

.010

• C30

.02 1

.C22

• C20

.02 7

.02 1

• C07

0

62

45

58

23

27

28

2 3

43

32

0

53

38

48

44

57

51

38

42

20

40

21

4 4

2C

18

4<3

68

29

50

21

73

47

55

36

25

24

46

40

.00920

.0111C

•0069C

.00290

.0085C

.C0960

.01010

.20700

.26800

.01560

.01720

•C2300

.02200

•1633C

.1638C

.01580

•0143C

.00605

.01480

.00734

.03C0C

.00500

.0046C

.07120

.05980

•0293C

.C7C2C

.01340

•0549C

.07310

.08660

3.0670C

2.09100

.90000

•172CC

3. 13800

-.0 5

-.2 5

-.0 3

+ .70

• .09

• .00

-.2 3

-.2 3

-.6 4

• •C6

-.0 2

-.2 4

-.1 9

-.1 8

-.1 8

-.1 1

-.0 2

• .56

-.0 5

• -45

-.1 3

-.0 9

-.0 3

-.4 9

-.2 4

• .35

-.4 6

• .13

• •78

-.1 4

-.0 2

-.1 8

-1 .33

-.2 7

• .41

• 1.25

- I .64

-11.35

-11.24

-11.3 3

-11.41

-11.09

-11.18

-11.39

-11.23

-11.10

-11.CO

-11.12

-11.13

-11.12

-10.79

-10.84

-11.0 0

-11.10

-11.32

-11.20

-11.31

-10.81

-11.82

-11.80

-11.52

-11.43

-11.50

-11.40

-11.53

-11.68

-11.45

-10.86

-10.92

-11.45

-11.55

-11.31

-11.29

-11.46

-9.10

-9.28

-9.10

-8.7 3

-8.61

-8.59

-9.12

-7.75

-8 .09

-8.4 7

-8.35

-8.8 5

-8.8 6

-7.85

-7.81

-8.91

-8.76

-8.20

-8 .66

-8.31

-8.94

-8.35

-8.35

-8.84

-8.70

-8.34

-8.9 3

—8 .44

-7.93

-8. 6 3

-7.85

-7.92

-8.19

-7.51

-7.19

-6.88

-8.31

-.0 1

-.0 7

-.0 3

-.0 5

-.5 3

-.4 7

• .09

• .63

• .43

-.6 5

- .46

-.12

-.22

-.4 8

-.4 4

-.2 9

-.2 3

-.21

-.1 0

-.2 2

-.11

• . 10

• .0 6

• .0 7

-.0 1

-.0 9

-.04

-.04

• .14

-.01

• .25

*.2?

-.06

-.04

-.1 0

-.0 2

7 . 3

8 . 0

7 . 2

3 . 7

6 . 7

7 . 1

7 . 1

l.H

7.2

6 . H

7 . 2

8 . 0

7 . 8

7 . 8

7.B

7 . 5

7 . 2

4 . 6

7 . 3

5 . 1

b . l

7 . 4

7.2

8 . 7

8 . 0

5 . 6

8 . 6

6 . 5

5 . 8

7 . 6

7 . ?

7 . H

7 . 8

8 . 1

5 . 3

7 . 3
98 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 1.2.—Basic physical data for 413 Super-Schmidt meteors: Accelerations.—Continued

Trail No.

10439

10447

10478

10480

10531

10555

1 C566

10583

10587

11816

1 1818

11825

H

77.04

69.39

63.80

93.73

90.90

85.53

96.14

93.09

85.57

94.80

93.12

89.29

93.86

92.60

89.14

87.14

95.57

95.8C

96.58

95.77

80.10

80.65

95.28

109.46

105.86

110.48

96.65

97.72

90.36

89.61

87.27

83.00

78.99

76.70

74.39

92.41

91.01

86.36

92.65

91.00

86.37

V

16.145

14.455

11.271

34.577

34.322

33.194

34.532

34.413

33.418

33.631

33.548

33.218

33.635

33.573

33.286

23.246

22.343

22.319

50.847

5C.850

17.534

17.641

26.118

68.892

68.460

68.810

36.566

36.536

19.777

19.662

15.377

15.123

14.534

13.885

12.712

22.847

22.780

22.181

22.807

22.735

22.224

-1.228

-2.964

-6.098

-1.465

-2.520

-6.560

-0.688

-1.249

-6.710

-0.72 9

-0.919

-1.805

-0.746

-0.938

-1.886

-2.455

-1.507

-1.091

-2.129

-2.706

-2.744

-2.217

-0.622

-3.C90

-0.344

-0.993

-0.728

-0.267

-0.621

-0.710

-0.811

-2.193

-2.930

-5.715

-0.614

-0.960

-4.378

-0.542

-0.828

-3.134

0 0 8

C 1 6

0 2 7

0 6 5

C34

3 4 0

0 1 9

O i l

2 6 0

0 2 2

C 1 2

C 6 8

C 3 8

0 2 8

1 0 1

C 5 1

0 6 3

1 8 4

0 5 7

0 5 0

1 0 4

1 0 5

C 1 6

0 2 2

3 9 0

C 3 2

0 2 1

0 1 6

0 0 7

0 4 3

C 1 3

O i l

0 2 1

0 5 1

2 2 9

0 2 4

0 1 4

1 5 5

0 1 5

0 0 8

1 1 2

30

45

4 1

35

50

?3

4 3

5 9

2 3

4 2

54

2 9

4 5

5 1

26

35

31

31

2 9

27

2 3

26

64

5 0

19

4 7

3 3

4 0

72

3 8

54

5 1

39

29

21

4 8

59

2 3

4 5

5 8

2 3

2.167CC

.93200

.19500

.0523C

•C431C

.C1840

.05800

•05C40

.01880

.03860

.03340

.01510

.03560

.03180

•0143C

.10500

.0324C

.0343C

.00940

.00B8C

.10130

.13030

1.15C5C

.00581

•CCC86

.00700

.05240

.0590C

.13150

.10110

.91990

.62550

.31460

.1634C

.03911

.07880

.0695C

.02020

.08020

.06950

.C202C

-

•

• 1

-

-

-

-

-

-

-

-

-

-

-

- 1

_

• I

-

_

-

-

•

f

• 1

-

t

-

-

+

. 12

. 3 9

. 19

. 4 8

. 2 1

. 4 5

. 70

. 4 2

. 4 3

. 38

. 2 0

. 4 2

. 2 7

. 14

. 4 5

. 2 9

. 1 2

. 1 8

. 0 7

. 0 1

. 0 5

. 33

. 2 5

. 0 9

. 0 4

. 3 0

. 2 7

. 4 3

. 16

. 0 8

. 9 7

. 2 0

. 3 5

. 7 2

. 4 0

. 5 6

. 3 5

. 6 0

. 5 9

. 3 5

. 6 0

-11.54

-11.3 0

-11.3 0

-11.6 3

- 1 1.63

-11.5 1

-11.46

-11.5 2

-11.54

-11.2 2

- 1 1. 30

-10.90

-11.24

-11.2 9

-10.9 2

-11.10

-11.35

-11.2 4

-11.47

-11.5 5

-io.e s

-10.93

-10.79

-1 1.16

-11.26

-11.05

-10.97

-10.98

-10.79

-10.96

-11.53

-10.92

-11.31

-11.20

-11.11

-11.08

-11.14

-11.09

-11.05

-11.08

-10.95

-7.55

- 7 . 18

-6.89

-8.67

-8.46

-8.13

-8.98

-8.74

- a . 13

-8 .99

-8.91

-8.7 2

-9.99

-8.91

-8.71

-8 .00

-8.35

-8 .48

-9.09

-9.00

-7.71

-7.7 7

-8.7 7

-9 .96

-9.5 3

-10 . 19

-8.89

-9.00

-8 . 79

-8.46

-7. 8 7

-7.85

-7.48

-7.4 1

-7.25

-8. 6 3

-8.45

-7.95

-8.68

-8.5 1

-8.0 9

.07

.07

5.4

2.5

7.9

4.6

9.1

8.5

5.2

7.8

5.2

7.3

7.6

4.6

7.5

3.1

7.3

7.1

7 . 3

8 . 3

7.4

1.7

6.5

8.1

8.5

7.7

6.1

9.5

7.8

5.6

4.0

2.0

8.9

8.3

4.5

8.9
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 99

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

85.70

85.12

82. 8C

86.00

85.03

82.53

98.83

97.38

90.80

98.30

96.84

91.01

87.67

86.88

83.22

87.91

86.56

84.35

93.13

90.40

87.85

91.41

92.53

90.22

88.08

91.12

89.04

87.44

85.48

87.68

91.19

87.63

85.52

87.84

85.24

80.51

88.33

85.86

81.53

93.28

89.69

86.60

83.79

89.73

94.06

20.611

20.576

20.289

20.621

20.569

20.223

-0.404

-0.553

-1.856

.010

.009

-C84

.06070

.O53CC

.C2218

-.1 3

+ .00

• .58

-10.6?

-10.7R

-11.04

10(5 "obs

-8.76

-8.64

-8.2 3

108.16 66.686

44.820

44.776

44.206

44.813

44.768

44.321

22.884

22.842

22.169

22.997

22.866

22.360

22.385

22.127

21.557

22.240

22.340

22.080

21.639

22.205

18.350

18.143

17.685

18.171

18.620

18.191

17.708

19.831

19.616

18.393

19.897

19.718

18.817

19.201

19.006

18.564

17.575

19.007

19.228

-0.576

-2.619

-0.929

-1.303

-6.381

-0.897

-1.276

-5.045

-0.643

-0.960

-5.7U

-O.e85

-1.734

-4.546

-0.508

-1.003

-3.C60

-0.831

-1.083

-2.269

-0.897

-0.506

-0.763

-1.480

-0.776

-0.410

-0.832

-1.371

-1.144

-2.307

-9.815

-1.060

-2.059

-7.786

-0.147

-0.542

-1.000

-3.514

-0.477

-0.155

.012

.102

.067

.029

• C18

.169

.031

.018

• 182

.020

.014

.207

.068

.026

.120

.012

.019

.088

.006

.026

.117

.008

.0 17

.C23

.057

.006

.0 14

.C24

.052

.051

• C21

.291

.034

• C14

.137

.005

.009

.011

.C43

• C01

.005

.05190

.01917

.00400

.0179C

.01640

.00489

.01740

•0157C

.C0528

.02460

•0213C

.C0944

.02560

.02010

•0134C

.09580

-0598C

.C096C

.07530

.05680

.01380

.07070

.35370

.26540

.11690

.27980

.45720

.27700

.12030

.12410

•C9740

.03080

.12760

.10450

.04760

.76300

•543CC

.2C90C

.03140

.54800

.791CC

-.19

-.5-*

-.38

+ .57

-.47

-.32

• •53

-.04

• •08

• .60

-.08

•.12

• .40

-.54

• •03

• 1 .07

-.19

-.16

• .10

+ .61

+ .06

-.51

+ .06

+ .60

-.69

-.27

+ .59

-. 76

-.36

+ .33

• 1.41

-.27

-1.22

-10.79

-11.03

-11.34

-11.38

-11.42

-11.29

-11.31

-11.34

-10.77

-10.97

-11.42

-10.99

-11.22

-11.48

-11.15

-11.02

-10.75

-11.09

-11.16

-11.01

-10.62

-11.10

-11.09

-11.10

-10.85

-11.14

-11.25

-11.17

-10.64

-11.23

-11.30

-11.23

-11.28

-11.30

-11.40

-10.96

-10.97

-11.02

-11.22

-10.93

-11.17

-8.62

-8.10

-9.25

-9.11

-8.59

-9 .2 7

-9.13

-8.68

-8.78

-8.62

-7.94

-8.64

-8.37

-8.00

-8.66

-8.43

-8.18

-8.48

-8.57

-8.40

-8.27

-8.45

-8.30

-8.16

-7.97

-8.14

-3.37

-8.12

-8.00

-8.17

-7.89

-7.3 7

-8.20

-7.93

-7.43

-8.77

-8.24

-8.09

-7.7 7

-8.30

-8.74

sbs

6 1

31

5?

2 0

? 2

0 3

0 1

0 2

0 9

0 7

0 9

4 7

3 7

0?

31

15

0 5

10

11

15

14

14

12

0 8

15

1 3

14

17

1 7

2 3

19

14

16

2 3

38

17

24

4 0

0 1

2 4

14

2 3

18

10

A log Pcorr

-.4 9

-.48

-.53

-.4 8

-.4 6

-.2 6

-.0 9

-.06

-.06

-.1 5

-.1 2

-.1 3

-.4 4

-.4 3

-.42

-.25

-.2 3

-.2 5

• •05

*.bb

• .11

+ .09

+ .09

• .07

• .04

• .10

+ .11

+ .14

• .20

• •17

+ .20

• .19

• .17

+ .30

+ .29

• .28

+ .32

+ .32

+ .35

+ .06

+ .25

• .10

•-1 4

+ .19

• .17

P

7 . 6

7.1

4 . 6

7.0

7.0

4 . 2

3 . 9

B . 8

8 . 4

4 . 6

B . 6

8 . 2

4 . 8

7 . 2

6 . 7

4 . 5

5 . 9

6 . 6

5 . 3

8 . 8

6 . 9

2 . 8

7 . 8

8 . 5

6 . 8

3 . 0

7 . 6

7 . 7

6 . 7

4 . 4

6 . 8

H . 7

6 . 8

4 . 5

9. 1

8 . 1

4 . 5

9 . 2

8 . 3

5 . 6

9 . 5

8 . 0

5 . 0

1 . 9

0 . 0

9 . 7
100 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 1.2.—Basic physical data for 418 Super-Schmidt meteors: Accelerations.—Continued

Trail No.

2577

12714

H

90.39

87.26

83.S9

90.16

94.47

89.70

85.58

91.63

94.62

89.54

85.42

91.92

93.53

91.46

88.03

91.89

v

19.04 3

18.682

17.673

19.035

29.537

29.29 3

28.587

29.429

29.576

29.294

28.536

29.477

25.697

25.597

25.344

25.588

v

-0.469

-0.786

-J.984

-0.425

-0.459

-1.677

-5.589

-0.968

-0.457

-1.643

- 7 . 124

-0.946

-0.843

-1.132

-1.804

- 1 . 163

p.e.

.006

.008

.096

• C01

.025

.038

.124

.007

.024

.C8C

.274

.009

-C24

.C19

.081

.022

n

7 1

7 1

35

172

4 1

2 9

19

6 0

4 4

2 7

1 9

6 ?

35

4 7

2 7

" l

.60500

.261CC

.03640

.58800

.07650

.054CC

.02180

.06490

•077CC

.C5260

.02060

.06620

•C5720

.04290

.01460

s

-.4 1

• •35

• 1 .34

-.3 7

- . 59

-.1 1

• •53

-.3 2

-.6 0

-.0 8

• .56

-.3 4

-.4 8

-.1 1

• .6?

-Log a

-11 . 14

-10.9 2

-It.2 9

-11.0 4

-11.2 1

-11 . 37

-11.4 1

-11.3 4

- I 1.22

-11 . 34

-11.5 0

-11.3 5

-11.0 4

-10.8 6

-10.fa?

6 po bs

-8. 2 9

-8.1 7

-7.7 1

-8.3 4

-8 .

-8 . '

-8. 1

-S .(

-8 .

-8 . '

_7 s '

- 8 .c

- 8 . f

- 8 .

- 8 .<

)8

6

5

8

)S

I

•)

<,

>5

9

TABLE 2.1.—Correlation between mass and velocity for

Super-Schmidt and small-camera meteors (In the

table for small-camera meteors only those were

included for which log «• was determined.)

Super-Schmidt Meteor

Mean v ± s.d.

(Ws)

13-5 ± 0.3

17-7 ± 0.2

22.U ± 0.2

27.U -t 0.2

31.9 ± 0.2

36.7 ± 0.2

U2.8 ± 0.2

U7.3 ± o.u

53-0 t 0.5

58.2 ± o.u

61.8 ± 0.3

67.7 ± 0.2

71-U ± 0.3

All

Mean m ± s.d.

(8)

1.U2 ± 0.15

2.65 ± 0.71

0.88 ± O.lU

0.70 ± 0.20

0.51 ± 0.09

0.U8 ± 0.15

0.09 t 0.01

0.2U -t 0.08

0.10 t 0.03

0.09 i 0.03

0.13 ± 0.05

0.27 ± 0.23

0.10 -t 0.0U

0.80 ± 0.11

No.

obs.

9

57

65

63

U8

39

3^*

11*

9

18

25

22

8

U ll

Mean

(

16.2

25-9

3U.U

1*5-5

55-5

61.6

All

cm

±

±

±

-t

±

±

±

0

0

0

2

1

0

s.d.

• 9

.6

• 5

. 1

• 9

•9

Mean

125

176

97

12

U7

7

110

(g)

± U5

t 85

-t Ul

t 5

i 25

i U

t 31

s.d. No

obs

9

27

36

U

5

7

88

Small-Camera Meteors

TABLE 2.2.—Correlation of velocity, mass, and brightness

with the zenith angle for Super-Schmidt meteors for

which a was determined

ge of cos Z.

0.1 - 0.2

0.2 - 0.3

0.3 - o.u

O.U - 0.5

0.5 - 0.6

0.6 - 0.7

0.7 - 0.8

0.8 - 0.9

0.9 - 1.0

, Mean cos Z,

O.lU

0.25

O.35

0.U6

O.55

O.65

0.75

0.8U

0.97

, Mean v

(W

U8.7±

>*3-3 ±

U0.3 ±

UU.5 ±

33-7 ±

33-8 ±

32-0 ±

31.7 ±

33-7 ±

± s.d.

s)

1U.5

7-1*

3-3

3-1*

2.U

1.7

1.6

1-9

1.8

Mean 1

0.5

1-3

0 . 6

0 . 8

l.U

1.2

O.U

0.6

1.1

1 ± s.d.

( g )

± 0.5

± 0.7

± 0.3

± 0.2

± 0.7

± 0.5

± 0.1

* 0.2

± 0.3

Mean e

-O.29

-O.lU

-O.36

-0.21

-O.U3

-O.UO

-0-53

-0.52

-0.28

„ * s-d-

± 0.03

± 0.15

± 0.09

± 0.10

± 0.09

± 0.06

± 0.05

± 0.06

-t 0.09

No.

3

9

28

32

29

76

70

61

UO
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 101

TABLE 3

Identification of coefficients for tables' 3.1 through 3.17. c0 to c5 are coefficients of an equation of the type:

log P=co+^E?,Ci(Xi—Xi), where k=2, 3, 4, 5 and Zi=log cos ZR, ia=log vw, xa=log mw, x4=log <r, z5=x, zi= —0.2,

!=/

x2=6.4771, 33= -0.5229, xt= -11.20, i6=0.25.

TABLE 3.1.—Solutions for the totality of Super-Schmidt

meteors

TABLE 3.2.—All Super-Schmidt meteors (D meteors

excluded)

c

o

c

l

C

2

c

0

c

l

C

2

C

3

c

o

°1

C

2

C

3

c

k

c

o

°x

C

2

°3

C

4

C

5

«B

-9.20 4 0.02

0.07 ± o. u

-2.97 ± 0.09

C*03)

-9.21 4 0.02

0.02 4 0.11

-3.59 ± 0.13

-0.25 ± 0.01*

(1*02)

-9.21 ± 0.02

0.05 ± 0.12

-3.1*9 ± 0.11*

-0.2U ± O.Ol*

0.13 ± 0.06

(387)

-9.22 4 0.02

0.15 4 0.12

-3.1*1* ± o.ll*

-0.22 4 O.Ol*

0.15 ± 0.06

0.16 t 0.06

(387)

TABLE 3.3.—

H

2.5

-9.16 ± 0.02

0.19 ± 0.11

-3-37 4 0.09

(1*02)

-9-17 4 0.02

O.ll* 4 O.U

-l*.O9 ± 0.12

-0.30 4 o.oi*

(1*02)

-9.17 ± 0.02

0.19 4 0.11

-l*.O2 4 0.13

-0.29 4 o.oi*

0.09 4 0.06

(387)

-9.17 * 0.02

0.23 4 0.12

-I*.OO 4 0.13

-0.28 ±0.01*

0.09 4 0.06

0.07 * 0.05

(387)

Svoradic Si

"ML

-8.U3 4 0.02

1.01 4 0.11

-2.1*1 4 0.09

(1*12)

-8.1*2 4 0.02

1.10 4 0.09

-1.1*3 ± 0.11

0.1*1 4 0.03

(<*11)

-8.1*1 4 0.01

1.13 4 0.10

-1.50 4 0.12

0.39 ± 0.03

-0.19 4 0.06

(396)

-8.1*1 4 0.01

1.09 4 0.10

-1.52 ± 0.12

O.38 4 0.03

-0.19 4 0.06

-O.O7 4 0.05

(396)

"E

-8.07 ± 0.02

1.36 4 0.10

-2.23 4 0.09

(1*11)

-8.05 4 0.01

1.1*2'4 0.09

-1.17 4 0.11

0.1*5 4 0.03

(1*09)

-8.05 4 0.01

1.1*6 4 0.09

-1.21 ± 0.11

0.1*1* 4 0.03

-0.15 4 0.05

(394)

-8.05 4 0.01

I.36 ± 0.09

-1.25 4 0.11

0.1*2 4 0.03

-0.16 4 0.05

-0.16 4 O.Ol*

(394)

iver-Schmidt meteors

«ML

0

1

2

0

1

2

3

0

1

2

3

4

0

1

2

3

4

5

-9-19 ± 0.02

0.07 4 0.14

-3.01 4 0.11

(282)

-9.20 4 0.02

0.04 4 0.14

-3-71 t 0.16

-0.27 ± 0.05

(281)

-9.20 4 0.02

0.01 4 0.15

-3.62 4 0.18

-0.26 4 0.05

0.11 4 0.09

(271)

-9.20 4 0-02

0.19 4 0.15

-3-52 * 0.17

-0.22 4 0.05

0.10 ± 0.09

0.28 4 0.07

(271)

-9.14 4

0.24 4

-3.41 4

0.02

0.14

0.11

(283)

-9-15 *

0.13 4

-4.16 4

-0.30 4

0.02

0.13

0.15

0.05

(283)

-9.16 4

0.20 4

-4.U 4

-0.29 4

0.05 4

0.02

0.14

0.17

0.05

0.09

(273)

-9.16 4

0.31 4

-4.07 4

-0.27 t

0.03 4

0.13 4

0.02

0.15

0.17

0.05

0.09

0.06

(273)

-8.43

0.82

-2.51

4 0.02

4 0.12

4 0.10

(289)

-8.42

0.95

-1.58

0.36

4 0.02

4 0.10

4 0.13

4 0.04

(289)

-8.40

0.96

-1.82

0.34

-0.39

4 0.02

4 0.10

4 0.13

4 0.04

4 0.07

(279)

-8.40

1.02

-1.79

O.36

-0.40

0.09

4 0.02

4 0.11

4 0.13

4 0.04

4 0.07

4 0.05

(279)

-8.O84

1.13 4

-2-35 4

0.02

0.12

0.09

(288)

-8.06 4

1.24 4

-1.35 *

0.40 4

0.02

0.10

0.13

0.04

(287)

-8.05 4

1.27 4

-1.48 4

0.39 *

-0.28 4

0.02

0.10

0.13

0.04

0.07

(277)

-8.05 4

1.24 4

-1.50 *

0-39 *

-0.28 4

-0.04 4

0.02

0.11

0.13

0.04

0.07

0.05

(277)

-9.22 4 0.02

0.04 4 0.12

-2.88 4 0.09

(38S)

-9.23 4 0.02

-0.00 4 0.11

-3.48 4 0.13

-0.24 4 0.04

(381)

-9.23 4 0.02

0.03 -t 0.12

-3.40 4 0.14

-0.24 4 0.04

O.U 4 0.07

(367)

-9.23 ± 0.02

0.10 4 0.12

-3-37 4 0.14

-0.22 4 0.04

0.12 4 0.07

0.13 4 0.06

(367)

"2.5

-9.18 4 0.02

0.16 4 0.12

-3-29 -t 0.09

(381)

-9.18 4 0.02

0.12 4 O.U

-3-99 4 0.12

-0.29 4 0.04

(381)

-9.I8 4 0.02

0.16 4 0.12

-3-94 4 0.13

-0.28 4 0.04

0.06 4 0.07

(367)

-9.1fi 4 0.02

0.19 4 0.12

-3-93 ± 0.13

-O.28 4 0.04

0.06 4 0.07

0.03 4 0.05

(367)

«ML

-8.43 4 0.02

1.01 4 O.U

-2.35 4 0.09

(390)

-8.42 4 0.02

1.09 4 0.09

-1-35 ± O.U

0.41 4 0.03

(389)

-8.42 4 0.01

1.12 4 0.10

-1.1*2 4 0.12

0.4O 4 0.03

-0.20 4 O.OC

(375)

-8.42 4 0.01

1.07 ± 0.10

-1.44 4 0.12

O.39 4 0.03

-0.81 4 O.OC

-0.10 4 0.05

(375)

-8.08 4 0.02

1.34 4 O.U

-2.15 4 0.09

(389)

-8.07 4 0.01

1.40 4 0.09

-1.08 4 0.11

0.45 4 0.03

(387)

-8.06 4 0.01

1.44 4 0.09

-1.12 4 0.11

0.44 4 0.03

-0.19 4 0.05

(373)

-8.06 4 0.01

1.33 * 0.09

-1.17 * 0.11

0.42 4 0.03

-0.20 4 0.05

-0.19 4 0.04

(373)

TABLE 3.4—Sporadic Super-Schmidt meteors (D meteors

excluded)

-9-21 4 0.02

0.01 4 0.15

-2.92 4 0.11

(261)

-9.22 4 0.02

-0.10 4 0.14

-3.6I 4 0.17

-0.26 4 0.05

(260)

-9.22 4 0.02

-0.04 4 0.16

-3.54 4 0.18

-0.25 4 0.05

0.06 4 0.10

(251)

-9.22 4 0.02

0.10 4 0.16

-3.48 4 0.18

-0.22 4 0.05

0.04 4 0.10

0.26 4 0.08

(251)

"2.5

-9.16 4 0.02

0.18 4 0.15

-3.32 * o.u

(262)

-9.17 ± o.oe

0.08 4 0.14

-4.06 4 0.16

-0.29 4 0.05

(262)

-9.17 ± 0.02

0.15 4 0.15

-4.04 4 0.17

-0.28 4 0.05

-0.02 4 0.10

(253)

-9.17 4 0.02

0.23 4 0.16

-4.02 4 0.17

-0.27 ± 0.05

-0.04 4 0.10

0.10 4 0.07

(253)

"ML

-8.1*3 4 0.02

0.79 4 0.12

-2.45 4 o.io

(267)

-8.42 4 0.02

0.92 4 0.11

-I..50 4 0.13

O.37 4 0.04

(267)

-8.41 4 0.02

0.91 4 0.10

-1.77 * 0.13

O.35 4 0.04

-0.48 4 0.07

(258)

-8.41 t 0.02

O.96 4 0.11

-I.76 ± 0.13

O.30 4 0.04

-O.5O 4 0.08

0.08 4 0.05

(258)

-8.09 4 0.02

1.08 4 0.12

-2.27 4 0.09

(266)

-8.07 4 0.02

1.18 4 0.10

-1.26 4 0.12

0.40 4 0.04

(265)

-8.06 t 0.01

1.19 + 0.10

-1.45 4 0.12

0.40 4 0.04

-0.40 4 0.07

(256)

S.Od t 0.01

1.15 ± 0.10

-1.46 4 0.12

0.39 f 0.04

-O.39 ± O.C7

-0.06 -t 0.05

(25O
102 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 3.5.—Sporadic Super-Schmidt meteors (A and

S excluded)

-9-24 4 0.02

-0.03 ± 0.14

-2.93 ± 0.11

(253)

-9.24 4 0.02

-0.13 * 0.13

-3-60 4 0.15

-0.26 -t 0.05

(252)

-9.25 i 0.02

-0.08 4 0.14

-3.58 * 0.17

-0.25 t 0.05

0.00 i 0.09

(2<*3)

-9.24 4 0.02

0.12 4 0.15

-3.48 -t 0.16

-0.21 4 0.05

-0.02 t O.09

0.29 -t 0.07

(243)

H

2.5

-9.18 t 0.02

0.14 i 0.14

-3-36 -t 0.11

(254)

-9-19 ± 0.02

0.04 ± 0.13

-4.10 ± 0.15

-0.29 ± 0.04

(254)

-9-19 ± 0.02

0.10 ± 0.14

-4.10 4 0.16

-0.29 4 0.04

-0.05 ± 0.09

(245)

-9.19 ± 0.02

0.22 ± 0.15

-4.07 * 0.16

-0.26 i O.05

-0.07 4 0.09

0.14 ± 0.06

(245)

-8.43 ± 0.02

0.82 4 0.12

-2.51 ± 0.10

(260)

-8.42 4 0.02

0.95 -t 0.11

-1.57 ± 0.14

O.37 4 0.04

(260)

-8.41 4 0.02

0.94 4 0.11

-1.80 ± 0.14

O.35 ± 0.04

-0.43 4 0.07

(251)

-8.41 4 0.02

1.00 t 0.13

-I.78 ± 0.14

O.36 i 0.04

-0.44 ± 0.08

0.09 ± 0.05

(251)

TABLE 3.6.—Sporadic Super-Schmidt meteors (A, 8

and D excluded)

h

 H2.5 "XL «F.

-8.09 ± 0.02

1.10 4 0.12

-2.36 ± 0.10

(259)

-8.07 ± 0.02

1.20 * 0.10

-I.34 4 0.13

0.41 -t 0.04

(258)

-8.06 ± 0.02

1.22 -t 0.10

-1.49 ± 0.13

0.40 ± 0.04

-0.35 ± 0.07

(240)

-8.06 4 0.02

1.39 t 0.11

-1.50 4 0.13

0.39 4 0.04

-0.35 i 0.07

-0.04 ± 0.05

(249)

o

0

1

2

0

1

2

3

0

1

2

3

4

-9-25

-0.09

-2.88

4 0.02

4 0.14

4 0.10

(240)

-9-26

-0.19

-3-56

-0.26

4 0.02

4 0.13

4 0.15

4 0.05

(239)

-9.26

-0.16

-3-56

-0.25

-0.05

4 0.02

4 0.15

4 0.17

4 0.05

4 0.10

(230)

-9-26

-0.00

-3-'t9

-0.21

-0.07

0.26

± 0.02

± 0.15

4 0.17

t 0.05

i 0.10

4. 0.07

(230)

-9.20

0.09

-3-31

4 0.02

4 0.14

4 0.10

(241)

-9.21

-0.01

-4.04

-0.28

4 0.02

4 0.13

4 0.15

4 0.04

(241)

-9.21

0.03

-4.08

-0.28

-0.12

4 0.02

4 0.14

4 0.16

4 0.04

4 0.10

(232)

-9.21

0.11

-4.06

-0.27

-0.14

0.10

4 0.02

t 0.15

t 0.16

± 0.05

4 0.10

4 0.06

(232)

-8.44 4 0.02

0.75 4 0.13

-2.47 4 0.10

(246)

-8.43 4 0.02

0.89 4 0.11

-1.51 4 0.13

O.37 4 0.04

(246)

-8.42 4 0.02

0.86 4 0.11

-1.79 4 0.14

O.35 4 0.04

-0.51 4 0.08

(237)

-8.42 * 0.02

0.92 4 0.11

-1.77 t 0.14

O.36 4 0.04

-O.53 4 0.08

0.08 4. 0.05

(237)

-d.10 4 0.02

1-03 4 0.12

-2-30 4 0.10

(245)

-8.O8 4 0.02

1.12 4 0.10

-1.28 ± 0.13

0.40 4 0.04

(244)

-8.07 4 0.01

1.13 4 0.10

-1.47 4 0.12

0.40 4 0.03

-0.44 4 0.07

(235)

-8.07 4 0.01

1.08 4 0.10

-1.49 4 0.12

0.39 4 0.04

-0.43 4 0.07

-0.06 + 0.05

(235)

TABLE 3.7.—Sporadic Super-Schmidt meteors (A, S,

and D excluded) with log <r <C. — 11.4

TABLE 3.8.—Sporadic Super-Schmidt meteors (A, S,

and D excluded) with —11.4 <log <r < — 11.0

D

1

2

0

1

2

0

1

2

3

4

0

1

2

3

4

5

"E

-9-42 4 0.09

0.03 4 0.40

-1.75 4 O.39

(35)

-9.28 4 0.09

-0.10 4 0.34

-3.07 4 0.48

-O.34 4 0.09

(35)

-9.66 4 0.11

0.04 4 0.27

-3.O6 4 O.38

-O.33 4 0.07

-1.08 4 0.26

(35)

-9.64 4 0.12

0.11 4 O.32

-3.04 4 O.39

-0.31 4 0.08

-1.04 4 0.23

0.03 4 0.17

(35)

H

2.5

-9.40 4 0.10

0.11 4 0.51

-2.05 4 0.43

(3<0

-9-25 4 0.10

-0.12 4 0.44

-3.42 4 O.54

-0.35 4 0.10

(3<0

-9-64 4 0.14

0.05 4 O.38

-3.41 4 0.46

-O.34 4 0.09

-1.10 4 0.31

(31*)

-9-66 4 0.15

-0.06 4 0.46

-3.43 4 O.47

-0.36 4 0.10

-1.15 4 O.33

-0.09 4 0.21

(34)

"ML

-8.03 4

O.63 4

-3-21 4

(37)

-8.21 4

O.87 4

-1.47 4

0.45 4

(37)

-8.51 4

0.94 4

-1.42 4

0.46 4

-0.85 4

(37)

^8.48 4

1.02 4

-1-39 4

0.48 4

-0.79 4

0.10 4

(37)

0.10

0.37

0.41

0.08

0.27

0.43

0.08

0.11

0.24

O.38

0.07

0.25

0.12

0.27

O.38

0.08

0.27

0.16

-7.64 4

1-03 4

-3.46 ±

(36)

-7-74 4

1.13 4

-2-43 4

0.24 4

(36)

-8.08 4

1.22 4

-1.89 ±

O.36 4

-O.83 4

(36)

-8.11 4

1.12 4

-1-95 4

O.33 4

-0.90 4

-0.12 4

(3<q

0.07

0.25

0.28

0.07

0.24

0.47

C.09

0.12

0.21

0.45

O.OO

0.26

0.13

0.24

0.45

0.10

0.27

0.14

-9.29 4 0.02

-0.01 4 0.18

-2.92 4 0.13

(150)

-9.30 4 0.02

-0.09 4 0.18

-3-32 4 0.21

-0.15 4 0.06

(150)

-9«3O 4 0.02

-0.04 4 0.18

-3-24 4 0.21

-0.15 4 0.06

0.57 4 O.23

(150)

-9-29 4 0.02

0.05 4 0.18

-3.19 4 0.21

-0.11 4 0.06

O.52 4 O.23

0.27 4 0.09

(150)

-9.23 4 0.02

0.19 4 0.18

-3-33 4 0.13

(152)

-9-24 4 0.02

0.08 4 0.18

-3.88 4 0.20

-0.20 4 0.06

(152)

-9.24 4 0.02

0.11 4 0.18

-3-81 4 0.20

-0.20 ± 0.06

O.39 4 O.23

(152)

-9-23 4 0.02

0.16 4 0.18

-3-79 4 0.20

-0.18 4 0.06

O.36 4 O.23

0.15 4 0.09

(152)

-8.47 4 0.02

0.72 4 0.15

-2.62 4 0.12

-8.45 4 0.02

0.90 4 0.13

-I.67 4 0.16

0.35 4 0.05

(154)

-8.45 4 0.02

0.89 4 0.13

-1.70 4 0.17

0.35 4 0.05

-0.17 4 0.19

(154)

-8.45 4 0.02

0.91 4 0.14

-I.69 4 0.17

O.36 4 0.05

-0.19 4 0.19

0.08 4 0.08

(154)

-8.13 4 o.oe

0.97 4 0.16

-2.45 4 0.13

(153)

-8.11 4 0.02

1.18 4 0.12

-1.29 4 0.15

0.43 4 o.ofc

(153)

-8.10 4 0.02

1.17 4 0.12

-1.31 4 0.15

0.1*3 4 O.<*

-0.08 ± 0.18

(153)

-8.11 4 o.oe

1.15 4 0.12

-1.32 4 0.15

0.1*2 4 0.04

-0.06 4 0.18

-0.11 4 0.07

(153)
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 103

TABLE 3.9.—Sporadic Super-Schmidt meteors (A, S,

and D excluded), with log a >—11.0

"B H

2.5 V

0

1

2

0

1

2

3

0

1

2

3

14.

0

1

2

3

4

-9-25

-0.01

-3.46

4

±

4

(1*5)

-9.24

-0.13

-4.26

-O.38

t

4

4

4

C*5)

-9.24

-0.09

-4.24

-O.36

-0.03

(1

-9.22

0.01

-4.21

-O.35

-0.09

0.13

±

-t

4

4

±

*5)

4

±

•t

±

±

(45)

0.06

0.34

0.30

0.06

0.31

0.38

0.13

0.21

0.33

0.40

0.13

O.58

0.21

0.35

0.40

0.13

0.59

0.15

-9.22

0

-3

.17

.89

±

±

4

(46)

-9.22

0

-4

-0

-9

0

-4

-0

-0

-9

0

-4

-0

-0

•09

.66

.36

4

4

4

4

(46)

.18

•13

• 59

-33

.14

i

4

4

4

±

(46)

.17

• 15

• 59

• 32

.16

0.01

4

±

4

4

±

4

(46)

0.06

0.29

0.27

0.05

0.27

0-35

0.12

0.19

0.27

O.36

0.12

0.51

0.19

0.32

0.37

0.12

O.54

0.11

-8.56

0.80

-2-79

i

±

(46)

-8.56

0.82

-2-55

0.11

±

i

i

±

(46)

-8.24

0.80

-2-37

0.14

-0.92

±

i

t

±

±

(46)

-8.21

0.95

-2.36

0.16

-1.04

0.10

±

i

4

±

4

i

(1*6)

0.05

0.26

0.25

0.05

0.27

0.35

0.12

0.18

0.27

0-35

0.12

0-50

0.19

0.31

O.35

0.12

0-52

0.11

-8.17

0.93

-2-39

(I

-8.17

0.99

-3.-93

0.21

i

±

4

'••'-')

4

.

4

4

(46)

-7-90

1.01

-1-75

0.26

-O.78

±

4

4

4

±

(46)

-7-93

0.88

-1.76

0.25

-O.67

-0.09

±

•i

4

4

±

4

(46)

0.05

0.24

0.22

0.04

0.23

0.30

0.10

0.15

0.22

0.29

0.10

0.41

0.16

0.26

0.29

0.10

0.43

0.09

TABLE 3.10.—Sporadic Super-Schmidt meteors (A, 8,

and D excluded) with | x | <0.t

"ML

=0

=1

C2

=0

cl

Z2

=3

co

cl

=2

C3

24

CO

C2

=3

C4

C5

-9.35 ± 0.03

0.29 ± 0.21

-2.86 ± 0.15

(117)

-9-33 * 0.03

-0.01 ± 0.21

-3.60 ± 0.21

-0.29 ± 0.06

(117)

-9.33 ± 0.03

0.02 ± 0.20

-3-39 ± O.23

-O.27 ± 0.06

0.25 ± 0.15

(116)

-9.17 ± O.06

-O.05 ± 0.20

-3-33 ± 0.22

-0.26 ± 0.06

0.30 ± 0.14

O.78 i 0.27

(116)

-9-28 ±

0.49 ±

-3-25 ±

0.03

0.22

0.15

(118)

-9.25 ±

0.16 ±

-4.03 ±

-O.32 ±

0.03

0.20

0.20

0.06

(118)

-9.25 ±

0.18 ±

-3.86 ±

-0.30 ±

0.22 ±

0.03

0.20

0.22

0.06

0.15

(117)

-9.14 ±

0.14 ±

-3-82 ±

-0.29 ±

O.25 ±

O.51 ±

0.06

0.20

0.22

0.06

0.15

0.27

(117)

-8.43 ±

0.74 ±

-2.38 ±

0.03

0.19

0.15

(120)

-8.46 i

1.08 ±

-1-31* ±

0,42 ±

0.02

0.16

0.19

0.06

(120)

-8.46 ±

1.02 *

-1-76 ±

0.37 ±

-0.59 ±

0.02

0.15

0.20

0.05

0.13

(119)

-8.36 i

0.99 ±

-1-73 i

0.38 ±

-O.56 ±

0.46 ±

0.06

0.15

0.20

0.05

0.13

0.24

(119)

-8.04

0.91

-2.16

± 0.03

t 0.17

± 0.14

(119)

-8.07

1.27

-I.07

0.44

± 0.02

± 0.14

± 0.16

* 0.05

(119)

-8.07

1.22

-1.36

0.41

-0.40

± 0.02

± 0.13

± 0.17

± 0.04

± 0.11

(118)

-8.06

1.22

-1-35

0.41

-0.40

0.06

± 0.05

± 0.13

* 0.17

± 0.05

± 0.11

± 0.21

(118)

TABLE 3.11.—Sporadic Super-Schmidt meteors (A, S,

and D excluded )with % >0.2

TABLE 3.12.—Sporadic Super-Schmidt meteors (A, S,

and D excluded) with % >04

-9.16 4 0.03

-0.17 4 0.21

-3.O6 4 0.15

(109)

-9.17 ± 0.03

-0.18 ± 0.21

-3-32 ± 0.23

-0.11 4 0.07

(109)

-9-15 4 0.03

-0.23 ± 0.21

-3.48 ± O.23

-0.10 4 0.07

-0.37 * 0.13

(109)

-9.18 ± 0.04

-0.15 ± 0.22

-3-1*5 ± 0.23

-0.08 4 0.07

-O.38 ± 0.13

0.I3 ± 0.13

(109)

H

2.5

-9.13 ± 0.03

0.05 4 0.21

-3.45 4 0.15

(110)

-9.15 ± 0.03

0.03 ± 0.20

-3.85 4 0.22

-0.16 ± 0.07

(no)

-9.12 ± 0.03

-0.10 ± 0.20

-4.05 ± 0.22

-0.16 ± 0.06

-0.45 4 0.12

(110)

-9.11 ± 0.04

-0.15 4 0.22

-4.06 4 0.22

-0.16 i 0.07

-0.44 ± 0.I3

-0.05 4 0.10

(no)

»ML

-8.44 ± 0.03

O.83 ± 0.21

-2.46 4 0.15

(113)

-8.40 4 0.03

0.88 ± 0.18

-1.54 ± 0.20

0.37 4 0.06

(113)

-8.38 4 0.03

O.78 4 0.16

-1.79 ± 0.19

O.38 4 0.06

-0.54 4 0.10

(113)

-8.37 4 0.03

0.75 4 0.18

-1.79 4 0.19

O.38 4 0.06

-0.53 4 0.11

-0.03 4 0.08

(U3)

-8.15 4 0.03

1.06 4 0.18

-2.38 4 0.14

(112)

-8.12 4 0.03

1.10 4 0.16

-1.47 ± 0.20

O.35 4 0.06

(112)

-8.09 4 0.02

1.00 4 0.15

-1.57 4 0.19

0.40 4 0.06

-0.48 4 0.10

(112)

-8.08 4 0.03

O.96 4 0.17

-1.58 4 o.i "

0.40 4 0.OT

-0.47 4 0.10

-0.04 4 0.08

(112)

-9.09 4

0.18 4

-2.98 4

(50)

-9-09 4

0.18 4

-3.07 4

-0.03 4

(50)

-9.02 4

0.19 i

-3-09 4

0.05 4

-0.52 4

(50)

-8.99 4

0.14 4

-3-13 4

0.05 4

-O.54 *

-0.09 4

(50)

0.05

0.28

0.20

0.05

0.29

0.40

0.12

0.05

0.27

0.37

0.12

0.13

0.08

0.29

O.38

0.12

0.18

0.17

-9-09

0.29

-3.46

4

4

4

(51)

-9.11

0.24

-3.86

-0.14

4

4

i

4

(51)

-9.05

0.19

-3-85

-0.06

-0.48

4

4

4

4

4

(51)

-9.01

O.OO

-3.87

-0.07

-O.45

-0.11

4

4

4

±

4

±

(51)

0.05

0.28

0.21

0.05

0.28

0.40

0.12

0.05

0.26

0.38

0.12

0.18

0.07

0.29

O.38

0.12

0.18

C.ll

-8.47 4

O.78 4

-2-55 *

(52)

-8.43 4

0.87 i

-1.77 t

0.26 4

(52)

-8.36 4

0.84 4

-I.78 4

0.37 4

-0.54 ±

(52)

-8.33 4

0.73 4

-1.80 4

O.36 i

-0.51 4

-0.10 4

(52)

0.05

0.28

0.21

0.05

0.27

O.30

0.12

0.05

0.24

O.35

0.11

0.16

0.06

0.27

O.35

0.11

0.16

0.11

-8.18 4

0.99 4

-2.42 4

(52)

-8.12 4

1.10 4

-1.43 4

0.3C 4

(52)

-8.0t 4

1.08 4

-1.43 4

0.44 ±

-0.50 4

(52)

-8.02 *

0.96 4

-1.46 4

0.43 4

-0.47 f

-0.10 i

(52)

0.05

0.27

0.20

0.05

0.25

O.37

0.11

O.05

0.23

O.33

0.11

0.15

0.06

0.25

0.33

0.11

0.15

0.10
104 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 3.13.—Super-Schmidt meteors with abrupt

beginning

o

1

2

0

1

2

0

1

2

3

k

0

1

2

3

4

5

-8.91

0.75

-3-95

B

± 0.06

± O.33

t 0.29

(26)

-8.92

O.Vl*

-5.16

-O.63

i 0.05

± 0.27

± 0.39

± 0.16

(26)

-8.88

0.42

-5.14

-O.69

-0.08

± 0.05

± 0.27

± 0.44

± 0.17

± 0.19

(24)

-8.88

0.41

-5-22

-O.70

-0.12

-0.14

± 0.05

± O.28

± 0.46

± 0.17

± 0.20

± 0.20

(24)

2

-8.91

0.86

-4.17

.5

t

±

4

(26)

-8.92

0.51*

-5.40

-O.65

±

t

±

±

(26)

-8.87

0.55

-5A7

-0.73

-0.15

±

±

±

-t

(24)

-8.87

0.52

-5.56

-0.74

-0.20

-0.17

i

±

±

4

t

(24)

0.06

O.33

O.30

0.05

0.27

0.39

0.16

0.05

0.27

0.1*3

0.17

0.18

O.05

O.27

0.45

0.17

0.19

0.20

-8.50

I.36

-3.11*

ML

±

±

±

(26)

-8.49

1.1*9

-2.63

0.27

-t

±

±

±

(26)

-8.38

1-55

-2.96

0.10

-O.45

±

-fc

±

±

±

(24)

-8.38

1.54

-2.98

0.09

-0.U6

-0.03

±

i

±

±

±

±

(24)

0.06

0.33

0.30

0.06

O.3I1

0.1*9

0.20

0.05

0.28

0.44

0.17

0.19

0.06

0.29

0.1*7

0.18

0.20

0.21

-8.00

1.78

-2.63

i

i

i

(26)

-8.00

1.78

-2.63

0.00

1

t

±

±

(26)

-7.95

1.79

-2.71

-0.09

-0.18

i

i

±

i

±

(24)

-7-95

1.76

-2.81

-0.10

-0.23

-0.17

•fc

i

±

±

±

±

(24)

o.o4

0.23

0.20

0.0"!

0.24

O.3I*

0.11*

0.01*

0.22

0.35

0.13

0.15

0.04

0.22

O.36

0.13

0.15

0.16

TABLE 3.14.—Sporadic Super-Schmidt meteors with Q

<6 a.u.

«ML

0

1

2

0

1

2

0

1

2

3

If

0

1

2

3

1*

5

-9-16

0.20

-3.20

i

±

0.04

0.19

0.24

(164)

-9.18

O.05

-3-77

-O.19

t

±

-t

±

0.04

0.19

0.3I

0.08

(163)

-9.21

0.28

-3-25

-0.10

0.59

±

-fc

-fc

t

•fc

0.04

0.20

O.33

0.08

0.13

(157)

-9-20

0.44

-3-10

-0.06

0.57

0.24

fc

i

t

•fc

•fc

±

0.04

0.21

0.33

0.08

0.13

0.10

(157)

-9.10

0.31

-3.49

i

t

t

0.04

0.18

0.2J

(164)

-9.14

0.13

-4.27

-0.28

±

-t

±

±

0.04

0.18

0.2Q

0.07

(164)

-9.16

0.35

-3.83

-0.20

0.50

t

±

i

•t

±

0.04

0.19

0.31

0.07

0.13

(158)

-9.15

0.4H

-3-72

-0.17

0.48

0.18

t

*

•fc

i

i

i

O.()4

0.20

0.32

0.07

0.13

0.10

(158)

-8.43

0.80

-2-59

i

ft

0.03

0.15

0.19

(165)

-8.38

1.06

-1.46

0.40

±

i

-t

±

0.03

0.13

0.P1

0.05

(165)

-8.39

1.18

-1.57

0.40

-0.08

±

±

i

±

I

0.03

0.15

0.24

0.05

0.10

(159)

-8.39

1.25

-1.51

0.42

-0.09

0.10

t

t

t

i

i

±

0.03

0.15

O.?4

0.05

0.10

0.08

(159)

-8.04 ± 0.03

0.99 ± 0.16

-2.12 i 0.20

(166)

-7-99 ± O.03

1.26 ± 0.13

-0.84 ± 0.21

0.48 ± 0.05

(165)

-8.00 i 0.03

1.39 ± 0.1k

-0.88 ± 0.2l»

0.50 ± 0.05

-0.02 ± 0.10

(159)

-8.00 t O.03

1-39 * 0.15

-0.88 i 0.2U

0.50 * 0.05

-0.02 t 0.10

-0.01 ± 0.07

(159)

TABLE 3.15.—Sporadic Super-Schmidt meteors urilh Q TABLE 3.16.—All small-camera meteors

0

1

0

1

2

3

0

1

2

3

4

0

1

2

3

4

5

-9-37

0.10

-2.29

3

±

±

i

(US

-9-35

0.11

-3-13

-0.30

±

±

i

0.04

0.20

0.17

>)

0.04

0.18

O.23

0.06

(118)

-9.34

0.10

-3-24

-0.30

-O.32

i

±

±

t

±

0.04

0.18

0.23

0.06

0.10

(114)

-9-33

0.20

-3-21

-0.26

-O.3O

0.22

±

±

i

i

±

±

0.03

0.18

0.22

0.06

0.10

0.09

(H4)

-9.31

0.32

-2.76

2,

-fc

±

±

• 5

0.04

0.20

0.17

(119)

-9.29

0.31

-3.54

-0.27

±

±

±

±

0.04

0.19

0.24

0.06

(119)

-9.28

0.24

-3.67

-0.28

-O.35

±

i

±

±

±

0.04

0.18

O.23

0.06

0.10

(115)

-9.28

0.29

-3.66

-0.27

-O.36

0.06

-t

±

±

±

±

0.04

0.20

0.23

0.06

0.10

0.08

(115)

-8.1*9

0.91

-2.26

±

•fc

i

0.04

0.19

0.19

(124)

-8.52

0.96

-1.18

O.38

±

±

i

±

0.04

0.17

0.24

0.06

(124)

-8.50

0.92

-1.43

O.38

-O.67

±

1

-fc

±

±

0.03

0.14

0.21

0.05

0.09

(120)

-8.50

O.96

-1.42

0-39

-0.68

0.07

±

±

±

±

±

±

0.03

0.15

0.21

0.05

0.09

0.07

(120)

-8.11

1.31

-2.26

•E

± 0.04

± 0.17

± 0.17

(122)

-8.14

1-33

-1.27

O.34

± 0.04

± 0.15

± 0.23

± 0.06

(122)

-8.12

1.29

-I.36

O.37

-0.48

± 0.03

± 0.14

± 0.21

± 0.06

± 0.09

(118)

-8.13

1.25

-1-37

O.35

-O.47

-0.07

± o.o4

± 0.14

± 0.21

± 0.06

± 0.09

± 0.06

(118)

"B "ML

0

1

2

0

1

2

3

0

1

2

3

1*

0

1

2

3

4

5

-8.79 t 0.04

0.26 ± 0.22

-3-28 ± 0.18

(209)

-8.73 ± 0.08

0.39 ± 0.26

-3.44 ± 0.22

-0.05 ± 0.04

(205)

-8.81 ± 0.15

0.14 ± 0.51

-4.41 ± O.50

-0.12 ± 0.09

-0.57 ± 0.25

(87)

-8.69 t 0.17

0.30 ± 0.46

-4.83 ± 0.48

-0.10 ± 0.09

-0.79 ± 0.24

1.13 4 0.28

(50)

-7.75 i 0.05

0.94 ± 0.23

-2.99 ± 0.22

(210)

-8.57 ± 0.08

1.77 ± 0.26

-1.48 ± 0.22

0.48 ± 0.04

(206)

-8.42 ± 0.12

1.24 ± O.38

-2.60 -t O.39

0.31 ± 0.07

-O.93 ± 0.19

(88)

-8.25 -t 0.17

1.20 ± 0.43

-2.40 ± 0.47

0.29 ± 0.09

-0.94 ± 0.24

0.24 ± 0.30

(51)

-7-33 ± 0.05

0.97 ± 0.29

-3.05 ± 0.24

(208)

-8.31 ± 0.08

1.90 ± 0.25

-1.17 ± O.23

O.58 ± 0.04

(204)

-8.13 ± 0.11

1.28 ± 0.35

-2.23 ± 0.37

0.41 ± 0.06

-0.99 ± 0.18

(86)

-8.04 ± 0.12

1.30 -t O.30

-1.86 ± 0.35

O.43 ± 0.06

-1.06 i 0.17

0.21 ± 0.21

(49)
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 105

TABLE 3.17.—Sporadic small-camera meteors

"B "ML «E

cQ -8.71 ± 0.06 -7.7U ± 0.07 -7-36 ± 0.07

c 1 0.U7 ± 0.32 0.72 ± O.38 0.70 ± 0.40

=2 -3-25 ± 0.25 -3.00 i 0.29 -3.07 ± 0.32

(88) (88) (88)

oQ -8.79 ± 0.14 -8.63 ± 0.13 -8.40 i 0.13

c1 0.95 ± 0.U3 1.90 ± O.39 1-97 ± 0.1*0

=2 -3-21 -t O.36 -1.21 -t 0.34 -0.92 ± O.35

c 0.02 ± 0.08 0.53 ± 0.07 O.63 ± 0.07

(84) (84) (81*)

Cg -8-9 9 ± 0.2 8 -8.69 ± 0.19 -8.36 -t 0.20

ex l.Olt ± 0.90 1.86 -t 0.57 1-74 t 0.59

c 2 -U.16 -t 0.75 -2.00 ± O.52 -I.87 ± O.56

c -0.01 ± 0.16 0.49 -t 0.11 0.55 ± 0.12

c^ -0.66 ± 0.37 -0.77 ± 0.26 -0.81 ± 0.27

(40) (41) (40)

cQ -8.79 ± 0.28 -8.60 ± 0.19 -8.23 ± 0.18

c± 0.50 -t O.78 2.13 ± 0.47 1.96 ± 0.45

c 2 -4.98 ± O.69 -1.79 ± 0.46 -I.70 ± 0.45

c -0.03 -t 0.15 0.48 i 0.10 0.54 ± 0.09

c^ -O.96 t O.34 -0.75 ± 0.23 -0.84 ± 0.21

c 5 I.50 ± O.39 -0.13 t O.3O 0.05 ± 0.28

(25) (26) (25)

TABLE 4.—Coefficients of the equation: log p= co+ Ci (log cos ZR+ 0.5) + c2 fio</ v ,

— 6.477) + c3 (logma + 0.523) + a (log a+11.20) +a(x—0.25) for four sets

of heights, from a critical evaluation of the solutions of table 3

h

 H2.5 "ML "E

Theory Observations Theory Observations Theory Observations Theory Observations

Hp 104.8 99-0 ± 0.3 104.3 98-5 ± 0.3 90.1 88.9 ± 0.2 83.3 84.5 ± 0.2

c -9.66 -9.23 ± 0.02 -9.62 -9.19 ± 0.02 -8.51 -8.41 ± 0.02 -1.9( -9.Of * 0.02

c 0 0.0 ± 0.1 0 0.1 ± 0.1 1 1.0 i 0.1 1 1.2 ± 0.1

c z* -5 -3-5 ± 0.15 -6 -4.0 ± 0.15 * -2 -1-7 ± 0.1 =, -2 -1.4 ± 0.1

c — -0.25 ± 0.05 ^ -0.28 + 0.05 i- O.37 ± 0.04 i 0.40 ± O.OU

c -1 0.0 ± 0.1 -1 0.0 ± 0.1 -1 -0.5 ± 0.1 -1 -0.4 ± 0.1

c 0.2 ± 0.1 0.1 ± 0.1 _ 0.0 ± 0.1 _ -0.1 ± 0.1

is the height corresponding to log D - cQ in the U.S. Standard Atmosphere 10c2.
106 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS *

TABLE 5.1.1.—Heights of the standard meteor when one parameter at a time is varied; all meteors, variable v0

Velocity

range

10-15

15-20

20-25

25O0

30-35

35-40

1*0-45

45-50

50-55

55-60

60-65

65-70

70-75

All

Mean

log v^

(km/s)

1.130

1.248

1.349

1.437

1.502

1.564

1.632

1.675

1.724

1.765

1.790

1.830

I.854

I.499

S.d.

±0.011

0.005

0.003

0.003

0.003

0.002

0.002

0.004

0.004

0.003

0.0O2

0.002

0.002

0.010

log p

(g/om3)

-7-66

- 8.37

- 8.82

- 9-22

- 9-35

- 9-37

-9-6 6

- 9-72

-10.22

-10.13

-10.29

-10.49

-10.63

- 9.28

Begii

S.d.

±0.07

0.05

0.05

0.04

0.04

0.05

0.05

0.12

0.06

0.10

0.05

0.05

0.10

0.04

mlng

Mean H

79.4

88.4

93.8

98.9

100.6

IOO.9

104.8

105.6

113.2

in.7

n4.2

117.7

L?0.2

99.7

Ho.

9

55

64

62

47

37

31

12

9

13

24

17

7

387

Mean

- 7.51

- 8.21

- 8.69

- 9-33

- 9-34

- 9.42

- 9-69

- 9-72

-10.29

-10.31

-10.42

-10.61

-10.76

- 9.24

S.d.

±0.09

0.05

0.05

0.04

0.05

0.05

0.05

0.13

0.06

0.10

0.06

0.07

0.08

0.04

2.5

Mean H

77-2

86.4

92.2

97-7

100.5

101.5

105.2

105.7

114.3

n4.c

116.5

119.9

122.4

99.2

Ho.

9

56

a

62

46

37

31

9

14

?4

15

7

387

log 0

-7-65

-8.05

-8.29

-8.39

-8.42

-8.42

-8.65

-8.58

-9.04

-8.77

-8.91

-8.95

-8.93

-8.4k

Maximum Light

E.d.

(S/CB3)

- 0.08

0.04

0.04

0.03

0.05

0.05

0.0*.

0.O9

0.O9

0.O5

0.06

0.07

0.12

0.02

Mean H

(km)

79-3

84.4

87.''

88.6

89.0

89.1

91.a

90.9

96.6

93-3

94.9

95.5

95.2

»9.5

t:o.

jbs.

9

56

64

"1

47

38

31

14

9

U

Sk

10

7

Mean

log p

-7.52

-7.75

-7.97

-8.02

-8.07

-8.02

-e.ao

-8.11

-8.55

-a.42

-fl.45

-8.:,i.

-B.«0

-a.07

S.d.

* 0.07

0.04

0.04

0.0}

0.04

0.04

0.04

0.09

0.06

0.06

o.or.

0.04

0.00

o.os

End

Mean H

77-4

80.6

83.k

84.1

84.6

84.0

86.2

85.2

90.6

89.O

89.2

90.5

91.2

84.7

No

9

55

6k

63

*7

38

31

Ik

9

16

2k

17

7

39k

TABLE 5.1.2.—Heights of the standard meteor wnen one parameter at a time is varied; all meteors, variable mc

Mass Mean

range log m^

0.01-0.05 -1-52

0.05-0.10 -1.15

0.10-0.20 -0.84

0.20-0.40 -0.55

0.40-0.80 -0.23

0.80-1.60 0.04

1.6 -5.0 O.37

5.0 -34 O.92

S.d.

(g)

±0.02

0.02

0.01

0.01

0.01

0.01

0.03

0.07

Mean

log p

-8.95

-9.03

-9.18

-9.23

-9-29

-9-32

-9-39

-9.52

Beginning

S.d.

±0.04

0.05

0.04

0.04

0.04

0.05

0.08

0.14

Mean H

95-5

96.4

98.4

99-0

100.0

100.2

101.1

102.8

No.

obs.

56

49

71

69

59

42

29

12

Mean

log p

(g/car)

-8.88

-8.96

-9.10

-9-18

-9.28

-9-30

-9.41

-9.52

S.d.

(g/c- 3:

±0.04

0.05

0.04

0.04

0.04

0.05

0.07

0.12

2.5

Mean H

94.5

95-5

97.4

98.4

99-7

100.0

101.3

102.9

Ho.

ohr.

55

49

71

69

58

43

29

13

Mean

log p

(g/em3)

-8.78

-8.66

-8.56

-8.41

-8.26

-8.18

-8.10

-7-83

Mutlnn

E.d.

±0.04

0.04

0.03

0.03

0.04

0.04

0.09

0.09

LlKht

Mean H

93-3

91.9

90-7

88.9

87-0

86.1

85-1

81.6

0 -

57

51

72

70

60

43

30

13

Mr an

-8.46

-8.33

-8.19

-8.05

-7.92

-7.82

-7.67

-7.38

E.d.

±0.04

0.04

0.03

0.03

0.03

0.04

0.08

0.11

End

Mean B

89.5

87.8

86.1

84.4

82.8

81.6

79-6

75-3

Ho

57

51

72

70

60

43

29

12

All -O.59 0.03 -9.20 0.O2 8.6 387 -9.15 0.02 3.0 387 -8.43 0.02 89.2 396 .7 39"

TABLE 5.1.3.—Heights of the standard meteor when one parameter at a time is varied; all meteors, variable ZR

Range of

0.1-0.2

0.2-0.3

O.3-O.4

0.4-0.5

O.5-O.6

O.6-O.7

O.7-O.8

O.8-O.9

0-9-1.0

All

Mean log

cos Z_,

-0.801 ±

-0.596

-O.458

-O.}35

-O.258

-O.187

-O.125

-0.075

-O.015

-O.195

S.d.

0.041

0.016

0.006

0.004

0.003

0.002

0.002

0.002

0.002

0.006

log p

-9.30

-9.26

-9.29

-9.23

-9.22

-9.15

-9.23

-9-21

-9.21

-9.21

Beginning

S.d.

, (s/cffl3)

±0.08

0.10

0.05

0.05

0.06

0.04

0.04

0.04

0.05

0.02

Mean H

(km)

99-9

99-5

99-9

99.O

98.9

98.0

99.O

9S.7

9S.8

98.8

Mo.

obs.

4

9

29

37

32

84

73

74

45

387

Mean

log p

(g/cm3)

-9-39

-9-27

-9.25

-9.22

-9.15

-9.12

-9.17

-9-13

-9.19

-9-17

2

S.d.

(g/TM3)

±0.12

0.10

0.06

0.05

0.06

0.04

0.04

0.04

0.04

0.02

• 5

Mean H

(km)

101.2

99-6

99-3

98.9

97-9

97.6

98.3

97.8

98.4

98.2

Ho.

obs.

5

8

28

37

33

85

72

74

45

387

Mean

log p

(g/cm3)

-9-03

-8.88

-8.61

-8.57

-8.52

-8.41

-8.34

-8.24

-8.19

-8.40

Maximum Light

E.d.

(g/cm3)

* 0.05

0.07

0.05

0.05

0.05

0.03

0.03

0.0}

0.05

0.02

Mean H

(Km)

96.4

94.6

91-3

90.8

90.3

88. e

88.1

86.-8

86.1

88.8

No.

6

10

31

37

33

8C

7}

T>

46

396

Mean £

log P ((

(g/cm3)

-8.76 ±

-8.62

-8.37

-8.27

-8.11

-8.04

-7-9C

-7.86

-7.78

-8.04

:

.d.

0.08

0.09

0.06

0.05

0.05

0.0}

0.0}

0.0}

0.05

0.02

End

Mean H

93-1

9 l >

88.4

87.1

85.2

84.3

83-3

82.0

81.0

64.3

obs

6

ID

31

35

33

86

73

7k

46

39k
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 107

TABLE 5.1.4.—Heights of the standard meteor when one parameter at a time is varied; all meteors, variable a

Be R inn in*?

Range of Mean S.d. Mean E.d. Mean H No

lo;*, o log o log p / / 3 \ (tan) obe

, -2 2 . , -2 2 . , -2 2, , ,3 , VS/cm-J

(cm E ) (cm s ) (cm E )(g/eur)

-10.40- -10.83 ±0.02 -9.12 ±0.04 97.6 86

-ll.oo- -11.09 o.oi -9.17 o.o4 98.2 92

-11.15

-11.15- -11.23

-11.30

-11.30- -11.37

-11.45

-11.45- -11.67

-12.05

0.01 -9.29 0.03 99.8 99

0.01 -9.33 0.03 100.3 64

0.04 -9.12 0.06 97.6 46

Mean S.d. Mean H No

^ P (g/e^j M obs

(g/cm3)

-9.11 ±0.04 97.4 87

-9.15 0.03 97.6 92

-9.24 0.05 99.2 98

-9.25 0.05 99.5 65

-9.09 0.06 97.1 45

Maximum Light

Mean S.d. Mean H No

*** (g/cm3)

 {im) ° b S

(g/cm5)

-8.48 ±0.03 89.8 88

-8.43 0.03 89.I 92

-8.45 0.02 89.4 102

-8.37 0.03 88.3 66

-8.21 0.06 86.4 48

-11.19 0.01 -9.21 0.02 3.8 3S7 -9.17 o.oe 98.2 387 -8.41 0.01 3-9 396

E.-.i

Mean S.d. Mean H No.

l°g P t 1 J5\ (^0 obs.

(g/cm3)

-8.09 + 0.03 84.9 88

-8.06 0.03 84.5 92

-8.11 0.02 85.2 101

-8.04 0.05 84.3 66

-7.84 0.05 81.7 47

-8.05 0.01 84.4 394

Actually 0.004

TABLE 5.2.1.—Heights of the standard meteor when one parameter at a lime is varied; sporadic meteors minus (A + S+D),

variable vm

Velocity

range

(km/0

10-15

15-20

20-25

25-30

30-35

35-40

40-45

45-50

50-55

55-60

60-65

65-70

70-75

A l l

Mean

log v .

(W0

1.124

1.250

I.549

1.436

1.505

1--571

1.634

1-673

1-724

1.762

1.794

1.830

1.855

1.484

E.d.

(W0

t0.016

0.005

0.004

0.004

0.003

0.006

0.005

0.005

0.005

0.004

0.003

0.003

0.003

0.013

Mean

l°g P

(g/cm5)

- 7-54

- 8.41

- 8.79

- 9-27

- 9.47

- 9-56

- 9-83

- 9-79

-10.24

-10.17

-10.29

-10.50

-10.51

- 9.26

Begir.

S.d.

(g/cm3)

* 0.11

0.05

0.06

0.05

..04

0.09

0.10

0.13

0.08

0.12

O.OL'

0.07

0.05

0.05

inlng

Mean K

(km)

77-7

88.9

93-5

99-6

102.1

103.4

107.2

106.7

113-5

112.4

114.2

117.8

118.1

09.4

No.

6

45

42

35

27

1 1

1 0

9

6

8

15

1 1

5

230

Mean

log p

(g/cm3)

- 7-34

- 8.25

- 8.66

-9-l £

- 9.48

- 9-56

- 9.84

-9-78

-10.29

-IO.39

-10.42

-10.57

-10.68

-9.21

2

S.d.

(g/cm3)

* 0.12

0.05

0.05

0.04

0.05

0.09

0.09

0.14

0.08

0.13

0.07

0.09

0.09

0.06

•5

Mean H

74.7

86.9

91.9

98.2

102.2

103.4

107-5

106.6

114.3

116.0

116.4

119.2

121.1

98.7

No.

6

46

42

35

27

1 1

1 0

1 0

6

9

15

1 0

5

232

Mean

log p

-7.44

-8.03

-8.20

-8.35

-8.52

-8.66

-8.76

-8.61

-8.97

-8.93

-8.95

-8.96

-9.03

-8.43

Maximum Light

S.d.

(g/cm3)

± 0.10

0.04

0.04

0.03

0.06

0.09

0.08

0.07

0.10

0.06

0.07

0.08

0.12

0.03

Mean H

(la.)

76.2

64.1

86.2

88.2

90.3

91.9

93-1

91-3

95.7

95-2

95J*

95.6

96.1.

69.1

obs.

6

46

42

35

27

1 1

1 0

1 1

6

1 1

15

12

5

237

Mean

log p

-7-35

-7-74

-7.9O

-8.01

-8.18

-8.20

-8.29

-8.17

-8.58

-8.53

-8A7

-8.58

-8.66

-8.08

E n d

S.d. 1

(g/cm5)

+ 0.07

0.03

0.03

0.03

0.05

0.07

O.09

0.08

0.03

0.08

0.06

0.05

0.06

0.02

fean H

(km)

7*.7

60.6

82.5

33-9

86.1

86.2

87.4

85-9

91.O

90.<*

89.7

90.9

91.9

84.8

o b s

6

45

42

35

27

i l

1 0

11

6

l i

15

1 1

5

235

TABLE 5.2.2.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

variable mm

Mass

range

(g)

0.01-0.05

0.05-0.10

0.10-0.20

0.20-0.40

0.40-0.80

0.80-1.60

1.60-5.0

5-0 - 34

A l l

Hean

logm,,

(g)

-1.54

-1.14

-0.84

-O.52

-0.22

0.04

O.39

0.91

-0.55

S.d.

, (g)

^ 0.03

0.02

0.01

0.01

0.01

0.02

0.04

0.07

0.04

Mean

log P

(g/cm5)

-9.OO

-9-07

-9.29

-9-25

-9-33

-9-35

-9.40

-9.56

-9.25

Beginning

S.d.

(g/cm3)

i 0.04

0.06

0.04

0.04

0.05

0.06

0.10

0.13

0.02

Mean H

(km)

96.0

96.9

99-9

99-3

100.3

100.6

101.3

103.4

99-3

obs.

37

23

39

36

38

30

16

11

230

Mean

log p

'g/cm3)

-8.91

-9.02

-9.18

-9.20

-9.30

-9.32

-9.42

-9-57

-9.20

2

S.d .

(g/cm3)

k 0.04

0.07

0.04

0.04

0.05

0.06

0.10

0.12

0.02

.5

Mean H

(km)

94.9

96.3

96.4

98.6

100.0

100.3

101.5

103.6

98.6

Bo.

obe.

36

24

39

36

38

3 1

16

12

232

Mean

log p

(g/cm3)

-8.73

-8.67

-8.58

-8.41

-8.29

-8.25

-8.07

-7-92

-8.42

Maximum

E.d.

(g/cm3)

± 0.04

0.06

0.03

0.04

0.04

0.05

0.07

0.07

0.02

Light

Mean H

(km)

92-7

92.0

91.0

88.8

87-3

86.6

84.7

82.7

89.1

N o .

38

25

39

37

39

31

16

12

237

Mean

log p

(g/cm3)

-8.42

-8-33

-8.25

-6.05

-7-96

-7.86

-7-70

-7-51

-8.08

End

S.d.

(g/cm3)

r 0-05

0.05

0.03

0.04

0.03

0.05

0.06

0.07

0.02

Mean H

89.O

87-9

86.8

84.4

83-3

82.0

80.0

77-3

84.8

o b s

38

25

39

37

39

31

15

11

235
108 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 5.2.3.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

variable ZR

Range ->f

cos Z^

0.1-0.2

0.2-0.3

0.3-0.4

0.4-0.5

0.5-0.6

0.6-0.7

0.7-0.8

O.8-O.9

0.9-1.0

A ll

Mean 1-

-0.828

-0.605

-0.453

-O.336

-0.263

-0.188

-0.122

-0.076

-0.017

-0.203

ig S.d.

± 0.081

0.021

0.008

0.005

0.005

0.003

0.002

0.002

0.003

0.010

Mean

log p

-9.40

-9.25

-9-35

-9-23

-9.25

-9.17

-9.28

-9.29

-9.29

-9.26

Begii

E.d.

—

±0.11

0.07

0.06

0.06

0.05

0.04

0.04

0.07

0.02

ininK

Mean H

(km)

101.2

99-3

100.3

99.0

99-3

98.2

99-7

99-9

99-9

99.4

No.

1

6

18

26

18

49

45

44

23

230

(g/cm5)

-9-55

-9.25

-9.27

-9.19

-9.17

-9.15

-9.23

-9.20

-9.24

-9.20

2

S.d.

(g/cm5)

±0.22

0.10

0.07

0.06

0.08

0.05

0.04

0.04

0.06

0.02

.5

Mean H

103.2

99-3

99-5

98.5

98.2

98.0

99.O

98.6

99.1

99.7

No.

2

5

18

26

19

50

45

44

23

232

Mean

-8-95

-8.84

-8.62

-8.52

-8.51

-8.39

-8.40

-8.28

-8.24

-£.42

Maximum

S.d.

±0.03

0.07

0.06

0.06

0.05

0.03

0.04

0.04

0.06

0.02

Li«ht

Mean H

95.4

94.0

91-3

90.3

90.1

88.6

88.8

87.2

86.8

89.0

No.

3

7

20

26

19

50

45

44

23

237

M«an

log p

(g/cm5)

-8.64

-e.58

-8.34

-8.20

-8.12

-8.05

-8.03

-7-93

-7.87

-e.07

El

S.d.

±0.06

0.11

0.06

0.0c.

0.05

0.03

0.03

0.03

0.05

o.oe

i d

* a n H

91.6

90.9

88.1

86.2

85.3

84.3

84.1

82.8

82.1

84.7

He

3

7

20

24

19

50

*5

44

23

235

TABLE 5.2.4.—Heights of the standard meteor when one parameter at a time is varied; sporadic ineteors minus (A + S+D),

variable a

Range of Mean

(cm s ) (cm s

S.d. Mean H No. Mea

2.5

S.d. Mean H

-10.40- -10.87 ±0.01 -9.20 ±0.05 98.7 47

-11.00

-11.00- -II.09 0.01 -9.23 0.04 99.1 59

-11.15

-11.15- -ia.23 0.01* -9.30 0.03 100.0 68

-11.30

-II.30- -H.38 0.01 -9.36 0.04 100.7 34 -9.23 0.05 99.I 35

-H.45

-II.45- -11.63 0.03 -9.13 0.07 97.8 22 -9.O9 0.09 97.2 21

-12.05 ~

-9.19 ±0.05 98.5 48

-9.18 0.04 98.4 59

-9.26 0.03 99.4 69

Maximum Llffht

Mean S.d. Mean H No.

log p

(g/cm5)

-8.55 ±0.05 90.6 48

-8.46 0.03 89.5 59

-8.46 0.03 89.5 71

-8.34 0.04 88.1 36

-8.10 0.04 85.O 23

Mean S.d. Mean H Ho.

1 0 8 P

, (s/ca 5)

 (km ) 0t>8<

(g/crrr)

-8.17 ±0.04 85.9 k6

-8.11 0.03 85.1 59

-8.11 0.02 85.1 70

-8.04 0.04 84.3 36

-7.79 0.04 81.2 22

-11.18 0.02 -9.26 0.02 99.4 230 -9.21 0.02 -8.43 0.02 89.I 237 -8.08 0.02 84.8 235

Actually 0.0049

TABLE 5.3.1.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q<6 a.u., variable vm

Velocity

(km/s)

10-15

15-20

20-25

25-30

30-35

35-40

40-45

Mear

log v

(km/s

1.130

1.247

1.345

1.437

1.507

1.564

1.623

S.d. Mean S.d. Mean H No

(km/s) log p (g/cnI3) (km) obs

(g/cm5)

t 0.011 -7.89 ±0.07 82.4 9

0.005 -8.50 0.05 90.I 47

0.004 -8.78 0.05 93.3 44

0.005 -9-15 0.07 98.O 31

0.004 -9.39 0.06 101.1 17

0.006 -9.07 0.19 96.9 7

0.004 -9.57 0.33 103.5 2

1.352 0.009 -8.8l 0.04 93.7 157

(g/cm5)

S.d. Mean E

(g/cm3) ("»)

-7.69 ±0.09 79.9

-8.31 0.04 87.6

-8.63 0.05 91.6

-9.07 0.06 96.9

-9.40 0.07 101.2

-9.10 0.18 97.3

-9.51 0.40 102.7

Maximum Light

Mean S.d.

-7.70 ±0.08

-8.05 0.03

-8.20 0.04

-8.35 0.04

-8.41 0.08

-8.36 0.08

-8.61 0.10

Mean H No.

80.0 9

84.3 48

86.3 44

88.2 32

88.9 17

88.3 7

91.2 2

Mean S.d. Mean H Ho.

1 0 6 p (g/cm3

)

 (km )

 °bS#

(g/cm3)

-7.62 ± 0.07

-7.8O 0.04

-7.91 0.04

-7.97 0.04

-8.05 0.07

.7.96 0.11

-8.08 0.22

78.9

81.3

82.6

83.4

84.4

83.2

84.8

0.04 92.1 158 -8.19 0.02 86.1 159 -7.89 0.02 82.4 159
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 109

TABLE 5.3.2.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q< 0 a.u., variable ma

Beginning Maximum Light

Mass Mean S.d.

ran<;e log m a (g)

( g )

 (g)

O.O1-0.05 -1.36 ± O.Ol*

0.05-0.10 -1.12 0.05

0.10-0.20 -0.85 0.02

0.20-0.1*0 -0.53 0.01

0.1*0-0.80 -0.2l» 0.01

0.80-1.60 0.05 0.02

1.6-5.0 0.37 O.oi*

5.0-34 0.96 0.10 -9.51*

Mean

log p

(g/cm3)

-8.92

-9.08

-9-26

-9.20

-9.26

-9.21*

-9.22

-9.51*

-9.25

S.d.

(g/cm5)

±0.22

0.18

0.08

0.06

0.05

0.06

0.09

0.16

0.05

Mean H

(km)

95.0

97.1

99-5

98.6

99.U

99.2

98.9

100.5

99.0

obs.

2

8

25

55

57

29

15

8

157

Mean

log p

(g/cm3)

-8.72

-8.99

-9.15

-9.il*

-9.25

-9.27

-9.27

-9-39

-9.21

S.d.

(g/co5)

± O.31

0.18

0.07

0.06

0.05

0.06

0..T9

0.12

0.05

Mean H

(km)

92.6

95-9

98.O

97-8

99-3

99-6

99-5

101.2

98.7

Ho.

obs.

a

8

25

33

57

29

15

9

158

Mean

log p

(g/cm3)

-8.69

-8.5"*

-8.51*

-8.1*0

-8.25

-8.15

-8.00

-7.75

-8.28

S.d.

(g/cm3)

± 0.08

0.12

0.05

O.Ol*

O.Ol*

0.05

0.07

0.10

0.03

Mean E

(km)

92.3

90.5

90.5

88.7

86.9

85-7

85.8

80.6

87.5

Ho.

obs.

2

8

26

55

57

29

15

9

159

Mean

log p

(g/cm3)

-8.58

-8.27

-8.20

-7-96

-7.87

-7.7U

-7-58

-7.21

-7.88

S.d.

(g/cm3)

±0.2U

0.12

0.05

O.Ol*

o.oi*

0.05

0.06

O.ll*

0.03

Mean H

(km)

88.5

87.1

86.3

83.2

82.2

80.5

78.3

72.5

82.5

He

obE

2

8

26

33

37

29

15

9

159

TABLE 5.3.3.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q <6 a.u., variable ZR

Range of Mean log

cos ZR cos ^

0.1-0.2

0.2-0.3

0.5-0.1*

o.i*-0.5

0.5-0.6

0.6-0.7

0.7-0.8

0.8-0.9

O.9-1.O

-0.796

-0.573

-0.1*36

-0.332

-0.262

-0.182

-0.123

-0.075

-0.019

S.d.

±0.003

0.012

O.OO8

0.007

0.005

0.003

0.003

0.005

0.007

Mean

log p

(g/cm3)

-9.51*

-9-33

-9.25

-9.29

-9.25

-9.19

-9.25

-9.il*

-9.08

Beginning

E.d.

(g/cm3)

±0.11

0.19

0.07

0.08

0.05

0.07

0.06

0.05

0.19

Mean H

(km)

105.1

100.5

99-3

99.3

99-3

98.1*

99.O

97.8

97-1

No.

obs.

2

5

11

10

16

35

30

1*2

6

Mean

log p

(g/cm5)

-9.50

-9-31

-9-18

-9.25

-9-18

-9.17

-9.16

-9.07

-9-07

S.d.

(g/cm3)

±0.K>

0.16

0.06

0.08

0.06

0.07

0.06

0.05

0.19

2.5

Mean H

(km)

102.6

100.1

98.1*

99.lt

98.I*

98.2

98.1

96.9

96.9

obs.

2

5

11

10

16

36

50

1*2

6

]

Mean

log p

(g/cm5)

-9.19

-8.95

-8.50

-8.53

-8.51

-8.36

-8.35

-8.21

-8.06

Maximum Li^ht

S.d.

(g/cm5)

±0.12

0.12

0.09

0.09

0.05

0.05

0.01*

0.01*

0.13

•w

98.5

95-1

90.0

90.1*

90.2

88.3

87-9

86.1*

81*.5

obs!

2

5

11

10

16

37

30

>*2

6

Mean

log p

(g/cm3)

-8.83

-8.59

-8.23

-8.15

-8.12

-8.00

-7-93

-7.80

-7-76

E.d.

(g/cm3)

±0.11

0.15

0.07

0.08

0.05

0.01*

0.05

O.OU

0.12

End

Mean E

(km)

93-9

91.0

86.6

85-7

85.3

83.8

82.9

81.2

8O.7

He

obs

2

5

11

10

16

37

30

1*2

6

-0.192 0.012 -9.20 0.03 -9.15 0-°3 98.0 158 -8.37 0.02 3.1* 159 -7-99 0.03 83.7 159

TABLE 5.3.4.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q <6 a.u., variable a

Range of Mea

, -2 2 W -2

S.d. Mean

log p

an"2 s 2) (g/cm3)

Beginning

S.d. Mean H No

0 0

-10.1*0- -10.81* i 0.02

-11.00

-8.99 ± 0.05 95-9

-11.00- -11.09 0.01 -9.09 0.05 97.2 1*7

-11.15

-11.15- -11.23 0.01 -9.27 0.05 99.5 1*2

-11.30

-11.30- -11.37 0.01

-11.1*5

-11.1*5- -11.62 0.07

-12.05

All -II.09 0.02

225-636 O-67—8

-9.50 0.03 102.5 12

-9.21* 0.15 99.2 7

-9.il* 0.03 97-9 157

Mean S.d. Mean S No.

1 0 8 p

, (g/cm3)

 (ta ) ObS

-

(g/cm3)

-8.97 ± O.oi* 95-7 1*9

-9.01* 0.05 96.6 1*7

-9.23 0.05 99-0 1*3

-9.39 O.OU 101.1 12

-9.20 O.lB 96.6 7

-9.10 0.03 97.1* 158

Maximum Light

Mean S A. Mean H Ho.

(g/cm3)

-8.1*0 ± O.OU 89.8 50

-8.35 O.CA 88.2 U7

-8.1*5 0.03 89.U U3

-8.U5 0.07 89.I 12

-8.08 0.05 81* .8 7

-8.39 0.02 3.6 159

Mean S.d. Mean H Ho.

1 0 6 p

, (g/cm3) <to>

 obs

-

(g/cm5)

-7.99 ±0.03 83.7 50

-7.98 O.Ol* 83.5 U7

-8.06 0.03 81*.5 1*3

-8.13 0.05 85.1* 12

-7.66 0.10 79-5 7

-8.00 0.02 63.8 159
110 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 5.4.1.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q> 0 a.u., variable vm

Velocity Mean S.d.

range log v (tan/s)

<w>

Beginning

Mean

log p

(g/cm3)

S.d.

(g/cm3)

Mean H

(to)

Mean

log p

(g/cm3)

S.d.

(g/cm3)

Mean H

(to)

(g/cm3)

Maximum Light

S.d. Mean H

(g/cm3) I***

Mean S.d. Mean H

l o g

 % (g/cm3) C")

(g/cm5)

15-20

20-25

25-50

30-55

35-40

i*o-i*5

U5-50

50-55

55-60

60-65

65-70

70-75

1.2*7 ± 0.015

1.348 0.010

l.*3* 0.006

1.501 0.005

1.578 0.007

1.636 0.005

1.67* 0.00*

1.726 0.00*

1.763 0.00*

1.79* 0.003

1.830 0.003

1.855 0.003

- 8.38 ± 0.19

- 8.96 0.08

- 9.31 0.08

- 9.*1 0.07

- 9-75 0.06

- 9.89 0.10

- 9.8O 0.15

-10.26 0.08

-10.18 0.13

-10.35 0.05

-10.55 0.06

.10.56 0.06

88.5

95-5

100.2

101.1*

106.1

108.1

106.8

133.8

112.5

115.3

II8.7

119.0

- 8.28 ± 0.19

- 8.79 0.06

- 9.22 0.09

- 9.*3 0.07

- 9-76 0.05

- 9.90 0.08

- 9-75 0.15

-10.27 0.08

-IO.3O 0.12

-10.*3 0.06

-10.56 0.07

-10.68 0.09

87.3

93.1*

98.9

101.6

106.2

108.1*

106.1

113.9

11U.5

U6£

119.1

121.1

-8.16 ± 0.1*

-8.31 0.08

-8.37 0.06

-8.57 0.08

-8.86 O.09

-8.79 0.08

-8.62 0.07

-8.98 0.11

-8.90 0.06

-8.98 0.08

-8.96 0.08

-9.02 0.12

85-7

87.7

88.5

90.8

9*-3

93.it

91-3

95.8

9U.8

95-7

95-5

96.1*

-7.75 *

-8.01

-8.0l*

-8.21*

-8.32

-8.38

-8.15

-8.61

-8.52

-8.51*

-8.60

-8.69

0.15

0.0*

0.05

0.07

0.09

0.10

0.08

0.08

0.07

0.07

0.05

0.06

80.6

83.9

81* .3

86.7

87.8

88.5

85.7

91-3

90.3

90.5

91-1

92.2

A l l 1.631 0.0l£ - 9.82 0.06 107.1 11* - 9.8I 0.07 107.0 115 -8.72 0.03 92.6 120 -8.3* 0.03 88.0 118

TABLE 5.4.2.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q> 0 a.u., variable mm

Mass Mean

range log "

(e> (g)

S.d.

(6)

Beginning

Mean S.d. Mean H

obs.

2.5

Mean S.d. Mean H

log p

(g/cm3)

Maximum Light

e P

(g/cm3)

S.d. Mean E

(g/cm5) (ta)

Mean

1 06 P,

(g/cnr)

0.01-0.05

0.05-0.10

0.10-0.20

0.20-0.1*0

0.1*0-0.80

O.8O-I.6O

1.60-5.0

5.0 -3*

-1-55*0.03

-1.1* 0.02

-0.85 0.02

-0-55 0.02

-0.21 0.02

0.03 0.03

0.39 0.0*

0.85 0.06

-9.O8 i 0.0*

-9.1* 0.07

-9.20 0.07

-9.28

-9.1*0

-9-52

-9.67

-9-71

97.1

97.9

98.7

0.05 99-7

0.11 101.2

0.08 102.9

0.02 105.0

0.16 105.5

-9.02

-9.12

-9-13

-9.23

-9-35

-9.58

-9-67

-9-69

± 0.0*

0.07

0.07

0.07

96.3

97-6

37.7

99-0

O.ll 100.7

0.1* 101.0

0.03 10*.9

0.17 105.2

-8.87 4 0.05

-8.82 0.07

-8.60 0.05

-8.53 0.09

-8.55 0.10

-8.51 0.10

-8.21 0.0*

-7.95 0.09

9*-5

93-7

91.2

90.3

88.2

87-7

86.*

83.2

-8.*7 * 0.05

-8.39 0.06

0.05

0.07

0.07

0.10

0.05

0.06

-8.18

-8.21

-7-99

-7-98

-7.85

-7-59

89.6

88.6

86.0

86.3

83.6

83-5

81-9

78.5

A l l -0.86 0.06 -9.2* 0.03 99.2 1 1* -9.18 0.03 98.* 115 -8.63 0.03 91.6 120 -8.25 0.03 86.9

1ABI

Range of

0.1-0.2

0.2-0.3

0.3-0.4

O.U-0.5

O.5-O.6

O.6-O.7

O.7-O.8

O.8-O.9

O.9-I.0

A l l

J5 5.4.3

Mean log

-0.845 i

-0.636

-0.1*68

-0.338

-O.274

-O.193

-0.124

-0.079

-0.017

-0.218

.—tie

S.d.

: 0.138

0.026

0.010

0.006

0.007

0.004

0.003

0.003

0.003

0.017

ights of the standai

Beginning

~

-9.52

-9.52

-9-33

-9-53

-9-19

-9-35

-9-37

-9.34

-9.34

-

*- 0.02

0.07

0.06

0.05

0.06

0.05

0.08

0.06

0.03

Mean h

(to)

--

IO2.9

102-9

100.3

103.0

98.5

100.6

100.8

100.5

100.5

a meteor when one

distance Q >

No.

obs.

-

3

10

21

3

21

19

17

20

114

Mean

log p

(g/cm3)

-9.66

-9.41 ±

-9.46

-9.29

-9.22

-9.13

-9-50

-9-27

-9.27

-9.27

2

S.d.

(g/cm3)

-

: 0.04

0.06

0.06

0.28

0.06

0.05

0.08

0.07

0.03

parameter at a

6 a.u., variable

.5

Mean B

(to)

104.7

101.3

102.0

99-8

98.9

97-7

100.0

99-6

99-5

99.6

Ho.

obs.

1

2

10

2 1

*

2 1

19

17

20

115

time is varied; sporadic meteors

Mean

log p

(g/cm3)

-9.01

-9.00

-8.80

-8.6*

-8.59

-8.41

-8.48

-8.41

-8.33

-8.52

Maximum Light

S.d.

(g/cm3)

± 0.01

0.07

0.06

0.06

0.16

0.05

0.06

0.08

0.06

0.03

Mean H

(to)

96.2

96.0

93-5

91.6

91-1

88.9

89.7

88.8

87.9

90.3

No.

obs.

2

4

12

21

4

21

19

17

20

120

Mean

log p

(g/cm3)

-8.72

-8.78

-8.49

-8.30

-8.18

-8.06

-8.06

-7.98

-7.90

-8.14

with aphelion

S.d.

(g/cm

± 0.15

0.04

0.06

0.07

0.20

0.05

0.05

0.06

0.06

0.05

End

Mean H

) (km)

92.6

93-3

89-9

87-5

86.1

84.5

84.5

83-5

82.5

85-5

Ho

obs

2

4

12

19

4

21

19

17

20

llfl
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 111

TABLE 5.4.4.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors with aphelion

distance Q >tf a.u., variable a

Range of Mean

log a log o

Mean S.d. Mean H Ho.

l oB P (g/cm3

) ("») °bs.

(g/cm3)

2-5

Mean S.d. Mean H No.

log P (-/ 5^ (km) obs.

(g/cm3)

Maximum Light

Mean S.d. Mean H NO.

log P /_ / 5\ (km) obs.

(g/cm3)

Mean S.d. Mean H Ho

1 0 8 p (g/cm3

) (t a )

 ob s

(g/cm3)

-10.40- -10.79 * 0.05 -9-54 ±0.09 100.5 17

-11.00

-11.00- -11.09 0.01 -9.38 0.04 100.9 21

-11.15

-11.15- -11.25 0.01 -9.3^ 0.05 100.5 55

-11.30

-II.50- -II.58 0.01 -9 . U2 0.04 101.5 25

-11.1*5

-11.45- -11.64 0.05 -9.13 0.08 97.7 18

-12.05

-9.51* i 0.08 100.5 18

-9.51 O.Ol* 100. 1 21

-9.29 0.05 99-9 53

-9.27 0.06 99.5 26

-9.06 0.10 96.8 17

-8.72 1 0.09 92.6 18

-8.60 0.05 91.1 21

-8.50 0.01* 90.0 55

-8.1*2 0.05 89.0 27

-8.16 0.06 85.8 19

-8.26 * 0.08 87.O 18

-8.17 O.Ol* 85.9 21

-8.15 0.01* 85.6 31*

-8.09 0.05 81*.8 27

-7.81* 0.06 81.8 18

All -11.24 0.03 -9.33 0.03 100.4 114 -9.26 0.05 99-5 115 -8.1*8 0.03 89.7 120 -8.11 0.03 85.I 118

TABLE 5.5.1.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with \x\ <0.2, variable v o

Beginning Light

Velocity Mean

range log y_

(km/s)

S.d.

(km/s)

10-15

15-20

20-25

25-50

30-55

35-40

40-45

45-50

50-55

55-60

60-65

65-70

70-75

.109 ± 0.029

.250 0.007

.552 0.005

.440 0.005

.507 0.005

.580 0.009

.649 0.004

.674 0.006

.721 0.008

.754 0.006

.799 0.004

.824 0.005

.856 O.OO6

Mean S.d. Mean H

(km)

- 7.51 ± 0.07 77-2 5

- 8.61 0.06 91.5 22

- 8.83 0.07 94.0 22

- 9.29 0.06 99.8 22

- 9.54 0.05 103.1 17

- 9.81 0.08 107.0 5

- 9.99 0.04 109.7 2

- 9.93 0.08 IO8.9 6

-10.14 0.12 111.9 3

- 9.97 0.17 109.4 4

-10.30 0.12 114.4 5

-ID.46 0.04 117.1 3

-10.54 0.07 118.7 2

Mean S.d.

1 0 6

 Ms/cm3)

(g/cm3)

1

Mean H

(km)

- 7-25*0.05 73-1 3

- 8.42 0.06 89.O 22

-•8.69 0.06 92.2 22

- 9.19 0.05 98.4 22

- 9.51 0.05 102.7 17

- 9.81 0.07 107.0 5

- 9.98 0.04 IO9.6 2

- 9.81 0.16 106.9 7

-10.21 0.12 113.0 3

-10.16 0.20 112.3 4

-10.40 0.12 116.1 5

-10.54 0.01 118.7 3

-10.59 0.11 119.6 2

Mean

log p

(g/cm3)

-7-37

-8.15

-8.18

-8.59

-8.57

-8.90

-8.78

-8.63

-9.11

-8.78

-9.04

-8.92

-9.24

S.d.

(g/cm3)

± 0.07

0.04

0.05

0.04

0.06

0.07

0.02

0.09

0.15

0.10

0.11

0.16

0.18

Mean H

(km)

75-1

85.7

86.0

88.6

90.3

94.8

9 3 -

91-5

97.4

93.4

96.6

95.0

99-1

No.

obs.

3

22

22

22

17

5

2

7

3

5

5

4

2

Mean

log p

-7.30

-7.80

-7.86

-8.02

-8.21

-8.26

-8.18

-8.15

-8.58

-8.37

-8.50

-8.45

-8.78

S.d.

± 0.05

0.05

0.04

0.04

0.04

0.12

0.04

0.10

0.06

0.13

0.09

0.08

0.02

Mean H

(km)

7-..0

31.3

82.0

84.0

86.4

87.I

86.0

85.6

91.0

88.4

90.0

89.4

93-3

No

3

21

22

22

17

5

2

7

3

5

5

4

2

All 1.468 0.017 - 9-27 0.06 99.6 116 - 9-19 0.07 98.5 117 89.5 119 -8.06 0.03 84.5 118

TABLE 5.5.2.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with |x| <0.B, variable mm

Beginning

Mass Mea

range log

( )

S.d. Mean E. d.

(d log P ( y^ j

(g/cm3)

0.01-0.05 - 1

0.05-0.10 -1

0.10-0.20 -0

0.20-0.40 -O

0.40-0.80 -0

0.80-1 £0 0

I.6O-5.O 0

5-0 -34 0

51 ±0.03

13 0.03

86 0.02

52 0.02

20 0.O2

03 0.02

39 0.06

90 0.07

-9.01 ± 0.05

-9.13 0.10

0.05

O.05

0.05

0.09

0.13

0.07

-9-35

-9.25

-9.1*5

-9-37

-9.52

-9-85

(km)

96.1

97.8

100.6

99-3

101.9

100.9

1O2.9

107-5

Mean S.d. Mean H Ho.

(g/cm3)

(g/cm3)

-8.92 ± 0.06 95-0 10

-9.07 0.10 96.9 11

-9.22 0.04 98.9 24

-9.20 0.05 96.6 18

-9.41 0.04 101.3 19

-9.28 0.09 99-7 18

-9.49 0.13 102.5 9

-9.78 0.06 106.5 8

Maximum Light

Mean S.d. Mean H Ho

1 0 8 p

, (g/em3)

 (ta ) ob B

(g/cm3)

-8.72 ± 0.08 92.6 11

-8.84 0.08 94.0 11

-8.64 0.04 91.6 24

-8.40 0.05 88.7 18

-8.32 0.06 87.8 20

-8.19 0.06 66.2 18

-8.11 0.07 85.I 9

-8.02 0.07 84.1 8

End

Mean S.d. Mean H Ho.

log P ( g / e n 3) (km) obs.

(g/cm3)

-8.32 ± 0.06 87.8 11

-8.45 0.07 89.4 U

-8.26 0.03 87.I 24

-8.02 0.04 84.1 18

-7.96 0.04 83.2 20

-7.79 0.06 81.1 18

-7.67 0.07 79-5 6

-7.52 0.08 77.4 8

A l l -0.43 0.06 -9-35 0.03 100.6 116 -9.28 0.03 99-6 117 -8.42 0.03 9.1 119 -8.03 0.03 84.2 Ufi
112 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 5.5.3.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with |xl <0.2, variable ZR

Range of Mean log

COS Z^ COS ZJJ

0.1-0.2

0.2-O.3

0.3-0.1*

0.4-0.5

0.5-0.6

0.6-0.7

0.7-0.8

0.8-0.9

0.9-1.0

A l l

-0.985

-O.587

-0.461

-0.338

-0.265

-O.I85

-0.124

-O.O76

-G.015

-0.184

S.d.

„

± 0.027

0.013

0.010

0.005

0.003

0.003

0.003

0.003

O.Oll*

Mean

log p

(g/c*5)

. .

-9.21*

-9.1*7

-9-54

-9.27

-9-27

-9-57

-9-55

-9-31*

-9-33

Beginning

S.d.

(g/c*5)

„

± 0.21

0.05

0.12

0.08

0.05

0.05

O.06

0.08

0.03

Mean H

(km)

—

99.1

1O2.1

100.5

99-6

99-5

100.8

100.5

100.5

100.5

Ho.

obs.

—

5

7

8

10

21*

28

22

11*

116

Mean

log p

(g/oB5)

—

-9.21*

-9.1*1

-9.30

-9.il*

-9.21

-9.28

-9.21

-9.25

-9.21*

2

S.d.

(g/cm5)

—

± 0.18

0.05

0.11

0.12

0.05

0.05

0.05

0.08

0.02

.5

Mean H

(km)

—

99.1

101.1*

100.0

97.8

98.8

99.6

98.8

99.5

99.2

Ho.

obs.

-

5

7

8

11

21*

28

22

14

117

Maximum

Mean

log p

(g/cm5)

-8-95

-8.88

-8.75

-8.69

-8.55

-8.1*1

-8.1*5

-8.50

-8.25

-8.W

S.d.

(g/cm5)

~

± 0.13

0.04

0.10

0.07

0.05

0.05

0.06

0.07

0.03

Light

Mean H

(km)

95.1

9U.5

92.7

92-3

90.3

88.9

89.2

87.5

86.7

89.3

No.

obs.

1

1*

7

8

11

2l*

28

22

11*

119

Mean

log p

(g/cn3)

-8.79

-8.51

-8.1*7

-8.25

-8.08

-8.03

-8.02

-7.88

-7.81*

-8.05

E

S.d.

(g/cm5

~

t 0.20

0.06

0.10

0.09

o.oi*

o.oi*

o.ou

0.07

0.05

nd

Mean H

(km)

9 3 . k

90.1

89.7

86.9

81. .7

81* .2

84.1

82.3

81.8

84.5

No

obs

1

4

7

7

11

24

28

22

14

118

TABLE 5.5.4.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus

with |x| <0.2, variable a

Range of Mean

log a

Mean S.d.

log p

Beginning

Mean H No.

-10.40- -10.88 ± 0.02 -9.25 ±0.09 99.1 IB

-11.00

-11.00- -11.09 0.01 -9.24 0.05 99.2 29

-11.15

-11.15- -11.25 0.01 -9.38 o.o4 101.0 34

-11.30

-11.30- -11.58 0.01 -9.45 o.o4 101.7 25

-11.45

-II.45- -11.54 0.02 -9.55 0.05 100.5 12

-12.05

0.O2 -9.33 0.03 100.3 116

-9.16 ±0.08 98.1 18

-9.16 0.05 98.2 29

-9.32 0.04 100.3 31*

-9.29 0.05 99.8 24

-9.29 0.04 99.8 12

-9.25 0.03 99-3 117

H—iHimim Ligh t

Mean S.d. MeanH Ho.

obs.

(g/cm5) ' "

-8.65 ±0.07 91.7 18

-8.48 0.05 89.8 29

-8.49 0.04 89.9 35

-8.37 0.04 88.3 25

-8.19 0.05 86.1 12

-8.46 0.02 89.5 119

Mean S.d. Mean H Ho.

-8.21 ±0.05 86.3 18

-8.06 0.04 84.5 29

-8.09 0.04 84.9 34

-8.02 0.05 84.0 25

-7.90 0.04 82.6 12

-8.07 0.02 84.6 llfl

TABLE 5.6.1.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with x >0.2, variable Vc

Velocity

range

(W.)

10-15

15-20

20-25

25-50

30-35

55-40

40-45

45-50

50-55

55-60

60-65

65-70

70-75

A ll

Mean

log v .

(ta/s)

1.140

1.250

1.544

1.431

1.500

1.565

I.629

I.672

1.727

I.768

1-791

1.835

1.854

1.501

S.d.

(*•/•)

±0.013

0.007

0.006

0.008

0.005

0.006

8.006

0.009

0.006

0.005

0.003

O.OO3

0.004

0.021

Mean

log p |

-7.62

- 8.29

-8.77

- 9.24

- 9.29

- 9.32

- 9-75

- 9.46

-10.15

-10.22

-10.10

-10.42

-10.36

- 9-22

fl» ginning

S.d.

[g/c 5)

±0.18

0.07

0.09

O.U.

0.06

0.10

0.09

0.27

0.03

0.07

0.06

0.05

0.05

0.08

Mean H

(ta)

78.8

87.4

93.2

99-1

99-7

100.2

106.1

102.0

112.0

113.2

111.4

llfi.5

115.5

98.9

Ho.

obs.

3

23

18

12

9

6

7

5

5

4

10

8

3

109

Mean

-7.49

- 8.14

- 8.64

- 9.U

- 9.27

-9.34

- 9-79

- 9-65

-10.23

-10.40

-10.30

-10.53

-10.64

- 9-19

S.d.

ig/co5)

±0.19

O.07

0.09

0.10

0.09

0.09

0.10

0.27

0.06

0.08

0.08

0.10

0.12

0.09

2 - 5

Mean H

(tan)

77-0

85-5

91.6

97.4

99-6

1O0.4

106.6

104.6

113.5

116.1

114.4

llfl .4

120.5

98.5

Ho.

obs.

5

24

18

12

9

6

7

3

3

5

10

7

3

110

Mean

log p

(g/cm5)

-7.51

-7-93

-8.22

-8.31

-8.47

-8.46

-8.81

-8.60

-8.84

-9.02

-8.87

-8.98

-8.88

-8.42

Maximum

S.d.

(g/cm5)

±0.20

0.05

0.06

0.06

0.13

0.09

0.07

0.14

0.11

0.03

0.09

0.09

0.13

0.04

Light

Mean H

(to)

77-2

82.9

86.5

87.6

89.6

89.5

95-7

91.2

94.0

96.5

94.5

95-7

94.5

89.0

No.

obs.

5

24

18

12

9

6

7

4

5

6

10

8

3

113

Mean

log p

-7.41

-7.70

-7-95

-7-99

-8.14

-8.13

-8.42

-8.22

-8.59

-8.7O

-8.1*7

-8.68

-8.59

-8.12

End

S.d. !

(g/cm5)

±0.16

0.05

0.05

0.06

0.12

0.08

0.09

0.13

0.05

0.06

0.08

0.08

0.03

0.04

Mean E

(km)

75-7

80.0

83.2

83-7

85-5

85.4

89.O

86.5

91.1

92.4

89.6

92.1

91.1

85.2

Ho

obs

5

24

IB

12

9

6

7

4

5

6

10

7

5

112
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 113

TABLE 5.6.2.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with x y-0.2, variable mm

Mass

range

(g)

Mean

log ma

(g)

S.d.

(g)

0.01-0.05 -1.55 ±0.01*

0.05-0.10 -l.lU 0.02

0.10-0.20 -0.81 0.02

0.20-0.1*0 -0.53

0.1*0-0.80 -0.25

0.80-1.60 0.05

1.60-5.0 0.59

5.0 -31* 0.91*

0.02

0.02

0.02

0.06

0.19

Beginning

Mean S.d.

log p

Mean H Ho.

(tan) obs.

-9.00 ±0.01* 96.O

-9.0i* 0.08 96.5

0.09 96.6

0.06 99-1

0.09 97.7

0.11 100.0

0.17 99.0

0.20 95-7

-9.19

-9.23

-9.33

-9.30

-9.23

-8.97

2.5

Mean S.d.

^ 8 P

(g/cn?)

Mean H Ho.

(h») obB.

-8.91* ±0.05

-8.99 0.08

0.07

0.06

0.08

-9.10

-9.18

-9.20

-9.32

-9.27

-9-15

95-3

96.0

97.1*

98.3

97-3

0.09 100.3

0.17 99-5

0.22 97.9

Maximum Light

Mean S.d. Mean H Ho.

1 08 p, (g/cm3) <ta> °*'-

(g/cm3)

-8.75 ±0.05 92.9

-8.55 0.08 90.6

-8.52 0.06 90.2

0.07 89.3

0.07 86.6

0.07 86.6

0.1* 83.7

0.05 80.3

-8.1*5

-8.22

-8.23

-7.99

-7.72

End

Mean S.d. Mean H Ho.

108 p, (e/cm3) 0") ol»-

(g/cm5)

-8.I18 ±0.05

-8.28 0.06

-8.21 0.05

-8.10 0.07

-7.97 0.06

-J.Sh 0.07

-7.71 0.1D

-7-39 0.06

89.8 27

87.2 13

86.3 15

85.O 18

83-1* 17

83.O 12

80.2 7

75.»* 3

All -0.67 0.07 -9.13 0.03 97.8 109 -9.10 0.03 97.3 n o -a A3 0.03 -8.15 0.03 85.6 112

TABLE 5.6.3.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with x >0.2, variable ZR

Range of Mean log

cos ZQ COS Z0.1-0.2

0.2-0.3

0.3-0.1*

0.4-0.5

0.5-0.6

0.6-0.7

0.7-0.8

0.8-0.9

0.9-1.0

A l l

-0.750 i

-0.628

-0.1*1*9

-0.336

-0.261

-0.191

-0.119

-0.077

-0.019

-0.227

S.d.

: 0.043

0.035

0.010

0.006

0.008

o.ooi*

o.ooi*

0.003

0.006

o.oi1;

Mean

log p

(g/cffl5)

-9.22

-9-17

-9.07

-9.09

-9-15

-9.08

-9.18

-9.2i*

-9-23

-Q.15

Beginnii

S.d.

(g/cm3)

—

± o.oi*

0.08

0.07

0.07

0.08

0.08

0.07

0.16

0.0^

3g

Mean E

(km)

98.9

98.3

96.9

97.3

98.0

97.0

98.3

99.2

99-1

97.q

Ho.

1

3

11

18

8

23

17

20

8

MO

Mean

log p

(g/cm3)

-9.21*

-9.11*

-9.07

-9.08

-9.12

-9.07

-9.16

-9.15

-9.19

-9.12

2 . 5

S.d.

(g/cm5)

4 0.01

0.09

0.09

0.07

0.07

0.07

0.07

0.06

O.ll*

0.03

Mean H

99-2

97.8

96.9

97-1

97-6

96.9

98.1

98.0

98.5

97.5

Ho.

2

2

11

18

8

21*

17

20

8

110

Maximum Light

Mean

log p

(g/cm5:

-8.83

-8.79

-8.53

-8.1*3

-8.50

-8.39

-8.36

-8.27

-8.19

-8.1*0

S.d.

(g/cm3)

±0.06

0.07

0.08

0.07

0.06

0.05

0.07

0.06

0.10

0.03

Mean H

93-9

93-5

90.3

89.1

90.0

88.6

88.2

87.1

86.2

88.7

Ho.

obs.

2

3

»

18

8

21*

17

20

8

133

Mean

(g/c*3

-8.65

-8.63

-8.29

-8.17

-8.1B

-8.09

-8.03

-7-97

-7.87

-8.11

End

S.d.

(g/cm3)

±0.03

0.03

0.08

0.07

0.05

0.05

0.06

0.05

0.08

0.03

Mean H

9i.e

91.6

87.3

85.9

86.0

8U .9

84.1

83-3

82.2

85.I

No

2

3

13

17

8

21*

17

20

8

U 2

TABLE 5.6.4.—Heights of the standard meteor when one parameter at a time is varied; sporadic meteors minus (A + S+D),

with x ~>0.2, variable a

Range of Mean

log a log

Mean S.d. Mean H

(km)

-10.1*0- -10.85 ± 0.02 -9.17 ± 0.06 96.3 27

-U.00

-11.00- -U.08 0.01 -9.22 0.05 9«.9 29

-11.15

-11.15- -11.23 0.01 -9.81 0.06 98.8 33

-11.30

-U.30- -11.37 0.01 -9.19 0.10 96.6 11

-11.1*5

-11.1*5- -11.75 0.05 -8.75 o.ll 93.0 9

-12.05

Mean S.d. Mean H Ho.

(ta) ob8'

-9.1B * 0.06 93.1* 28

-9.19 0.05 98.5 29

-9.19 0.05 99.5 31*

-9.12 0.10 97.5 n

-8.68 0.1} 92.1 8

Maximum Light End

Mean S.d. Mean H Ho. Mean S.d. Mean H Ho.

-8.1*8 ± 0.06 89.8 28

-8.1*6 O.Cd* 89.5 29

-8.1*1 O.Oi* 88.9 35

-8.32 0.09 87.7 11

-7.99 0.07 83.7 10

-8.17 ±0.05 85.9 28

-8.17 o.oi* 85.9 29

-8.11 0.03 85.2 35

-8.09 0.09 84.9 11

-7.69 0.08 79-8 9

All -11.16 0.02 -9.16 0.03 98.2 109 -9.1U 0.03 97.9 n o -8.1*0 0.03 88.7 113 -8.11 0.03 85.1 112
1 1 4 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 6.1.—Mean observed heights of Super-Schmidt meteors for groups of different velocity

Velocity

range

(km/6)

10 - 15

15 - 20

20-25

25 - 30

30 - 35

35 - 40

UO-45

45-50

50-55

55-60

60-65

65-70

70-75

A l l

Mean v^

(km/s3

13-5

17.7

22.4

27.4

31-9

36-7

42.8

47.3

53-0

58.2

61.7

67-7

71.4

35.3

S.d.

(W»)

±0. 3

0 . 2

0 . 2

0 . 2

0 . 2

0 . 2

0 . 2

0 . 4

0 . 5

0 . 4

0-3

0 . 2

0 . 3

0 . 8

Mean K

(km)

81.7

89.6

94.4

99.O

100.9

100.2

102.8

104.8

110.5

109-3

111.7

114.7

117.2

100.0

S.d.

(km)

* 0.3

0 . 6

0 . 6

0 . 6

0 . 6

0 . 7

0 . 7

1.8

0 . 6

1 . 1

0 . 9

0 . 5

1.8

0 . 4

Mo.

obs.

10

56

65

62

48

38

34

12

9

15

25

21

8

403

MeanHg

(km)

79-1

88.2

93-P

97-7

100.6

100.6

102.9

104.7

111.1

111.2

113.4

116.8

119.0

99.6

.5

 S-d*

(km)

± 1.2

0 .6

0 .6

0 .5

0 . 7

0 . 7

0.7

1-9

0 . 7

1.4

0 . 9

0 . 7

1-3

0 . 5

No.

obs.

9

57

65

62

47

38

31*

13

9

16

25

19

8

402

(km)

75-9

81.9

86.1

87-7

88.5

88.7

95.O

92.0

99.8

98.1

99-7

102.4

100.5

89.8

. S.d.

(km)

± 1.8

0.6

0 .6

0-5

0 . 7

1.0

0 .6

1.2

1.9

1.1

1.0

1.4

2-3

0 . 4

No.

obs.

9

57

65

63

48

39

*

14

9

18

26

22

8

412

Mean Hj

(km)

74.8

77-2

81.7

82.8

83.9

83.I

90.1

86.4

93-7

94.5

94.4

98.4

96.6

85.1

, S.d.

(km)

± 2.1

0.8

0.6

0 .6

0 . 7

1.1

0 . 8

1-3

1.9

1.2

1.1

1.4

2.0

0 . 4

NO.

obs

10

56

65

63

48

39

Jfc

14

9

18

26

21

8

411

TABLE 6.2.—Mean observed heights of Super-Schmidt meteors for groups of different mass

Maes range

( g )

0.01 - 0.05

0.05 - 0.10

0.10 - 0.20

0.20 - 0.40

0.40 - 0.80

0.80 - 1.60

1.60 - 5.0

5.0 - 34

All

Mean m

Cs> "

0.031

0.072

0.146

0.290

0.596

1.11

2.51

10.15

o.ao

S.d.

( g )

± 0.001

0.002

0.003

0.007

0.014

0.03

0.17

2.27

0.12

Meanly

(km)

109.2

104.4

100.2

98.8

95-1*

93-2

95.0

97-3

100.0

S.d.

(km)

± 0.8

1.0

0.7

1.0

1.1

1-3

1-5

2-5

0.4

No.

obs.

65

51

73

70

60

42

29

12

402

Mean H

(km)

110.3

104.2

99-4

98.1

94.6

92-5

94.5

95.6

99.6

(km)

± 0.9

1.1

0 . 8

1.0

1.2

1.4

1.7

2.5

0.5

No.

obs.

64

51

73

70

59

43

29

13

402

Mean R

(km)

100.1

94.9

90.8

88.7

85.O

83.3

82.4

78.1

89.8

S.d.

(km)

± 0.7

0 . 7

0 .6

0.6

0 . 6

0 . 8

1-3

1.8

0 . 4

No.

obs.

66

53

74

71

61

1*3

30

13

4 l l

Mean H

(km)

95-4

90.3

85.8

83.9

8O.7

79-0

77-1

70.9

85.I

, S.d.

(km)

± 0.8

0 . 7

0 . 5

0 . 6

0 . 6

0 . 7

1-3

2 . 4

0 . 4

N i .

obc.

(•(.

53

74

71

61

43

29

12

409
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 115

TABLE 7.1.— The position of maximum

light defined by . the parameter

TT TT

F = - — H

for Super-Schmidt

meteors

Group

All meteors

A meteors

S meteors

Southern Taurids

Geminids

Draconids

Mean F

0.65

0.36

0.48

O.69

0.72

0.55

S.d.

± 0.01

0.05

0.05

0.04

0.03

0.02

Ho. 0

400

26

12

17

19

2

TABLE 7.2.— The position of the maximum light defined

TT TT

by F = TT _TJ—» <w o function of velocity for SuperSchmidt meteors

Velocity range

(km/*)

10-20

20-25

25 - 30

30 - Uo

UO - 60

60 -7 3

All

Mean v^

(WO

17.2

22.U

27.U

34.0

48.2

65-5

35.1

Mean F

0.59

O.63

0.66

0.68

0.64

0.70

0.65

S.d.

± 0.03

0.02

0.03

0.02

0.02

0.02

0.01

No. obe .

64

65

62

86

70

53

400

TABLE 7.3.— The position of the maximum light, defined

TT TT

by F = „ _ „ » as a function of the ablation coefficient <r for Super-Schmidt meteors

Ablation coefficient range Mean log a Mean F

(cm"2 S)

-12.1 — -11.5

-11.5 - -11.3

-11.3 11.1

-11.1 - -10.9

-10.9 - -10.4

All

1 -2 2\

(em s )

-II.65

-11-37

-H.19

-11.01

-10.75

-11.17

0.64

0.73

O.67

0.6U

0.53

O.65

± 0.03

0.01

0.01

0.02

0.03

0.01

35

79

139

78

52

383

TABLE 7.4.— The position of the maximum light, defined

TT TT

by F = " _j^ < L ' <w a function of the fragmentation

index for Super-Schmidt meteors

Fragmentation index

range

X < 0

O s x < 0.1

0.1 £ x < 0.2

0.2 s x < O.3

0.3 s x < 0.5

x » 0.5

All

•feanx

-0.09

O.06

0.15

0.25

O.38

0.73

0.26

0.67

0.67

0.65

0.65

0.66

0.60

± o.oe

0.02

0.02

0.03

0.02

0.02

71

59

62

Ul

87

67

0.65 387

TABLE 8.1.—The ratio -jr^ of observed and theoretical durations and the mean

differences AH between observed and theoretical heights for Super-Schmidt meteors

Groups

All meteors

Sporadic meteors

Shower meteors

All - (A+S)

Sporadic - (A+S)

No. Mean

obs.

S.d. S.d.

)

S.d. tf^ S.4. iHj, S.d.

(tal> (k») (K.) (k.) U.)

384

273

111

348

245

Sporadic - (A+s), with Q « 6 a.u. I38

Sporadic - (A+s), with <J > 6 a.u. 107

A 2U

S 12

r 11

0.61

0.60

0.65

0.63

0.62

O.63

0.62

0.45

0.35

0.74

(km)

 w

± 0.01 -8.9 ± 0.4 -6.8 ± 0.4 -1.5 ± 0.2 0.9 ± 0.2

0.01 -9.0 0.5 -6.7 0.5 -1.6 0.2 1.0 0.3

0.02 -8.7 0.8 -7.0 0.8 -1-3 O.U 0.7 O.U

0.01 -8.3 O.U -6.3 O.U -l.U 0.2 1.1 0.2

0.01 -8.U 0.5 -6.2 0.5 -l.U 0.3 1.2 0.3

0.01 -7.1 0.6 -4.4 0.5 -2.0 0.4 1.0 0.4

0.01 -10.0 1.0 -8.6 1.0 -0.6 0.3 1.4 0.3

0.03 -14.3 1.1 -10.9 1-1 -3-0 0.8 -1.7 1-1

0.04 -15.5 2.7 -1^.3 2.5 -1-7 1-3 0.5 1-5

0.04 -9.9 1.4 -6.1 1.1 -2-6 I.3-1.O 1.8
10-2 0

20-3 0

30-4 0

40-5 0

50-6 0

60-7 3

All

17-3

25.0

33-9

44.2

56.1

65.O

35-0

O.58

0.68

0.68

0.60

0.59

O.56

O.63

0.4

0.5

0.6

0.9

0.5

0.2

1)3

76

3

a

21

44

34H

1 1 6 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 8.2.— The ratio yf^ of observed and theoretical durations and the mean

JLJth

differences AH between observed and theoretical heights for all Super-Schmidt

meteors minus (A+S), as functions of velocity

Velocity range Mean v^ Mean g ^ S.d. AHg S.d. iHg^ S.d. tjX^ S.d. AIL, S.d. Ho^^

(km/s) (km/s)

 t h

± 0.02 -7.8 ± 0.8 -4.7 t 0.6 -2.7 ± 0.6 0.9 ± 0.6 55

0.02 -4.9 0.6 -2.9 0.5 -0.5 0.3 2.2

0.02 -8.2 0.7 -5-7 0.7 -1-7 0.5 0.2

0.02 -9-2 1.1 -7-8 0.9 -0.6 0.5 0.9

0.03 -11.4 2.3 -10.9 2.5 -1-3 1-0 1.0

0.02 -15.4 1-9 -14.8 1.8 -2.0 0.6 0.1

.0.01 -8.3 0.4 -6.3 0.4 -1.4 0.2 1.1

D

TABLE 8.3.— The ratio ^r^ of observed and theoretical durations and the mean

Dth

differences AH between observed and theoretical heights for all Super-Schmidt

meteors minus (A+S) as functions of mass

>.d. ^r i S.d. AH C S.d. AfL. S.d. AH^, S.d. No.

obB.

0.61 ± 0.01 -8.5 ± 0.7 -7.2 ± 0.6 -1.0 ± 0.4 1.1 ± 0.4 98

0.02 -6.3 1.1 -4.8 1.1 -0.7 0.4 1.4 0.5 64

0.02 -8.9 1.2 -6.8 1.2 -2.1 0.4 0.4 0.5 76

0.02 -7.7 0.7 -5-3 0.7 -1-5 0.5 1.4 0.5 84

0.05 -11.2 1.9 -7-3 1-8 -1.9 1-3 1-2 1.3 13

0.05 -I3.6 3.5 -9.6 3.0 -2.0 1.1 0.4 1.6 13

0.01 -8.3 0.4 -6.3 0.4 -1.4 0.2 1.1 0.2 348

TABLE 8.4.— The ratio-^r^ of observed and theoretical durations and the mean

•L'th

differences AH between observed and theoretical heights for all Super-Schmidt

meteors minus (A+S), as functions of the ablation coefficient <r

Range of log o Mean log r Mean jp ^ S.d. AH_ S.d. AH S.d. AHJ- S.d. AIL, S.d. N).

/„ -2 2. , -2 2> th * * ' obs.

ITM s ) (cm s )

-12.05, -11.45 -11.60 0.70 ± 0.03 -7.0 ± 1.3 -5.3 ± 1.2 0.0 ± 0.6 1.9 ± 0.6 42

-11.45, -11-30 -II.36 0.70 0.02 -5.1 0.8 -3.8 0.7 0.2 0.3 2.8 0.4 68

-II.30, -11.15 -11.22 O.65 0.01 -6.3 0.7 -4.4 0.7 -0.3 0.3 2.3 0.3 01

-11.15, -11-0 -11.08 0.60 0.02 -9.0 0.7 -6.8 0.6 -2.2 0.4 0.4 0.4 80

-11.0, -10.40 -IO.83 O.55 0.02 -14.1 1.3 -11.6 1.3 -4.2 0.5 -2.1 0-5 67

All -11.22 O.63 0.01 -8.3 0.4 -6.3 0.4 -1.4 0-2 1.1 0.2 348

Mas

0.01

0 . 1

0 . 2

0 . 5

2 . 0

5.0

All

s range

(g)

- 0.1

- 0.2

- 0.5

- 2.0

- 5-0

- 34

Mean m

(g) "

0.05

0.15

O.32

1.29

3-28

10.15

0.86

0.61

O.67

O.65

O.63

0.58

0.66

0.6^!
ATMOSPHERIC TRAJECTORIES OP 413 METEORS 11 7

TABLE 8.5.— The ratio r=^ of observed and theoretical durations and the mean

Dth

differences AH between observed and theoretical heights for all Super-Schmidt

meteors minus (A+S), as functions of the fragmentation index x

D

Range of x Mean x *a n S.d. filL S.d. AH S.d. AR_ S.d. AH S.d. So.

th

 2 ° ML T ob£._

X < 0 -0.11 0-72 ± 0.02 -6.8 ± 0.9 -5.2 ± 0.9 -0.6 ± 0.4 0.9 -i 0.4 (.3

0 i x < 0.2 0.09 O.69 0.01 -6.9 0.6 -5.0 0.5 -0.9 O.U 1.2 o.U 110

0.2 s x < 0.4 0.30 0.62 0.02 -9.4 1.2 -7.1 1.1 -1.8 0.4 1.2 0.5 86

0.4 s x < 0.6 0.48 O.54 0.02 -10.8 1.3 -9.2 1.4 -2.2 0.6 0.9 0.^ 45

X a 0.6 O.87 0.52 0.02 -9.2 1.1 -7.1 1.0 -2.0 0.7 1.0 0.8 44

All 0.24 O.63 0.01 -8.3 0.4 -6.3 0.4 -1.4 0.2 1.1 0.2 348

TABLE 8.6.—The ratio -.

ob* of observed and theoretical durations and the mean

•L»th

differences AH between observed and theoretical heights for all Super-Schmidt

meteors minus (A+8), as functions of the brightness ea

D t

S.d. iHg S.d. AH2_5 S.d. AH^ S.d. aHj. S.d. M.i.

±0.03 -4-8 ±1.1 -2-5 ±0.9 -2.1 ±0.9 1.2 ±1.0 23

0.02 -4-3 0.6 -2.4 0.5 -1.0 0.5 1.9 0.5 '3

0.02 -6.0 0.6 -4.0 0.5 -0.9 0.4 1.7 0.4 34

0.02 -9.0 0.7 -7.1 0.7 -1.3 0.4 0.8 0.5 -'7

0.03 -9.0 1.0 -7.3 1.0 -1.3 0.5 1.0 0.5 52

0.03 -12.9 1.4 -10.6 1.5 -1.9 0.6 0.5 0.7 40

0.05 -21.8 3.9 -19.8 3.7 -3.1 1.0 -2.2 1.2 10

0.01 -8.3 0.4 -6.3 0.4 -1.4 0.2 1.1 0.2 346

TABLE 9.—A log p0Orr as a function of aphelion distance Q (*=hannonic mean)

rlghtne

-1.4,

-1.0,

-o-75,

-0.50,

-0.25,

0,

0.50,

All

ss range

-1.0

-0.75

-0.50

-0.25

0

0.50

2.0

Mean e^

-1.14

-0.86

-0.64

-0.39

-0.14

0.18

O.78

-0.41

Mean?

0.62

O.67

O.63

0.61

O.67

0.61

O.63

O.63

Range

(a..

0 -

3 -5 -

4.2 -

4.8 -

5.4 -

7-0 -

20 -

70 -

of Q

I.)

3-5

4 . 2

4 . 6

5-4

7.0

20

70

Mean Q

(a.u.)

2-9

3.8

4.6

5.0

5-9

12

j4

312*

A lo g p corr

-0.066

-0.054

-0.025

0.018

0.054

O.O58

0.021

0.021

S.d.

± O.O36

0.034

0.037

0.031

O.03I

0.027

O.O33

0.041

No. .

47

44

48

43

42

41

51

34

350
118 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 10.1.—A log pj»r as <* function of vm, the

velocity at the point where the mass of the meteor is

reduced to half its original value

TABLE 11.1.—Values obtained by least squares of the

coefficients of the equation Mpm = k0+k, (log vm —

6471)+k, (log ma+0.588)+k3 (log cos Z R +

0.2) for Super-Schmidt meteors

15-5

19-7

23-3

26.2

30.0

3 ^ 3

42.0

49.1

60.4

68.5

All: 29.".

0.017

-0.008

0.001

0.028

0.016

-0.008

0.029

-0.028

-0.061

-0.022

0.000

± 0.041

0.037

0.042

0.032

0.025

0.044

O.O32

0.055

O.O33

0.047

0.012

37

47

35

3

1

*

50

28

31

27

3

1

*

27

350

TABLE 10.2.—A log ftm as a function of the height

H corresponding to individual decelerations

Height range

(km)

50-7 5

75-8 0

80-8 4

84-8 6

86-8 8

88-9 0

90-9 2

92 - 95

95 - 99

99 -114

All

Mean height

72.6

78.2

82.3

85.O

87.O

89.O

91.1

93-5

96.7

103.2

90.1

i log o*

-0.26

-0.18

-0.08

-U.03

0.02

0.04

0.05

0.07

0.04

0.03

0.00

± 0.03

0.03

0.02

0.02

0.02

0.02

0.02

0.01

0.02

0.02

44

88

145

110

105

99

125

165

ne

15c

1149

TABLE 10.3.—A log /&„ as a function of H, the

average for each meteor of the heights for which decelerations were determined

Height range

(fan)

72 -

80 -

84 -

86 -

88 -

90 •

92 •

94 -

99 •

103 •

• 80

• 84

• 86

• 88

• 90

• 92

• 94

• 99

• 103

- 114

Mean height H

(km)

76.9

82.3

84.8

87.O

89.1

91.0

92-9

96.1

100.9

106.1

Meai1 fi log 0*

-0.28

-0.04

-0.06

0.01

0.06

0.06

0.04

0.04

0.07

-0.01

0.05

0.04

0.05

0.05

0.04

0.02

O.03

0.03

0.04

O.03

17

32

26

31

33

^3

42

52

35

39

All meteors

0.07 ± 0.02

-8.44 ± 0.16

-2.19 t 0.05

-1.45 ± 0.13

411

Sporadic mete

0.05 ± 0.03

-8.57 ± 0.21

-2.24 ± 0.06

-I.56 -t 0.17

289

k

o

" l

k

2

k

3

No.

All meteors minus

(A + S + D)

0.12 t 0.02

-8.68 i 0.15

-2.22 ± 0.04

-1.52 ± 0.13

obs. 367

Sporadic meteors minus

(A + S + D)

0.12 * 0.02

-8.84 i 0.19

-2.31 i 0.06

-1.55 t 0.16

246

TABLE 11.2.— Values obtained by least squares of the

coefficients of the equation: Mp m =ko+ki (log vm —

6.477)+ k, (log ma + 0.52S) + k, (log cos ZK+0.2)

for particular groups of Super-Schmidt meteors

Sporadic meteorc

minus (A + S + D)

with X < 0.2

(Mean x = 0.05)

0.21 ± 0.04

-9.01 ± 0.29

-2.30 ± 0.08

-1.81 ± 0.25

bs. 124

Sporadic meteors

minus (A + S + D)

with log ci < -11.40

(Mean log n = -11.55)

kQ 0.52 ± 0.08

kx -10.19 ± 0.43

Kg -2.22 ± 0.08

kj -2.02 ± O.27

No. obs. 36

Sporadic meteors

minus (A + S + D)

with x > 0.2

(Mean X = O.49)

0.02 ± 0.03

-8.83 ± 0.25

-2.41 ± 0.08

-1.40 ± 0.22

114

Sporadic meteors

minus (A + S + D) with

-11.40 fi log a £ 11.00

(Mean log o = -U.19)

0.15 ± 0.03

-9.46 ± 0.25

-2.41 ± 0.07

-1.67 ± 0.20

155

Sporadic meteors

minuD (A + S + D)

with log cr > -11.00

(Mean log a - -ID.86)

0.01 ± 0.06

-8.71 ± 0.42

-2.59 ± 0.14

-1.64 ± 0.32
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 119

TABLE 11.3.— Values obtained by least squares of the

coefficients of the equation: Mp m =ko+ki (log v M -

6477)+k, (log mw+0.68S) + k8 (log cos ZK+0.0)

for short- and long-period Super-Schmidt meteors

*2

No.

Sporadic meteors minus

(A + S + D) with

Q s 6 a.u.

0.20 ± 0.05

-7.82 ± 0.1*3

-2.il* ± o.lO

-1.13 ± 0.28

>bs. 133

Sporadic meteors minus

(A + S + D) with

Q > 6 a.u.

0.16 ± 0.03

-9->*5 ± 0.21

-2.1*2 ± 0.05

-1.82 ± 0.15

113

TABLE 11.4.—Values obtained by least squares of the

coefficients of the equation: Mp m =ko+k1 (log vm —

6.477) +k, (log ma>+0.6£S)+kl (log cos ZR+0.« )

for smaU-camera meteors

All meteors

0.08 -t O.ll*

-10.00 i 0.37

-2.1*6 ± 0.07

-1.90 -t O.U3

207

Sporadic meteor

-0.18 ± 0.21

-9-37 ± O.55

-2.27 ± 0.12

-2.03 ± O.63

85

k

o

\

k

2

No.

Meteors with flares

-0.25 ± 0.26

-10.29 ± 0.58

-2.53 ± 0.12

-1.79 ± O.78

obs. 80

Meteors without

-0.25 ± 0.12

-8.73 ± 0.31*

-2.02 ± 0.07

-1.67 ± O.35

127

TABLE 11.5.—Values obtained by least squares of the

coefficients of the equation: Mp m =ko+ki (log va —

6.477)+kt (log ma>+0.52S)+k, (log cos Z^+0.2)

for Super-Schmidt meteors minus (A+S+D) and nonflaring small-camera meteors

kQ = 0.10 ± 0.02

v^ = -8.93 ± 0-12

k£ = -2.25 ± 0.03

1*91*

TABLE 11.6.—Comparison between the values of ku kt,

kj of the general solution (see tables 11.1 and 11.4)

and the values of kt and kj when kj is assumed a

priori equal to —2.6

SUPER-SCHMIDT METEORS

ALL METEORS

sneral Solutlo

-8.1*1* ± 0.16

-2.19 * 0.05

-1.1*5 ± 0.13

oa. 1*11

oiutlon with k

-8.63 * 0.17

-2.21 i 0.05

-2.5

1*11

SPORADIC METEORS

"3

No. obs.

neral Solutio

-8.57 ± 0.21

-2.2>* ± 0.06

-1.56 1 0.17

Solution with k. « -2.5

-8.83 + 0.21

-2.29 ± 0.07

-2-5

289

SMALL-CAMERA METEORS

k

l

k

2

k

3

No.

k

l

k

2

No.

General

-10.00

-2.1*6

-1.90

obs.

General

-9.37

-2.27

-2.03

obs.

Solution

+ 0.37

± 0.07

± 0.1*3

207

-10.06

-2. .1*7

SPORADIC METEOR';

Solution

+ 0.55

± 0.12

± O.63

85

Solution

-9.

-2.

.50

.30

with

i 0.

k3 - -2.

.36

± 0.07

-2.5

207

with

t 0.

± 0.

-2.5

85

k, - -2.

52

,11

TABLE 12.—The mass (in g) of a zero visual magnitude

meteoroid as a function of velocity vw and zenith

angle ZR

0°

30°

1*5°

60°

75°

85°

120

132

151

191

269

617

8.13

8.91

10.2

12.9

18.2

1*1-7

1.66

1.82

2.09

2.63

3-72

8.51

0.55

O.63

O.69

O.87

1-23

2.82

O.23

0.25

0.29

O.36

0.51

1.17

0.11

0.12

0.11*

0.18

0.25

O.58

0.062

0.068

0.078

0.098

0.11*

0.32
120 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

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ATMOSPHERIC TRAJECTORIES OF 413 METEORS 121

TABLE 13.5.—The absolute photographic magnitude as a

function of mass for small-camera meteors (MTM is

the observed magnitude reduced to on=40 km/s

and cos Z«=10-°J=0.631.)

TABLE 13.6.— The absolute photographic magnitude as a

function of the zenith angle ZR for small-camera meteors

(ilf^*1 is the observed magnitude reduced to mm —10

gand va0=40km/8.)

Mass

(i

0.04

1.6

5.0

15

5P

150

All

range

s)

- 1.6

- 5-0

- 15

- 50

- 150

- 3600

Mean c

O.78

3.O3

9-1

29-0

102

811

82

n

l i

-t

i

i

i

±

i

i

i s.d.

0.05

0.15

0 . 5

2 . 1

6

232

24

Mean M

-3-1 i

-3-5 i

-4.3 i

-4.8 ±

-6.0 i

-6.7 i

-4.2 ±

n * s-d -

0.2

0.2

0 . 3

0.3

0-5

0.6

0 . 1

Mean W '

pro

-2.02 ±

-3-53 -t

-4.72 ±

-5-89 ±

-7-48 ±

-8.48 i

-4.31 ±

0.14

0.12

0.13

0.15

0.27

0.45

0.17

No. obs.

65

46

36

23

20

17

207

Range of cos Z_

0.0 - 0.3

0.3 - 0.4

0.4 - 0.5

0.5 - 0.6

0.6 - 0.7

0-7 - 0.8

0.8 - 0.9

0.9 - 1.0

All

Mean

0.26

O.33

0.47

O.56

0.66

0-75

O.85

0.95

O.76

c

i

*

t

i

+

4.

i

i

OS Zj^

0.02

0.01

0.01

0.01

0.01

0.01

0.01

0.00

0.01

Mean 1

-6. 1

-3-2

-4.5

-4.8

-4.1

-4.2

-4-3

-3-7

-4.2

V

±

±

±

•t

•t

i

4.

1.1

0.4

0 . 9

0.5

0-5

0.3

0-3

0.2

0 . 1

Mean M

-3-87

-4.17

-5.03

-4.86

-4.94

-5.16

-5-19

-5.19

-5.05

pm

t

*

±

±

*

*

± s.d.

0.28

0.15

O.52

0.13

0.18

0.12

0.11

0.10

0.06

Ho. c

4

8

7

20

20

y

y

%

207

TABLE 14.1.— The difference AMDin between observed

and theoretical absolute magnitudes for Super-Schmidt

meteors

All mete

Sporadic

Sporadic

Sporadic

Sporadic

Sporadic

Sporadic

Sporadic

Sporadic

(A + S + D)

•teors vitfc Q. -: '- a.u.

•tcors with Q > c a.u.

?teors minus (A + S + D) with x

 s 0.2

•teors minus (A + S + D) with X > 0.2

;teors minus (A + S + D) with log o < -11.4

iteors minuc (A + S + D) with -11.4 i log o s -11.0 -Q-%' * 0.03

Sporadic meteors minus: (A + S + D) with log a > -11.0 -O.83 ± 0.07

Individual Showers

•M

Quadrant ids

Virginids

Lyrids

T, Aquarids

'. Aquarids

a Capricornids

-0.59 t 0.05

-O.38 4- 0.28

-0.19 i 0.15

-0.55

-0.91 * 0.08

-O.65 + 0.09

i s.d . No. ols,

9 K Cygnids

DraccnidE

Orionids

Southern 1

Northern 1

Leonidr

Mean AM ± s.d.

pra

-0.61 ± 0.03

-0.66 ± 0.03

-0.50 t 0.05

-O.58 ± 0.03

-0.7' i 0.05

-O.53 ± 0.03

-0.47 ± 0.04

-0.71 t 0.04

-0-3' ± 0.06

Southern L Aquarid;; -C.V5 ± D-28

northern i. Aquarids -0.1*3 i 0.14

Perseids -0.3C t C.18

Mean 4M ±5 .

pm

-0.77 * C.13

-2.<7 * 0.43

-0.42 ± C.ll

rids -0.15 i 0.05

rids -0.0° -i 1.03

-0.03 t 0.13

-0.33 t C.OJ:

278

117

23'

159

119

123

112

3t

154

46
122 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 14.2.— The difference AMDm between observed

and theoretical absolute magnitudes for small-camera

meteors

TABLE 14.3.— The difference AMpm between observed

and theoretical absolute magnitudes as a Junction of x

for sporadic Super-Schmidt meteors

Mean AM ± s.d.

Range

All meteors

Sporadic meteors

Shower meteors

Flaring meteors

Honflaring meteor

Lyrids

Perseids

Southern Taurids

Northern Taurids

X Orionids

Geminids

-0.63

-0.61*

-O.63

-I.03

-0.30

-0.04

-0.83

-0.92

-O.65

-0.99

-O.3O

±

i

±

±

i

±

i

±

±

*

±

0.08

0.10

0.13

0.11

0.09

0.26

0.25

0.31

0.06

0.28

0.23

90

42

48

41

49

3

6

13

2

3

15

x < 0

0 s x < 0.1

0.1 <; x < 0.2

0.2 <; x < 0-3

0.3 s x < 0.4

0.4 <, x < 0.6

X 2 0.6

All

-0.10 i 0.02

0.04 ± 0.00

0.14 ± 0.00

0.24 i 0.00

0.34 t 0.00

0.48 i 0.01

0.88 ± 0.07

0.27 ± 0.02

-0.1 ± 0.2

0.1 ± 0.2

0.1 ± 0.1

-0.1 ± 0.3

0.4 ± 0.2

0.2 ± 0.2

0.4 ± 0.4

0.1 4 0.1

-0.50

-0.46

-0.62

-0.68

-0.74

-0.76

-0.97

-0.66

i

*

i

i

i

t

i

0.0'

0.07

0.08

0.08

0.07

0.07

0.0"

0.03

48

"*3

49

35

36

33

37

281

TABLE 15.1.— The color index C.I. as a function of

velocity for Super-Schmidt meteors

Velocity

10 -

20 -

30 -

40 -

60 -

All

range

20

30

40

60

73

Mean

(W

17-

2 4 .

34.

4 8 .

65.

35-

sf

2

8

1

4

5

3

Mean c.

-1.29

-1-39

-1.49

-1.34

-I.30

-1-37

1 .

±

±

±

±

±

±

± s.d.

0.10

0.07

0.07

0.09

0.11

0.04

NO. OD!

62

125

79

71

53

390

TABLE 15.2.—The color index C.I. as a function of the

maximum photographic magnitude Mpm for SuperSchmidt meteors

Magnitude range Mean M

(absolut e photographic )

 p i

-6.0

-1-3

-0.6

-0.1

0 . 4

0 . 9

1.4

All

t o

t o

t o

t o

t o

t o

t o

-1-3

-0.6

-0.1

0 . 4

0 . 9

1.4

2.5

-2.18

-0.96

-0.39

0.11

0.63

1.18

I.83

0.02

-1.93

-1.77

-1.49

-1-33

-1.16

-0.97

-1.00

-1.37

*

*

i

*

±

i

±

±

0.11

0.09

0.10

0.09

0.08

0.08

0.10

0J04

48

58

60

57

66

63

38

390

The distribution of the color index C.Lfor seven magnituie groups.

-4.0 to -3.3

-3-3 to -3.0

-3.0 to -2.7

-2.7 to -2.4

-2.4 to -2.1

-2.1 to -1.8

-1.8 to -1.5

-1.5 to -1.2

-1.2 to -0.9

-0.9 to -0.6

-0.6 to -0.3

-O.j to 0.0

0.0 to O.j

n.j to 0.6

All

-4.0 to -3.3

-3-3 to -3.0

-3.0 to -2.7

-2.7 to -2.4

-2.4 to -2.1

-2.1 to -1.8

-1.8 to -1.5

-1.5 to -1.2

-1.2 to -0.9

-0.9 to -0.6

-0.6 to -0.3

-0.3 to 0.0

0.0 to 0.3

0.3 to 0.6

AU

63
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 123

TABLE 16.1.—The distribution of the

Range of log c

-12.10 12.01

-12.00 11.91

-11.90 11.81

-11.80 11.71

-11.70 11.61

-11.60 11.51

-11.50 11.1*1

-11.1*0 11.31

-II.30 11.21

-11.20 11.11

-11.10 11.01

-11.00 10.91

-10.90 10.81

-10.80 — -10.71

-IO.7O 10.61

-10.60 10.51

-10.50 — -10.1*1

All

ablation

a for Super-Schmidt meteors

All

1

1

2

0

6

8

18

30

50

k3

39

21

15

1*

3

1

0

21*2

Sporadic

Q < 6 a.

1

0

0

0

2

2

6

11

26

27

28

15

12

3

2

1

0

136

meteors

u. 0. > 6 a.u.

0

1

2

0

1*

6

12

19

21*

16

11

6

3

1

1

0

0

106

Shover nw

c

0

2

1*

1

12

25

10

u.

12

3

5

3

0

0

1

106

coefficient

steors All meteors

1

1

1*

k

7

11*

30

55

66

59

51

21*

20

7

3

1

1

31*8

TABLE 16.2.—The distribution

Range of log o

-12.30 to -12.21

-12.20 to -12.11

-12.10 to -12.01

-12.00 to -11.91

-11.90 to -11.81

-11.80 to -11.71

-II.70 to -11.61

-11.60 to -11.51

-11.50 to -11.1*1

-11.1*0 to -II.3I

-II.30 to -11.21

-11.20 to -11.11

-11.10 to -11.01

-11.00 to -10.91

-10.90 to -10.81

All

of the abla

for smaU-camera meteors

Sporadic meteors

0

0

2

2

0

1*

1

7

2

1*

1*

6

1*

1*

1

1*1

Shover net

1

1

2

3

6

9

5

7

3

3

3

2

2

0

0

hi

TABLE 17.1.1.—The ablation coefficient o as a function

of the velocity vm for sporadic Super-Schmidt meteors

having, respectively, Q <6 a.u. and Q ><? a.u. (classes

A and S excluded)

Range of v

(km/s) "

10-2 0

20-2 5

25 - 30

30 - 35

35 - 1*0

uo - 50

50-6 0

60-73

Mean v

17.2

22.3

27-3

32.2

36-5

1*2.0

Q £ 6 a.u.

Mean log c

(cm"2s

2

-11.05 ±

-11.12 ±

-11.17 ±

-11.22 ±

-II.38 ±

-11.1*6 ±

± s.d.

0.03

0.03

0.03

0.01*

0.11*

0.20

No.obs•

1*8

37

26

17

6

2

Mean v

18.1

22.3

27.2

31.7

37.7

1*5.6

55-8

65.6

Q> 6 a

Mean log

-11.01*

-11.11*

-11.21

-11.20

-11.20

-U.32

-11.32

-11.35

.u

±

±

±

i

±

±

0.08

0.06

0.07

0.05

0.08

0.06

o.oi*

0.01*

6

8

10

11

6

19

16

30

23.6 ± 0.6 -11.ll* i 0.02 136 1*5.8 ± 1.6 -11.27 ± 0.02
124 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 17.1.2.—The ablation coefficient a as a function of the velocity for Super-Schmidt meteors {classes A and S excluded)

Velo

C

11

20

25

30

35

1*0

50

60

city range

taa/s)

- 20

- 25

- 30

- 35

- 1*0

- 50

- 6o

- 73

A10.

Mean v^

17-3

22.6

27.3

31.7

36.6

1*1*.2

56.2

65.1

35.0

Mean lot!

(c^s 2)

-11.05

-11.12

-11.19

-11.27

-11.26

-11-35

-11.33

-11.30

-11.22

All Met

S

of

±

eors

.d.

0.03

0.03

0.03

0.03

0.05

o.oi*

0.03

o.oi*

0.01

S.d. of

1 obs.

± 0.19

0.20

0.20

0.18

0.28

0.25

0.16

0.2l*

0.2U

Mean log

-11.00

-11.11

-11.18

-11.26

-11.25

-11.35

-11.33

-11.30

-11.20

0

0

±

±

±

±

±

±

±

±

±

± s.d.

•8 g)

0.02

0.03

0.03

0.03

0.05

o.oi*

0.03

o.oi*

0.01

No.

Obs.

5U

55

56

1*1*

31*

1*0

21

1*1*

31*8

Mean v^

17-3

22.3

27.3

32.0

37-1

1*5.2

55.8

65.6

33.1*

Mean loo; 0

I " 2 2^

-11.05

-11.12

-11.18

-11.21

-11.29

-11.33

-11.32

-11.35

-11.19

Sporadic Met

S.d.

± 0.03

0.03

0.03

0.03

O.08

0.05

o.oi*

o.oi*

0.02

eors

S.d

1 0

± 0.

0 .

0 .

0 .

0 .

0 .

0 .

0 .

0 .

. of

b s.

19

19

19

17

28

25

16

21*

23

Mean log

-11.00

-11.11

-11.17

-11.20

-11.28

-11.33

-11.32

-11.35

-11.18

0

±

±

±

±

±

t

±

±

± s.d.

•8 6)

0.02

0.03

0.03

0.03

0.08

0.05

O.Ol*

o.oi*

0.02

Ns

Obs

5U

1*5

36

28

12

21

16

30

2U2

TABLE 17.2.— The ablation coefficient a as a function of the integrated brightness «„ for Super-Schmidt meteors (classes

A and S excluded)

All Meteors Sporadic Meteoro

All Q < 6 a.u . Q > 6 a.u.

Range of e._ Mean e_ Mean loo; - S.d. S.d. of No. Mean ,- Mean log i S.d. S.d. of No. Mean log 3 S.d. No. Mean log a S.d. No.

/ -2g 2j 01 mean 1 obs. obs. * tcm2

e

2

) ° r ">ean 1 obs. obs. (Cra2

S

2N obs. ( cra -a

,.2, obs.

-1.1*0 to -1.00 -l.ll* -11.ll* ± 0.05 ± 0.25 23 -l.ll* -11.05 * 0.05 ± 0.19 16 -11.03 * 0.05 I1* -11.15 *• 0.22 2

-0.99 to -0.75 -O.85 -11.17 0.03 0.25 65 -O.85 -11.17 O.olt 0.26 1.8 -11.lit O.Ol* 36 -11.21* 0.08 12

-0.71 to -0.50 -O.63 -11.21 0.03 0.25 81 -0.61* -11.18 0.03 0.21 57 -11.12 0.03 37 -11.30 0.05 20

-0.1-9 to -0.25 -0.39 -11.20 0.03 0.22 66 -O.38 -11.18 0.03 0.23 1*6 -11.10 0.05 19 -11.23 O.Ol* 27

-0.21. to 0.03 -O.lU -11.29 0.02 0.17 53 -O.llt -11.30 0.03 O.l8 33 -11.30 0.06 11 -11.31 O.Ol* 22

0.01 tc 0.50 3.19 -11.19 0.03 0.20 39 0.18 -11.18 0.0't 0.19 29 -11.ll* 0.05 15 -11.21 0.05 ^

3.51 to 1.03 O.67 -11.33 0.06 0.26 18 O.65 -11.31 0.07 0.21* ij -11.32 0.08 1* -11.31 0.10 8

1.01 to 2.00 1.35 -11.67 0.10 0.18 3 1.91 -11.88 — — 1 _ -- _ -11.88 — 1

All -0.1-1 -11.216 0.013 0.235 31*8 -0.1*2 -H.I9IJ 0.015 0.229 21*2 -11.135 0.018 136 -II.267 0.021* 106

TABLE 17.3.—The ablation coefficient a as a function of the initial mass m,,, for Super-Schmidt meteors (classes A and

S excluded)

Range

0.01

0.05

0 . 1

0 . 2

o.i.

0 . 8

1.6

5.0

All

(I) m'"

- 0.05

- 0.1

- 0.2

- O.U

- 0.8

- 1.6

- 5.0

- 31

; Mean m

(i) "

0.033

0.072

0.11*5

O.29I*

O.591*

1.122

2.59

10.15

0.66

i

t

i

t

±

±

±

0.002

0.002

0.003

0.0O8

0.016

0.039

0.20

2.27

0.13

All Mr-te

Mean loe n

(en' 2/ ) 0

-11.31

-11.32

-11.23

-11.15

-11.1U

-11.15

-11.21

-11.26

-11.22

i r s

s .a.

± 0.03

0.01.

0.02

0.02

o.oit

0.01*

0.05

0.09

0.01

S.d. of

1 obs.

1 0.2ll

0.25

0.17

0.18

0.27

0.21

0.21*

0.32

0.21*

Mean log o

K * 3°

-11.23 ±

-11.26 ±

-11.23 ±

-11.19 *

-11.23 ±

-11.29 ±

-11.32 ±

-11.1*3 ±

-11.25 ±

± s.d.

km/s)

0.03

0.03

0.02

0.02

0.03

0.03

o.oi*

0.08

0.01

No.

52

1*7

62

62

53

3t

25

13

3U8

0

0

0

0

0

1

2

10

1

Met

1

.032

.075

• 1U5

.30 6

.60 1

.11 6

.56

.15

• 05

in

Is.

±

±

±

i

±

±

±

r

0.002

0.003

o.oou

0.009

0.017

0.01*2

0.25

2.27

0.19

(cm-2s

2

)

-11.30

-11.35

-11.21

-11.16

-11.09

-11.12

-11.10

-11.26

-11.19

Sporadic

S. d.

of mean

± O.Olt

0.05

0.02

0.02

0.01*

0.01*

O.Olt

0.09

0.01

Meteor

S .d

± 0.

0 .

0 .

0 .

0 .

0 .

0 .

0 .

0 .

s

obs.

21*

25

15

ll*

26

19

16

32

23

Mean log

(•'„

 = 5 0

-11.18

-11.26

-11.20

-11.20

-11.16

-11.22

-11.22

-11.37

-11.21

a ± s.d.

km/s)

± O.Ol*

± 0.05

± 0.02

± 0.02

i O.OU

i 0.03

± 0.03

± 0.08

± 0.01

No

38

2lt

1.0

38

1*2

30

17

13

2l*2
ATMOSPHERIC TRAJECTORIES OF 413 METEORS 125

TABLE 17.4.—The ablation coefficient vat a function of velocity for small-camera meteors

Range of

(ta/s)

10 - 20

20 - 30

30 - ItO

Ho - 50

50-6 0

60-7 0

All

Mean vm * s.d.

(ta/s)

16.2 ± 0.9

25.9 * 0.6

3H.H ± 0.5

H5.5 ± 2.1

55-5 ± 1.9

61.6 ± 0.9

33.8 ± 1.3

Mean log c

(cm"2s

2

)

-11.2H

-11.Ha

-11.59

-11.53

-11.80

-11.70

-11.52

S.d.

of mean

± 0.07

0.06

0.06

0.09

0.13

0.06

0.03

S.d. of Mean log

1 obs. (0.8 g)

± 0.21

0.29

0.3H

0.17

0.29

0.15

0.32

-10.89

-11.09

-II.36

-11.32

-11.5H

-11.59

-11.26

Mean log a

(m « 110 g)

-11.3H

-11.5H

-11.81

-11.77

-11.99

-12 . OH

Ho

obs

9

27

36

H

5

7

TABLE 17.5.—The ablation coefficient a as a function of the initial mass for

small-camera meteors

Range

(s.

0 . 1

1.6

5

15

50

150

I "

- 1.6

- 5.0

- 15

- 50

- 150

- 2000

Mean m^ ± s.d.

(I)

0.77 ± 0.13

3.23 ± 0.30

9.63 ± 0.72

28.6 ± 2.6

107 ± 6

66H ± l&c

Mean log T

(c^s 2)

-11.37

-11.HO

-11.H6

-11.63

-11.68

-11.57

S.d.

of mean

± 0.11

0.07

0.06

0.07

0.08

0.12

S.d. of

1 obs.

± 0.3H

0.28

0.30

0.27

0.32

0.39

Mean log 0

-11.22

-11.32

-11.Hi

-II.63

-II.69

-11.67

Nc

obs

10

15

22

1H

16

11

TABLE 17.6.—The ablation coefficient a for shower meteors; Super-Schmidt (classes A andS excluded) and small-camera meteors

Shower

Quadrantids

Virginids

Lyrids

1 Aquarids

S Aquarids

a Capricomids

Southern 1 Aquaride

Northern t Aquarid?

Perseids

* Cygnids

Draconids

?rionids

Jthern Taurids

i 'rthem Taurids

i'.-onids

OriDnids

Hydrids

eminids

Jrsids

Mean

log 0

-11.1*8

-11.2H

-11.17

-11.01

-11.35

-11.09

-11.35

-11.1*8

-11.26

-11.07

-1H.8S

-11.12

-11.31

-11.Hi

-10.99

_

-11.H6

-11.23

S.d.

of mean

± 0.09

_

0.17

_

0.0H

0.08

0.11

0.25

0.06

0.08

0.79

0.05

0.03

0.0H

_

_

0.06

0.07

Super-Schmidt Meteors*

S.d. of

1 obs.

± 0.28

_

0.30

_

0.10

0.28

0.2H

0.35

0.19

0.16

1.12

0.10

0.11

0.08

—

_

0.10

0.29

Mean v

± s.d."

(Ws)

H3.0 ± 0.2

27.1

H8.8 ± 1.1

66.8

H2.1 ± 0.3

25.6 ± 0.H

3H.2 ± 1.2

35-9 * 1-7

60.3 ± 0.2

23.2 ± 0.H

20.2 ± 0.1

68.H ± 0.8

29.0 ± 0.H

30.9 * 0.3

71.7

_

59.2 ± 0.6

36.3 ± 0.1

_

Mean m

± s.d. "

(g)

0.09 ± 0.2

1.07

0.13 ± 0.0H

0.0H

0.10 ± 0.01*

0.53 ± 0.2H

0.10 t 0.02

0.11 ± 0.0H

0.30 ± O.lH

0.39 ± 0.06

2.00 ± 0.13

0.0H ± 0.01

o.ne ± 0.13

0.85 ± 0.35

0.29

_

0.05 ± 0.01

0.79 t 0.29

Mean log -,

(y^ = 30 km/s)

(»>„ - 0.8 g)

-11.35

—

~ -11.0

—

-11.23

-11.12

-11.33

—

-11.10

-11.lH

—

-IO.96

-11.31

-II.38

—

—

-11.31

-11.lH

—

No.

obs.

9

1

3

1

8

lH

5

2

9

H

2

I*

18

5

1

—

3

19

—

Mean

loi* c

(cm"2*

2

)

-

-11.25

-11.52

—

—

—

—

—

-11.77

-

—

—

-11.70

-II.U9

—

-11.HI*

-11.62

-11.69

-11.19

S.d.

cf mean

-

± 0.15

0.10

—

-

—

-

—

0.10

—

—

-

0.0H

0.23

—

0.23

0.03

0.09

—

S.

1

± 0

0

0

0

0

0

0

0

d.

ob;

.21

.17

.25

.16

.32

• 31-

.01-

.33

—

Small-C amera Meteors

3f Mean v. Mean ^

1. ± s.d. ± s.d.

30.9 ±0. 1 7 ± 3

H9.H ± 0.7 10 ± 8

6O.5 ± 0.H 29 ± 20

30.3 ± 0.6 11*9 ± 102

28.7 ± 1-5 99 * 65

30.9 * 0.7 136 ± 117

55.3 * H.3 1,6 ± 58

36.H t 0.1 95 i CO

35.2 7

log a

30 km/s)

11.0 g)

-11.1

, -11.0

-11. ;H

225-636 O-67— 9
126 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 17.7.— The ablation coefficient o as a function

of the initial matt mm;the observed values have been

reduced to a velocity of SO km/s; Super-Schmidt

(classes A and S excluded) and small-camera meteors

Mass n

(8)

0.01 -

0.05 -

0.10 -

0.20 -

0.1*0 -

0.8 -

1.6 -

5.0 -

15 -

50 -

150 -

A l l

»nge

0.05

0.10

0.20

0.1*0

0.80

1.6

5.0

15

50

150

2000

Mean mass

(g)

0.03 ±

0.07 ±

0.15 ±

0.29 ±

o.6o t

1.13 ±

2.83 ±

8.8 ±

28.1* ±

107 *

66U ±

22.9 *

± s.d.

0.00

0.00

0.01

0.01

0.02

0.01*

0.17

0 . 7

2 . 3

6

180

6.5

Mean loir -

-11.23 ±

-11.26 ±

-11.23 *

-11.19 *

-11.23 *

-11.30 t

-11.31 ±

-11.1*1 ±

-11.62 ±

-11.69 *

-11.67 *

-11.30 ±

± s.d.

0.03

0.03

0.02

0.02

0.03

0.03

o.oi*

0.05

0.06

0.08

0.12

0.01

No.

obs.

52

>*7

63

63

58

37

1*0

33

16

16

11

1*36

TABLE 17.8.— The ablation coefficient a as a function of the integrated brightness «„ for SuperSchmidt (classes A and S excluded) and small-camera meteors

Rang*

-1.1*0

-0.99

-0.7U

-0.1*9

-0.2"*

0.01

0.51

1.01

1.51

2.01

2.51

All

• ° f S,

-1.00

-0.75

-0.50

-0.25

0.00

0.50

1.00

1.50

2.00

2.50

3.1*0

Super-Schmidt Meteors

Mean tm

-l.ll*

-O.85

-O.63

-0.39

-O.lU

0.19

O.67

1.08

1.91

-

-

-0.1*1

Mean log J

(cm^s 2)

-11.1U

-11.17

-11.21

-11.20

-11.29

-11.19

-11.33

-11.57

-11.83

-

-

-11.22

obs.

23

65

81

66

53

39

18

2

1

-

-

3ue

Small-Camera Meteo:

-

-

-0.66

-

-

0.31

0.81

1.21

1.76

2.2U

3.03

l."*3

Mean log e

(c^s2)

-

-

-11.05

-

-

-11.28

-11.3k

-11.1*8

-11.6U

-II.78

-11.76

-11.52

rs

No.

obs.

-

-

1

-

-

11

1U

21*

16

10

8

8U

Mean ea

-1.1U

-O.85

-0.63

-0.39

-O.lU

0.22

0.73

1.20

1.77

2.2U

3.03

-0.05

All Cameras Mete

Mean log n

(cm"2s

2

)

-11.11*

-11.17

-11.21

-11.20

-11.29

-11.21

-11.3".

-11.1*9

-11.66

-11.78

-11.76

-11.28

S.d.

± 0.05

0.03

0.03

0.03

0.02

0.03

0.04

0.05

0.06

0.09

0.15

0.01

o rs

S.d. of

1 obs.

± 0.25

0.25

0.25

0.22

0.18

0.23

0.25

0.21*

0.23

0.27

0.1*1*

0.28

No.

obs.

23

65

82

66

53

50

32

26

17

10

8

1*32
NO. i ATMOSPHERIC TRAJECTORIES OF 413 METEORS 12 7

TABLE 17.9.— The ablation coefficient a as a function of the zenith angle cos ZH for Super-Schmidt

meteors (classes A and 8 excluded)

ge of cos 2^

0.1 - 0.2

0.2 - 0.3

0.3 - 0.1*

0.U - 0.5

0.5 - 0.6

0.6 - 0.7

0.7 - 0.8

0.8 - 0.9

0.9 - 1.0

Mean cos Z.

0.11*0

0.253

0.351

0.1*61

0.555

0.6U8

0.751

O.8U3

O.969

All Mete

^ Mean log -

-11.12

-11.21

-11.21

-11.23

-11.26

-11.23

-11.19

-11.20

-11.22

E.d.

of mean

0.10

0.06

0.05

o.oi*

O.OU

0.03

0.03

0.03

O.OU

E.d. of

1 obs.

0.18

0.18

0.28

0.21

0.19

0.2U

0.26

0.20

0.26

Ho.

obs.

3

9

28

32

29

76

70

61

uo

Mean cos Z

0.133

0.250

0.356

O.U59

O.5U9

O.6U9

0.751*

0.8U1

0.963

Spoi

Mean log -

(c'V)

-11.08

-11.21

-11.19

-11.23

-11.23

-11.19

-11.18

-11.18

-11.19

radio Meteor

S.d.

of mean

0.17

0.07

0.07

O.OU

O.OU

0.03

0.0U

0.03

0.05

'S

S.d. of

1 obs.

0.2U

0.19

O.32

0.20

0.16

0.2U

0.2U

0.21

0.25

Ho

obs

2

8

20

26

18

52

U7

U6

23

O.677 -11.216 0.013 0.235 31* 0.666 -U.19U 0.015 0.229 2U2

TABLE 17.10.—The ablation coefficient * as a function of the

aphelion distance Q for sporadic Super-Schmidt meteors (classes A

and 8 excluded) (•=harmonic mean)

Range of Q

(a.u.)

0.9 - 3-5

3-5 - U.2

U.2 - U.8

U.8 - 5.U

5.U - 7-0

7.0 - 20

20-7 0

70 - -

All

Mean Q

2.65

3-90

U.56

5.09

6.01

11.63

36.18

1U03*

Mean log -

(CB-V)

-11.12

-11.11

-11.10

-11.18

-11.18

-11.27

-11.31

-11.27

-11.19

S.d.

of mean

± O.OU

O.OU

O.OU

O.OU

0.03

O.OU

O.OU

0.05

0.02

S.d. of

1 obs.

± 0.23

0.23

0.19

0.23

0.15

0.22

0.2U

0.2U

0.23

Mean log a

{ym - 30 ta/s)

-11.20

-11.23

-11.22

-11.26

-11.23

-11.17

-11.21

-11.17

-11.21

Ho.

obs.

32

29

30

30

29

35

32

25

2U2
2 2 8 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 17.11.1.—The ablation coefficient v as a function of the perihelion distance q for

Super-Schmidt meteors (classes A and S excluded)

VOL. 10

Range

(a.,

0.0 -

0.1 -

0.2 -

0.3 -

0.4 -

0.5 -

0.6 -

0.7 -

0.8 -

0.9 -

1.0 -

of q

••)

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

1.0

1.1

Mean q

(a.u.)

0.08

0.14

0.25

0.35

0.46

0.55

0.66

0.74

O.85

O.96

1.01

All Meteors

Mean log a

-11.41

-11.28

-11.35

-11.29

-11.26

-11.18

-11.18

-11.14

-11.12

-11.21

-11.06

S.d.

of mean

± 0.04

0.06

0.04

0.03

0.03

0.04

0.04

0.04

0.04

0.02

0.06

S.d. of

1 obs.

± 0.13

0.30

0.22

0.17

0.15

0.24

0.23

0.21

0.23

0.2J

0.22

No.

obs.

8

30

28

30

20

30

35

28

33

91

15

Mean q

(a.u.)

0.08

0.13

0.25

O.36

0.46

0.55

0.66

0.74

O.85

O.96

1.01

Spo

Mean log

(cm" s )

-11.56

-11.39

-11.33

-11.26

-11.25

-11.25

-11.18

-11.14

-11.10

-11.19

-11.05

radio Meteors

c E.d.

of mean

± 0.11

0.14

0.06

0.05

0.05

0.04

0.04

0.04

0.04

0.03

0.07

E.d. of

1 obs.

± 0.15

O.36

0.25

0.20

0.17

0.19

0.23

0.21

0.20

0.22

0.24

No

obs

2

7

16

16

14

19

28

27

32

70

11

0.64 348

TABLE 17.11.2.—The ablation coefficient o as a function of the perihelion distance q for

short-periodandlong-periodsporadic Super-Schmidt meteors (classes A and8excluded)

Range

(a.i

0.0 -

0.1 -

0.2 -

0.3 -

0.4 -

0.5 -

0.6 -

0.7 -

0.8 -

0.9 -

1.0 -

All

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.9

l.o

l.l

Meteors with Q ' 6

Mean q Mean log

(a.u.) , -2 2>

S.d.

of mean

0.08

0.11

0.25

0.37

0.46

0.55

0.66

0.75

0.85

0.97

1.01

0.59"

-11.56

-11.15

-II.38

-11.16

-11.19

-11.23

-11.10

-11.05

-11.07

-11.10

-11.11

-11.14

S.d. of

1 obs.

± 0.11 ± 0.15

0.05 0.09

0.09 0.29

0.04

0.04

0.07

0.05

0.04

0.04

0.03

0.11

0.10

0.11

0.22

0.22

0.16

0.19

0.25

0.02 0.21

17

16

21

34

5

136

Meteors with Q > 6

Mean q Mean log a S.d. S.d. 0

(a.u.) 1 -2 2\ of mean 1 obi

0.15

0.24

0.35

0.46

0.54

0.66

0.74

0.85

0.96

1.01

0.72

-11.57

-11.24

-II.36

-11.40

-11.28

-11.31

-11.27

-11.15

-11.27

-11.01

-11.27

0.19

0.05

0.08

0.10

0.05

0.06

0.06

0.08

0.03

0.10

O.39

0.13

0.23

0.21

0.16

0.19

0.18

0.27

0.21

0.24

0.23

obs

TABLE 17.12.—Dependence of log <r on % and vice versa for sporadic Super-Schmidt

meteors (classes A and S excluded)

-12.02 11.45

-11.45 11.30

-11.30 —-11.15

-11.15 —-11.00

-11.00 10.42

Mean loi; 7

-11.62

-11.37

-11.23

-11.09

-10.87

Mean x ± s.d.

0.21 ± 0.05

0.23 ± 0.04

0.22 ± 0.03

0.22 ± 0.03

O.28 ± 0.06

26

40

69

63

41*

Range

-O.85

0.0

0.2

0.4

0.6

of X

— 0.0

— 0.2

— 0.4

— 0.6

— 1.28

Mean >

-0.10

0.09

0.29

0.47

O.78

-11

-11

log

.16

.22

-11.21

-11

-11

•13

.18

±

±

*

±

±

± s.d.

0.03

0.02

0.03

0.04

0.05

No.

obs

44

80

63

26

29
NO

-

 1 ATMOSPHERIC TRAJECTORIES OF 413 METEORS 129

TABUS 18.1.—The distribution of the fragmentation TABLE 18.2.—The distribution of the fragmentation

index x for Super-Schmidt meteors index x for smalUamera meteors

Range

-0.85 -

-o.to -

-0.30 -

-0.20 -

-0.10 -

0.00 -

0.10 -

0.20 -

0.30 -

0.1*0 -

0.50 -

0.60 -

0.70 -

0.80 -

0.90 -

1.00 -

1.10 -

1.20 -

1.30 -

1.1*0 -

1.50 -

2.00 -

of X

- -0.1*1

- -0.31

- -0.21

- -0.11

- -0.01

- 0.09

- 0.19

- 0.29

- 0.39

- 0.1*9

- 0.59

- 0.69

- 0.79

- 0.89

- 0.99

- 1.09

- 1.19

- 1.29

- 1-39

- 1.1*9

- 1.99

- 3.00

A l l

1

2

3

8

31*

"*j

1*9

35

36

23

1 0

12

9

7

2

2

0

2

0

1

1

1

Table 18.1

Sporadic Meteors

q £ 6 a.u. (

0

1

i

3

17

25

29

2l»

21*

11

1*

5

l*

5

2

2

0

2

0

0

0

0

I > 6

1

1

0

5

17

18

20

11

12

12

6

7

5

2

0

0

0

0

0

1

1

1

Shower

meteors

a.u.

0

1

2

6

1 2

19

15

12

18

9

1 0

7

3

2

0

2

0

0

1

0

0

1

All

meteors

1

3

5

11*

1*6

62

61*

1*7

51*

32

2 0

19

1 2

9

2

1*

0

2

1

1

1

2

Range

-0.50

-0.1*0

-0.30

-0.20

-0.10

0.00

0.10

0.20

0.30

0.1*0

A ll

of x

—-O.Ul

—-0.31

0.21

0.11

— -0.01

— 0.09

— 0.19

- 0.29

— 0.39

— 0.U9

Sporadic

meteors

1

0

2

It

7

3

5

3

3

2

30

Shaver

meteors

0

3

3

5

5

7

it

0

1

0

28

All

meteo

1

3

5

9

12

10

9

3

It

2

58

TABLE 19.1.1.— The fragmentation index %as a function of the velocity for Super-Schmidt meteors (classes A and

8 excluded)

AU Meteors Sporadic Meteors

Velocity range Mean v Mean x S.d. S.d. of Mean x No. Mean v Msan x S.d. S .d. of Mean x Ho.

(km/s) (km/s)* of mean lobs. (11^=0.86) obs. (km/s)~ of mean lobs. (1 . • 0.8 g) obs.

11-2 0 17.3 0.25 ± 0.0U ± 0.29 0.27 56 17.3 0.25 ± 0.0U ± 0.29 0.27 56

20-2 5 22.5 0.27 O.OU 0.33 0.28 57 22.3 0.26 0.05 0.33 0.27 1*6

25 - 30 27.3 0.22 O.OU 0.32 0.22 58 27.3 0.22 0.05 0.32 0.23 38

30 - 35 31.7 0.12 O.OU 0.25 0.12 I*U 32-0 0.15 0.05 0.27 0.15 26

35 - >*0 36.6 0.23 0.03 0.20 0.22 35 37.1 0.25 0.05 0.17 0.23 12

1*0 - 50 Mt.2 0.37 0.05 0.31 0.33 1*0 U5.3 0.28 0.06 0.28 0.2l* 20

50-6 0 56.I 0.27 0.05 0.21* o.22 22 55.7 0.29 0.06 0.25 0.2U 17

60-7 3 65.1 0.32 O.OU 0.26 0.23 1*7 65.5 0.32 0.05 0.26 0.22 32

All 35.O 0.25 0.02 0.29 0.23 359 33-1* 0.25 0.02 0.29 0.23 2!*9

TABLE 19.1.2.— The fragmentation index x as a function of velocity for sporadic Super-Schmidt meteors in

short-period and long-period orbits (classes A and 8 excluded)

Meteors with Q < 6 a.u. Msteors with 0 > 6 a.u.

Velocity range Mean v Mean x S.d. S.d. of Mean x v Ho. Mean v Mean x S.d. S.d. of Mean v Ho.

(km/s) (Ws f of mean lobs. (m, = 0.8 g) obs. (km/s) of mean lobs. (. . • 0.8 d obs.

11 - 20 17.2 0.28 ± O.Ott * 0.29 0-30 50 18.1 -0.01 i 0.06 * O.lU 0.01 6

20-2 5 22.3 0.27 0.05 0.33 0.28 38 22.3 0.22 0.11 0.31 0.22 8

25 - 30 27.3 0.22 0.06 0.29 0.22

 2? ^-2

 °'22 °'12 °M °-2K U

30 - 35 32.2 0.20 0.07 0.30 0.20 17 31.7 0.07 0.06 0.19 0.07 H

35 - 1*0 36.5 0.32 0.05 0.12 0.30 6 37.7 0.17 0.08 0.19 0.15 6

UO - 50 U2.0 0.28 0.07 0.09 0.20 2 1*5.7 0.28 0.07 0.29 0.2U 18

50-6 0 __ — — - - 55.7 0.29 0.06 0.25 0.2U 17

60-7 3 __ — — — — 65.5 0.32 0.05 0.26 0.21 32

All 23.5 0.26 0.03 0.29 0.27 l>*0 «>.l 0.2U 0.0 3 0.28 0.20 109
130 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS VOL. 10

TABLE 19.2.1.—The fragmentation index % « a function of the integrated brightness «o

for Super-Schmidt meteors (classes A and S excluded)

Range of €„

-1.1*0 1.00

-1.00 0.75

-0.75 0.50

-0.50 0.25

-0.25 — 0.00

0.00 — 0.50

0.50 — 1.00

1.00 — 1.50

1.50 — a.00

All

Mean

-0.39

-o.ii*

0.19

0.67

1.08

1.91

-0.1*1

All Meteors

Mean x E.d.

or mean

-1.14 O.32

-0.86 0.2U

-0.6U 0.35

0.26

0.17

0.19

0.10

0.35

0.23

0.25

0.0U

o.oi*

0.02

S.d. of

1 obs.

± 0.06 ± 0.28

0.03 0.25

O.Ol* 0.33

0.31

0.27

0.27

0.16

0.28

0.29

23

359

Mean

Sporadic Meteors

Mea

-l.lU 0.29

-0.86 0.2U

-o.6i* 0.36

-0.38 0.23

-o.ii* 0.20

0.17 0.18

o.6i* 0.05

of mean

± 0.06

0.01*

0.05

0.01*

o.oi*

0.05

0.01*

1.91 0.23 —

-0.1*2 0.25 0.02

E.d. of

1 obs.

± 0.21*

0.26

0.35

0.28

0.2U

0.25

0.15

obs.

16

1*6

60

"»7

33

31

13

21*9

TABLE 19.2.2.—The fragmentation index % <*« <* function of the integrated brightness

«« for sporadic Super-Schmidt meteors in short-period and long-period orbits

(classes A and S excluded)

Range of e

-1.1*0,

-1.00,

-0.75,

-0.50,

-0.25,

0.00,

0.50,

1.00,

1.50,

All

-1.00

-0.75

-0.50

-0.25

0.00

0.50

1.00

1.50

2.00

-1.13

-0.86

-0.61*

-0.39

-O.lU

0.17

0.60

Meteors with <J < 6 a.u.

Mean e_ Mean x S.d.

of mean

0.29

0.22

O.36

0.21

0.25

0.18

0.11

0.06

0.06

0.09

0.08

0.08

S.d. of No. obs.

1 obs.

± 0.06 ± 0.23

O.Ol* 0.25

0.35

0.26

0.31

0.32

0.15

Mean ca

-1.21*

-0.86

-0.63

-0.37

-O.lU

0.17

0.66

Meteors with Q > 6 a.u.

Mean x S.d.

of mean

0.32

0.32

O.38

0.21*

0.17

0.18

0.03

-0.55 0.26

1.91 0.23

-0.26 0.2U

± 0.28

0.09

0.08

0.06

0.01*

0.05

0.05

0.03

S.d. of No. obs

1 obs.

± 0.39 2

0.31 11

0.35 21

O.30 28

0.21 22

0.18 15

0.16 9

TABLE 19.3.—The fragmentation index % <** « function of mass for Super-Schmidt

meteors (classes A and 8 excluded)

Mas

0.01

0.05

0.10

0.20

O.UO

0.80

1.6

5.0

s range

(g)

- 0.05

- 0.10

- 0.20

- o.uo

- 0.80

- 1.6

- 5.0

- 31-

Mean m

(g) '

0.033

0.072

0.1U6

0.291*

0.596

1.12

2.57

10.2

Mean x

o.uo

0.26

0.21

0.2U

0.20

0.20

0.28

0.08

All Meteors

S.d.

of mean

± O.OU

0.03

0.03

0.0U

O.OU

0.05

0.07

O.Ol*

S.d. of

1 obs.

± 0.27

0.23

0.2U

0.32

0.32

0.29

0.35

o.iu

No. obs.

5U

1*7

65

61*

5U

35

27

13

Mean m

(g)

0.032

0.075

0.1U6

0.305

0.601*

1.11

2.5U

10.2

Sporadic Meteors

Mean x

0.39

0.23

0.17

0.25

0.2U

0.21

0.28

0.08

S.d. S

of mean

± o.Ol* ±

O.OU

0.03

0.05

0.05

0.05

0.08

O.Ol*

. d . of

1 obs.

0.26

0.20

0.21

0.35

0.33

0.29

O.3I*

O.lU

No. 0

38

2U

U2

1*0

1*3

31

18

13

0.85 21*9
ATMOSPHERIC TRAJECTORIES OF 418 METEORS 131

TABLE 19.4.— The fragmentation index x « <* function TABLE 19.6.—The fragmentation index x as a function

of the velocity for small-camera meteors of zenith angle ZR for small-camera meteors

10-20

20-30

30-40

40-70

All

15-U

25-2

34.0

57-1

32.4

0.07 ±

-0.01 ±

0.01 ±

-0.12 ±

-0.01 ±

0.04

0.06

0.04

0.04

0.03

(v.-30 W« )

0.08

0.00

-0.05

-0.18

-0.04

7

17

26

8

58

TABLE 19.5.—The fragmentation index % <** a function

of mass for small-camera meteors

Range of cos Z_

0.2

0.4

0.6

0.7

0.8

0.9

All

- 0.4

- 0.6

- 0.7

- 0.8

- 0.9

- 1.0

Mean cos Zp

0.28

0.52

0.66

0.75

0.85

0.95

0.74

Mean x *

-0.08 ±

0.14 *

-0.01 ±

-0.05 *

-0.07 ±

0.04 ±

-0.01 ±

s.d.

0.17

0.06

0.06

0.07

O.06

0.05

0.03

Mean X

A -30 km/*

(m][»30 g

-O.09

0.11

-0.02

-0.10

-0.04

0.01

-0.02

Mas

0.3

5.0

15

50

150

All

s range

(g)

- 5-0

- 15

- 50

- 150

- 2000

Mean mass

(g)

3-1

11.1

29.0

101

555

137

Mean X ± s.d.

0.06 ± 0.06

0.03 ± 0.06

-0.02 * 0.07

-0.09 ± 0.06

0.01 ± 0.06

-0.01 ± 0.03

Mean x

(^=30 km/s)

0.12

0.06

-0.02

-0.10

-O.O3

0.00

No.

12

12

9

14

11

58

TABLE 19.7.—The fragmentation index x for shower meteors; Super-Schmidt (classes A and S excluded) and smallcamera meteors

Super-Schmidt Mete

Quadrant Ids

Vlrglnids

Lyrids

H Aquarids

6 Aquarids

a Capricomids

Southern i Aquarids

Northern t Aquarid6

Perseids

H Cygnids

Drac raids

Orionids

Southern Taurids

Northern Taurids

Leonids

X Orionids

<j Kydrids

Geminids

Mean x S d.

0.44

0.12

0.08

0.09

O.58

O.38

0.20

0.10

0.23

0.11

1.89

0.54

0.04

0.11

O.37

0.04

0.21

0.09

0.09

0.07

0.11

0.26

0.09

0.09

0.57

0.06

0.05

0.15

0.04

0.05

S.d. of

1 obs.

0.11 ± 0.34

0.15

0.25

0.27

0.24

0.37

0.28

0.19

0.80

0.13

0.20

0.33

0.07

0.20

Mean m^ ± s. d

Is)

0.08 ± 0.02

1.07

0.13 ± 0.04

C.05

0.10 ± 0.04

0.53 ± 0.24

0.1D ± 0.02

0.11 ± 0.04

0.30 ± 0.14

0.39 ± 0.06

2.00 ± 0.13

0.04 ± 0.01

0.48 ± 0.13

O.85 ± 0.35

0.29

0.05 ± 0.01

0.76 ± 0.28

(Mean x)

(n = 0.8 g)

0.08

0.51*

0.38

0.17

0.22

0.11

0.40

0.04

0.11

-0.01

0.20

Meanx

10 — —

1 -0.08 —

3 -0.11 —

14 — —

5 — —

2 _ _

-0.13 0.10

-0.17

-0.13

0.07

0.10

1 — —

— 0.06 0.05

3 0.00 —

20 0.00 0.07

Small-Onera Meteors

of Mean m ± s.d. Mean v

* e.d.'

O.17

0.17

(g)

26.5

46 ± 41

44 i 19

71 ± 47

117 * 85

84.0

146 ± 99

(Ws)

31.1

48.8

60.2 ± 0.8

31.3 ± 0.2

29.4 * 1.1

30.6 ± 0.6

59.6

36.2 ± 0.1

Mean X

(m^ - 0.8 g

v. - JO to/.)

0.02

. 0.10
132 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS

TABLE 19.8.— The fragmentation index x os a function

of mass for Super-Schmidt (classes A and S excluded) and small-camera meteors. The values for smallcamera meteors were reduced to vm —SO km/s

Mass range Mean m Mean x

 s-d- S.d. of No.

(g) (g)°° of mean lobs. obs.

0.01 - 0.05 0.03 0.1*0 ± 0.01* ± 0.27 51*

0.05 - 0.10 0.07 0.26 0.03 0.23 "»7

0.1 - 0.2 0.15 0.21 0.03 0.2U 65

0.2 - 0.1* 0.29 0.21* O.Ol* 0.32 65

0.1* - 0.8 0.60 0.20 O.OU 0.32 5l*

0.8 - 1.6 1.12 0.20 0.05 0.28 37

1.6 - 5.0 2.9 0.21* o.O6 0.3lt 36

5 - 15 9.2 0.07 O.Ol* 0.18 23

15 - 50 28.7 -0.01 0.06 0.20 11

50 - 150 101 -0.10 0.06 0.21 lU

150 - 2000 555 -0.03 0.06 0.20 11

All 20 0.22 0.01 0.29 1*17

TABL E 19.9.— The fragmentation index x« a function of the integrated brightness «„ for

Super-Schmidt (classes A and S excluded) and small-camera meteors

Range o

-l.Uo —

-0.99 —

-O.7U —

-0.1*9 —

-0.21* —

0.01 —

0.51 -

1.01 —

1.51 —

2.01 —

2.51 —

A l l

f ex

-1.00

-0.75

-0.50

-0.25

0.00

0.50

1.00

1.50

2.00

2.50

3.1*0

Supei

Mean eo

-l.ll*

-0.86

-0.61.

-0.39

-O.ll*

0.19

O.67

1.08

1.91

-

-

-0.1*1

•-Schmidt Mat

= Mean x

0.32

0.21*

0.35

0.26

0.17

0.19

0.10

0.35

0.23

-

-

0.25

eors

No. obs.

23

6U

86

69

51*

1*1

19

2

1

-

-

359

Small-Camere

Mean £(>

-

-

-

-

-

0.28

0.81

1.21

1-76

2.22

3.02

1.61

Mean x

-

-

-

-

-

-0.05

0.11

0.05

-0.07

-0.15

0.00

-0.01

Meteors

No. obs.

-

-

-

-

-

2

11

lU

16

8

7

58

Mean e

-l.il.

-0.86

-0.6k

-0.39

-O.ll*

0.20

0.72

1.20

1.77

2.22

3.02

-0.13

Mean x

0.32

0.21*

0.35

0.26

0.17

0.18

0.10

0.09

-0.05

-0.15

0.00

0.22

All Met

S.d.

of mean

± 0.06

0.03

o.oi*

O.Ol.

o.oi*

0.01*

0.03

0.05

0.05

0.05

0.08

0.01

eors

S.d. of

1 obs.

± 0.28

0.25

0.33

0.31

0.27

0.26

0.18

0.19

0.19

0.15

0.22

0.29

No. ,

23

61*

86

69

^

1.3

30

16

17

8

7

k l 7

TABLE 19.10.1.— The fragmentation index x as a function of the zenith angle ZR for Super-Schmidt meteors (classes

A and S excluded)

All Meteors Sporadic Meteors

Range of cos 2^ Mean cos Z^ Mean x S.d. S.d. of Mean x No. Mean cos L Mean x S.d. S.d. of Mean X. No.

of mean 1 obs. (m^ = 0.8 g) obs.

 R

 O f mean 1 obs. (m^ = 0.8 g) obs.

0-1 - 0.2 0.15 0.59 ± 0.2U ± 0.1*8 0.51 1* O.lU 0.6U ± 0.33 ± 0.5Y

O-2 " 0.3 0.25 O.36 0.12 0.39 0.33 10 0.25 0.2U 0.11 0.31

°-3 - O.U 0.35 O.39 0.07 O.36 O.36 28 O.36 0.1*2 0.03 0.37

°-U - 0.5 0.U6 O.38 0.05 0.29 0.35 3l* 0.U6 0.37 0.06 0.30

0-5 - 0.6 0.55 0.26 0.06 0.1k o.2l* 31 0.55 0.26 0.07 0.31

°-6 " °-7 O.65 0.27 O.Ol* o.31 0.25 78 O.65 0.25 O.OU 0.31

°-7 - 0.8 0.75 0.22 0.03 0.23 0.21 71 0.75 0.17 0.03 0.19

°-8 " 0.9 0.8U 0.17 0.03 0.2l* 0.16 61 0.81* o.21 O.OU 0.25

°-9 - 1.0 0.97 O.lU 0.03 0.19 0.13 U2 O.96 0.15 0.05 0.22

A11 °-6

7 0.25 0.02 0.29 0.23 359 0.66 0.25 0.02 0.29

0.59

0.22

0.39

0.33

0.25

0.2U

0.17

0.21

O.lU

3

8

20

28

19

53

U8

U6

2U
ATMOSPHERIC TRAJECTORIES OF 413 METEORS

TABLE 19.10.2.—The fragmentation index x <w <* function of cos ZR for sporadic

Super-Schmidt meteors (classes A and S excluded)

133

nge of cos ^

0.1 - 0.2

0.2 - 0.3

0.3 - 0.1*

O.U - 0.5

0.5 - 0.6

0.6 - 0.7

0.7 - 0.8

0.8 - 0.9

0.9 - l.o

A l l

Mean cos

0.16

0.27

0.37

0.1*6

9.55

0.65

0.75

0.8U

0.95

O.67

Meteors with Q £ 0 a.

Z_ Mean x S.d.

of mean

0.97 ±

0.16

0.1*7

0.1*1*

0.26

0.23

0.17

0.21*

0.18

0.26

0.01*

0.19

0.13

0.10

0.08

0.05

O.OU

0.05

0.09

0.03

S.d. of

1 obs.

± 0.06

0.37

O.38

0.28

0.32

0.27

0.21

0.27

0.25

0.29

Ho.

obs.

2

It

9

8

15

3"*

30

31

7

lUO

Mean cos

0.10

0.23

0.3U

0.U6

0.53

0.6U

0.75

0.83

0.97

0.65

Meteors with Q > 6 a.

Zj, Mean x

-0.01

0.32

O.38

0.33

0.26

0.29

0.17

0.13

0.13

0.2U

S.d.

of mean

-

* 0.13

0.12

0.07

0.15

0.08

0.03

O.OU

0.05

0.03

u .

S.d. of

1 obs.

-

± 0.25

0.38

0.31

0.29

0.36

0.1U

0.17

0.22

0.28

Ho

obs

1

1*

11

20

U

19

18

15

17

109

TABLE 19.11.— The fragmentation index x o« a function

of the aphelion distance Q for sporadic Super-Schmidt

meteors (classes A and S excluded)

Ran^e of Q

(a.u.)

0 - 3.5

3-5 - U.2

U.2 - U.8

U.8 - 5.U

5.U - 7.0

7.0 - 2a

20-7 0

70 - -

Mean x

0.29

0.32

0.26

0.17

0.2U

0.21

0.28

0.2U

S.d.

of mean

± 0.07

O.OU

0.05

0.05

0.07

O.OU

O.OU

0.05

S.d. of

1 obs.

± o.Uo

0.21

0.30

0.27

O.38

0.22

0.22

0.27

Mean x

(m^ = 0.8 g)

0.29

0.3U

0.26

0.17

0.2U

0.18

0.20

0.21

Ho. 0

36

29

30

30

30

36

32

26

2l*9

TABLE 19.12.— Correlation between the

fragmentation index x and the ablation

coefficient a for small-camera meteors

Range_£f£ log 7

-12.2—11.8

-11.8 -11.6

-11.6 11.3

-11.3 10.8

Range of x

X < -0.2

-0.2 < X * 0

0 < x * 0.2

X > 0.2

-11.99

-11.72

-11.50

-11.15

b) 0

Mean x

0.28

-0.09

0.09

0.3U

Mean x

-0.11

-0.00

O.OU

0.02

vs. x

Mean lc« g •

(cm s )

-11.78 ± 0

-11.59 ± 0

-11.Uo ± 0

-11.56 ± 0

± s.d.

± 0.05

t 0.07

± 0.05

± O.OU

t s.d.

.12

.06

. 1 0

. 1 0

No.

obs.

11

13

13

1U

Ho.

obs,

9

20

15

7

TABLE 19.13.1.— The fragmentation index x as a function of the perihelion distance q for

Super-Schmidt meteors (classes A and S excluded)

Range of q

(a.u.)

0.0 - 0.1

0.1 - 0.2

0.2 - 0.3

0.3 - O.U

0.1* - 0.5

0.5 - 0.6

0.6 - 0.7

0.7 - 0.8

0.8 - 0.9

0.9 - 1.0

1.0 - 1.1

All

Mean q

(a.u.)

0.08

O.lU

0.25

0.35

0.1*6

0.55

0.66

0.7U

O.85

O.96

1.01

0.61*

Mean x

0.1*1*

0.32

0.18

0.16

0.21

0.2l*

0.29

0.28

0.23

0.29

0.12

0.25

All Meteor

S.d.

of mean

± 0.07

0.05

0.05

0.05

0.07

0.06

0.05

0.06

0.05

0.03

0.05

0.02

S .d. of

1 obs.

± 0.19

0.27

0.2"*

0.25

0.31

0.33

0.28

0.3U

0.32

0.30

0.18

0.29

Ho. obs. Mean q

(a.u.)

0.08

0.13

0.25

O.36

0.1*6

0.55

0.66

0.71*

0.85

O.96

1.01

0.71

Sporadic Meteors

Mean x s -

d0.30

0.1*3

0.26

0.20

0.26

0.18

0.28

0.27

0.23

0.26

O.lU

0.25

± 0.09

0.09

0.07

0.06

0.07

0.08

0.05

0.07

0.06

0.03

0.06

0.02

S.d. of

1 obs.

* 0.13

0.2U

0.27

0.25

0.28

0.29

0.3U

0.32

0.27

0.19

0.29

7

17

16

ll*

20

29

27

3

1*

72

11

21*9
1 3 4 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS TMt. »

TABLE 19.13.2.— The fragmentation index x as a function of the perihelion distance

q for sporadic Super-Schmidt meteors (classes A and S excluded)

Meteors with Q s 6 a.u. Meteors with 0 > 6 a.u.

Range of q Mean q Mean x S.d. S.d. of No. Mean q Mean x S.d. S.d. of No.

(a.u.) (a.u.) of mean 1 obs. . obs. (a.u.) of mean 1 obs. obs.

0.0 - 0.1 0.09 0.30 t 0.09 * 0-13 2

0.1 - 0.2 0.11 0.3U 0.07 0.13 3 0.15 0.51 ± 0.15 ± 0.30 U

0.2 - 0.3 0.25 0.15 0.06 0.21 11 0.2t 0.1*5 0.11 0.27 6

0.3 - O.U 0.37 0.17 0.06 0.16 8 0.35 0.2k 0.11 0.32 8

O.U - 0.5 0.1*6 0.22 0.09 0.28 10 0.U6 0.35 0.15 0.30 **

0.5 - 0.6 0.55 0.22 0.13 0.1*0 10 0.55 O.ll* 0.09 0.28 10

0.6 - 0.7 0.66 0.32 0.07 0.28 18 0.66 0.20 0.09 0.29 11

0.7 - 0.8 0.75 O.3U 0.10 0.39 16 0.7U 0.17 0.07 0.21* 11

0.8 - 0.9 O.85 0.19 0.06 0.27 21 O.85 0.31 O.ll O.38 13

0.9 - 1.0 0.97 0.30 0.05 0.30 36 O.96 0.21 O.Ol* 0.2l* 36

1.0 - 1.1 1.01 0.20 0.09 0.21 5 1.01 0.10 0.07 0.18 6

All 0.70 0.26 0.03 0.29 1'tO 0.73 0.21* 0.03 0.28 109

TABLE 19.13.3.—The fragmentation index x as a function of the perihelion

distance q for Super-Schmidt meteors (classes A and 8 excluded)

Meteors with Q s 6 a.u. Meteors with Q > 6 n.u.

Range of q Mean q Mean x S-d. E.d. of No. Mean q Mean x S.d. S.d.of No.

(a.u.) (a.u.) of mean 1 obs. obs. Of mean 1 obs. obs.

0.0 - 0.1 0.08 0.1*3 ± 0.08 ± 0.20 7 0.06 O.58 1

0.1 - 0.2 O.I1* 0.26 O.OU 0.21 26 O.ll* 0.6l ± 0.16 i 0.35 5

0.2 - 0.3 0.25 0.13 0.01* 0.18 18 0.21* 0.27 0.10 0.31 10

0.3 - O.U 0.35 0.13 0.05 0.23 22 0.35 0.21* 0.11 0.32 8

0.1* - 0.5 0.1*6 0.19 0.08 0.31 16 0.1*5 0.26 0.15 0.33 5

0.5 - 0.6 0.55 0.28 0.08 0.35 20 0.55 0.18 0.08 0.29 12

0.6 - 0.7 0.66 0.31 0.06 0.27 21 O.65 0.25 0.08 0.29 15

0.7 - 0.8 0.75 0.3l« 0.10 0.39 16 0.7U 0.20 0.07 0.25 12

0.8-0.9 O.85 0.18 0.06 0.27 22 O.85 0.31 0.11 0.38 13

0.9 - 1.0 0.97 0.31* 0.05 0.32 i*6 0.96 0.2U 0.01* 0.27 i»9

1.0 - 1.1 1.01 0.13 0.08 0.21 7 1.01 0.12 0.06 0.16 8

All 0.59 0.26 0.02 0.29 221 0.72 0.25 0.03 0.29 138

TABLE 20.1.— The blending and wake indices B and W for Super-Schmidt meteors. Also shown are the percentages of

meteors falling within each group of B and W.

No.obs. B±s.d . B = 0 0< B< 1 1<B< 2 2<B« 3 B> 3 V ± s.d. W. O 0<W* l 1<W*2 2 <W £ 3 W>3

All meteors U13 0.51 ± 0.05 67.6 15.5 10.2 5.1 1.7 0.7U ± 0.05 1*6.7 30.3 15.0 5.8 2.2

All meteors minus A and S 375 0.U6 ± 0.05 70.9 l^.U 8.5 4.8 1.3 0.75 ± 0.05 U7.2 29.3 1U.9 6.1 2.U

Sporadic meteors 290 0.1*7 ± 0.05 70.7 13.8 9.3 V.8 1.1* O.77 ± 0.06 U5.5 29.7 16.5 6.2 2.1

Sporadic meteors minus A and S 251 0.1.2 ± 0.06 73-3 13.1 8.0 U.U 1.2 0.71 ± 0.06 1*7.1* 29.1 16.3 5.6 1.6

Sporadic meteors minus A and S, 138 0.U6 ± 0.08 71.7 15.2 5.8 5.8 1.1* O.73 ± 0.03 U7.I 27.5 19.6 5.1 0.7

with aphelion distance < 6 a.u.

witrathellon°distence > Tt u'

 U 3

 °'^ * °'° 7 ^^ 10'

6 10*6 2-T

 °"9 °'7° * ° - 0 9 '*T-

8 31l ° 12-'* 6#2 2"6

Meteors with abrupt beginning (A) 26

Short-trail meteors (S) 12

Meteors with visible fragments (F) 11

1

0

0

• 35

• 57

.27

±

±

±

0

0

0

.2U

•23

.27

23.1

58.3

90.9

30

16

0

.8

.7

26.9

25.0

0

0.59

0.83

2.11

±

±

0

0

0

•13

.30

.1*3

38.5

50.0

18.2

1*6

25

9

. 1

. 0

. 1

15.1*

16.7

27-3

0

8.

27.

3

3

0

0

18.2
ATMOSPHERIC TRAJECTORIES OP 413 METEORS 135

TABLE 20.2.—The blending and wake indices B and W for Super-Schmidt shower meteors (arranged in

order of time of the year); also shown are the percentages of meteors falling within each group of

Band W

Shower

Quadrantids

Vlrginlds

Lyrids

Ti Aquarlds

1 Aquarids

y Capricornids

Southern L. Aquarlds

Northern v Aquarids

Perseids

H Cygnids

Draconlds

Orionids

Southern Taurlds

Northern Taurids

Leonids

a Hydrlds

Geminids

obs.

1 0

2

3

l

11

lU

6

2

11

1*

3

8

18

5

l

3

20

B ±

o.6o

0.25

0.50

1-55

1.00

0.83

0.50

0.03

0.50

U.00

O.Ul

0.00

0.06

0.00

0.U7

t

±

±

±

0

±

t

±

±

±

±

±

±

±

0

±

+

i.d.

0.11

0.25

0.50

0.27

0.3U

0.5U

0.50

0.03

0.50

0.00

0.19

0.00

0.06

0.00

0.17

B - 0 1

10.0

50.0

66.7

1 0 0

9-1

57.1

66.7

50.0

90.9

75.0

0

50.0

1 0 0

80.0

1 0 0

1 0 0

60.0

D<B £1

90.0

50.0

0

0

27-3

0

0

50.0

9-1

0

0

37-5

0

20.0

0

0

25.0

1< BS2

0

0

33-3

0

U5.5

21.U

16.7

0

0

25.0

0

12.5

0

0

0

0

10.0

2<S

0

0

0

0

18

2 1

16

0

0

0

0

0

0

0

0

0

5

.2

.u

.7

. 0

w ±

0.1*0

1.15

0.U3

0.21

0.7U

0.33

0.50

O.96

1.00

0.33

O.3U

0.11.

0.72

0.33

l.ue

8

i

±

±

0

±

±

±

±

±

±

±

±

±

±

1*

i

±

. d .

0.19

1.15

0.30

0.12

0.27

0.21

0.50

0.35

0.20

0.33

0.25

0.08

O.U3

0.33

0.26

w - 0

60.0

50.0

33.3

1 0 0

72.7

1*2.9

66.7

50.0

36.U

0

66.7

75-0

83.3

1*0.0

0

66.7

10.0

0< WS1

20.0

0

66.7

0

27.3

35.7

33.3

50.0

36.1*

75.0

33.3

12.5

16.7

20.0

0

33-3

U5.0

1< W s

20.0

0

0

0

0

7.1

0

0

9.1

25.0

0

12.5

0

1*0.0

0

0

30.0

1U.3

TABLE 20.3.— The blending and wake indices B and W as functions of velocity vn for (1) all

Super-Schmidt meteors, (2) sporadic meteors only; also shown art the percentages of meteors

falling within each group of B and W

l) Range of v^ No. B+ s.d. B-0 0<B' l

velocity ° obs.

10 - 20 17.1 67 0.70 -t 0.15 65.7 11.9

20 - 30 2U.9 128 0.51 * 0.09 71.1 12.5

30 - 1*0 3U.0 87 0.1*1 ± 0.08 70.1 16.1

1*0 - 50 1*1*. 1 1*8 0.92 ± 0.12 33-3 33-3

50-6 0 56.5 27 0.23 t 0.12 85.2 3.7

> 60 65.1* 56 0.20 ± 0.06 78.6 16.1

2)

10 - 20 17.1 66 0.65 * O.lU 66.7 12.1

20 - 30 2U.5 96 0.1*3 ± 0.09 70.8 16.7

30-1*0 33.8 1*5 O.38 ± 0.12 73-3 13.3

1*0 - 50 U5.0 25 0.70 i 0.17 52.0 16.O

50-6 0 56.1 21 0.30 ± 0.15 80.9 U.8

> 60 65.9 37 0.20 ± 0.03 8l. l 13.5

<B52

9.0

7-8

9-2

27.1

11.1

3-6

9-1

6.2

8.9

26.0

1U.3

2 . 7

2<Bs 3

9 .0

5-5

U.6

6.3

0

1.8

9.1

U.2

u.u

U.O

0

2 . 7

B > 3

U.5

3.1

0

0

0

0

3.0'

2 . 1

0

0

0

0

W i

1.02

0.7U

0.85

0.56

0.1*7

0.52

1.02

0.81

0.75

0.76

0.53

O.3U

*

i

i

t

*

t

±

±

±

±

±

s.d.

0.13

0.08

0.11

0.11

0.13

O.lU

O.lU

0.09

0.15

0.19

0.16

0.13

w =0

3U.3

U5.3

U2.5

50.0

59-3

62.5

3U.8

UO.6

51.1

Uo.o

57.1

67.6

0< W* l

31.3

31.3

31.0

35.U

25.9

23.2

30.3

33.3

22.2

UO.O

23.8

2U.3

1< W S2

23.9

1U.8

17.S

10.U

iu.6

5.U

2U.2

17.7

15.6

12.0

19.1

2 . 7

6.0

s

5

2

0

5

6

8

e

i*

0

2

.6

.8

. 1

.U

. 1

• 3

•9

.0

.7

W-- i

U.5

0

3-5

2.1

0

3-6

U.6

0

2 . 2

U.O

0

2.7
1 3 6 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS vc

TABLE 20.4.— The blending and wake indices B and W as functions of mm for (1) all Super-Schmidt meteors,

(2) sporadic meteors only; also shown are the percentages of meteors falling within each group of B and W

Rang e o f n S ^ No . B±s.d . B = 0

1 ) m < 0.1 0 0.0 5 11 9 0.U 5 ± 0.0 7 63. 0

O.lOS m < 0. 5 0.2 l 15 9 O. 1 *

1 * ± 0.0 6 68. 6

0 . 5 i •_ < 1. 0 0.7 1 6U 0.1*1±0.11 78.I

1.0 s m_ < 5 1.93 56 0.92 t 0.19 57.1

m^ > 5 10.15 13 0.19 ± O.19 92.3

2)

m^ < 0.10 0.05 75 0.3I* ± 0.08 72.0

0.10 < m^ < 0.5 0.21* 103 O.36 ±0.0 7 71.8

0.5 s m^ < 1.0 0.71 57 0.1*1 ± 0.11 77.2

1.0 s na < 5 1.86 1*1 O.96 ± 0.20 51.2

m > 5 10.15 13 0.19 ± 0.19 92.3

:B

22.

15.

7.

lU,

0

s l

.7

,1

.8

.3

16.0

15. .5

8.8

17.

0

.1

1< B

10

13

7

7

0

9

10

S 2

. 1

.2

.8

.1

.3

.7

8.8

9

0

.8

2<B «3

U.2

2.5

6.3

12.5

7-7

2 . 7

1.0

5.3

17-1

7-7

B

0

0

0

8

0

0

1

0

u

0

> 3

.6

• 9

.0

.9

w ±

0.1 9

0.6 0

1.0 6

1.5 U

2.U 8

0.2 0

0.5 2

1.0 9

l.U U

2.1* 8

8

i

±

±

±

±

±

±

±

±

i

.&.

O.OU

0.06

0.12

0.16

0.33

0.05

0.07

0.12

0.17

0.33

W - 0

75.6

U7.2

26.6

16.1

7.7

73-3

52.u

2U. 6

17.1

7-7

O'< W £ 1

21. 0

37- 1

35.9

3 0 . U

0

22. 7

3 U . 0

36. 8

31- 7

0

1 < WS 2

3.U

12. 0

28. 1

28. 6

3 8 . U

u.o

10.7

28.1

31.7

38.u

2 < 1

0

3.

6.

19.

V s 3

.1

• 3

.6

30. 8

0

2.

7.

17

30.

.9

.0

.1

,8

w >

0

0 . 6

3 . 1

5.U

23. 1

0

0

3.5

2.U

23. 1

TABLE 20.5.— The blending and wake indices B and W as functions of AM, the difference between the plate

limit and the maximum absolute magnitude, for (1) all Super-Schmidt meteors, {2) sporadic meteors

only; also shown are the percentages of meteors falling within each group of B and W

:B5 l

0

I8. 9

19. 8

1U. 1

0

0

15. 1

20. 8

12. 5

0

1<B* 2

7-9

7-2

lU.l t

13. 0

0

6.5

7-6

13. 0

10. 9

0

2<BS 3

2.6

2.6

7.2

6.5

11. 1

3.2

0.9

7.8

6.3

16. 7

B > 3

2 . 6

2.0

2 . 7

0

0

3.2

0 . 9

2 . 6

0

0

W i

0.1 8 ±

0.3 3 ±

0.6 3 ±

1.3 5 ±

2.8 6 ±

0.1 9 ±

o.uo ±

0.67 ±

1.U2 ±

2.63 ±

s.d.

0.03

0.03

0.06

0.11

0.U8

O.OU

0.05

0.08

O.lU

0.U8

W - 0

8U.2

67.3

Ul.U

13.0

0

83.9

63.2

U1.6

10.9

0

0<W SI

13.2

23.5

U2.3

38.0

5.6

12.9

25.5

39.0

37.5

8.3

1<W*2

0

8.5

13.5

32.6

22.2

0

10. u

16.9

32.8

25.0

2<w s 3

2 . 6

0 . 7

2 . 7

13.0

38.9

3.2

0 . 9

2 . 6

1U.1

Ul.7

w >

0

0

0

3

33

0

0

0

u

25

3

• 3

.3

• 7

.0

Rang e o f AM AM o ^ ° * B ± s.d . B- 0 0<Bs l

;

 4MSI.5 1.29 3 8 0.3 2 t 0.0 5 86. 8

1.5 < « « 2.5 2.10 153 0.U3 ± 0.05 69.3

2.5 < IMS 3.5 3-02 111 0.69 ± 0.08 55.9

3.5 < A M S 5 U.18 9 2 0.5 2 i 0.1 1 66. 3

A M > 5 5.6 9 1 8 0.3 1 ± 0.2 U 68. 9

A M s 1. 5 1-3 0 3 1 0.3 3 ± 0.0 6 87. 1

1 . 5 < A M s 2. 5 2.0 9 10 6 0.3 2 ± 0.0 6 75- 5

2 . 5 < A M s 3. 5 3-0 0 7 7 O.69±O.O 9 55. 8

3 . 5 < <M« 5 U.2 1 6U 0.U8 ± O.lU 70. 3

A M > 5 5.7 1 1 2 0.U 6 ± 0.2 6 83. 3

TABLE 20.6.— The blending and wake indices B and Was functions of the integrated brightness tfor (1) all

Super-Schmidt meteors, (£) sporadic meteors only; also shown are the percentages of meteors fallina within

each group of B and W

Rang e o f c t a No . B±s.d . B- 0 0<Bs l 1<B* 2 2<B* 3 B > 3 X I ± s.d . W = 0 3<WS 1 1<WS 2 2<W« 3 W> 3

obs .

1 )

-0.7 5 < c^ * -0.5 0 -O.6 U io o 0.61 * ± o.i o 57. 0

-0.5 0 < e ^ * -0.2 5 -0.3 9 7 7 0.6 2 ± 0.1 2 62. 3

-0.2 5 < e ^ * 0.0 0 -O.l U 6 0 0.5 5 ± 0.1 3 70. 0

c ^ > 0 O.3 7 6 7 0.2 9 ± 0.0 9 82. 1 7. 5 U. 5 6. 0 0 1.9 7 * O.l U 7. 5 22. U 31. 3 25. U 13. U

2 )

c _ « -O.7 5 -O.9 2 7 5 0.3 2 ± 0.0 7 73- 3

-0.7 5 < t m * -O.5 0 -0.6 U 7 0 O.5 2 ± 0.1 1 62. 9

-0.5 0 < e ^ s -0.2 5 -O.3 9 5 2 O.3 9 ± O.l l 73. 1

-0.2 5 < £ ,

 s 0.0 0 -O.l U 1 0 0.7 0 ± 0.1 7 65. O

e _ > 0 O.3 U 1, 5 0.3 U ± 0.1 3 82. 2

15. 3

25. 0

16. 9

8.3

7.5

1U. 7

22.9

13.5

5 . 0

6.7

11.2

9.0

13.0

13.3

U.5

10.7

7-1

9.6

20.0

2.2

2 . 1

7.0

3.9

6.7

6.0

1.3

U.3

3.8

7.5

8.9

0

2

3

1

0

0

2

0

2

0

.0

• 9

.7

.9

.5

0.27

o.uu

0.70

0.79

1.97

0.31

0.U6

o.7£

0.9 a

1.9 6

±

±

±

±

±

i

i

i:

±

i

0.0 5

0.0 7

0.0 9

0.1 0

0.1 U

0.0 6

0.0 8

0.1 2

0.1 3

0.1 7

70.1 *

58. 0

Ul. 6

33.3

7.5

66.7

57. 1

Uo.l*

22. 5

8.9

25. 5

23. 0

U0. 3

LO.O

22.1*

28.0

27.1

36.5

U7.5

17.8

U.I

12.0

1U.3

23. 3

31. 3

5.3

1U. 3

17- 3

25- 0

33.3

0

2

3

3

25

0

1

5

5

26

.0

.9

.3

.1*

.It

.8

.0

.7
NO

-

 x ATMOSPHERIC TRAJECTORIES OP 41 3 METEORS 13 7

TABLE 20.7.— The blending and wake indices B and Was functions of the mass-loss coefficient o for (1) all Super-Schmidt

meteors, (£) sporadic meteors only; also shown are the percentages of meteors falling within each group of B and W

1)

-11.U5

-11.30

-11.15

2)

-11.U5

-11.3

-11.15

£

£

£

£

£

Range of log o

(cm-2s

2)

log a < -11.U5

log

log

log

log

log

log

log

log

log

a <

c<

a<

a a

a <

a <

a <

o <

a >

-11.3

-11.15

-11.0

-11.0

-11.U5

-11.3

-11.15

-11.0

-11.0

loft a

-11.66

-11.37

-11.23

-11.09

-10.83

-11.62

-11.37

-11.23

-11.09

-10.82

Ho.

Obs.

51

63

102

92

88

28

37

78

68

68

B *

0.61 ±

0.22

O.36

0.52

0.7U

0.35

0.25

0.35

0.U2

O.69

±

±

*

±

±

±

-t

±

s.d.

0.15

0.07

0.08

0.09

0.11

O.lU

0.11

0.10

0.09

0.12

B = '

6U.7

8U.1

76.5

65.2

53. U

71.1*

83.8

78.2

70.6

57.3

15.7

9-5

10.8

17.1.

23.9

17.9

10.8

10.3

19-1

26.5

3-9

3.2

6.9

6.5

8.0

0

2.7

6.U

8.8

8.8

5.9

3.2

1.0

0

3.1*

7.1

2.7

1.3

0

2.9

0 0<B* l 1<B*2 2<B«3 B>3 W ± «.d. V-0 0<W*l KW42

17.7 7.8 3.9 5.9 O.78 ± 0.16 51.0 23.5

7.9 6.U 1.6 0 0.5U ± 0.12 63.5 20.6

13.7 U.9 2.9 2.0 0.66 + 0.09 U9.0 32.3

1U.1 16.3 3-3 1.1 O.78 ± 0.09 39.I 37.O

21.6 13.6 11.U 0 1.02 4 0.11 29.5 35.2

17.9 7.1 0 3.6 0.75 ± 0.21 50.0 25.0

5.U 8.1 2.7 0 0.51 t O.lU 62.2 21.6

11.5 5.1 2.6 2.6 0.68 ± 0.10 U6.1 35.9

11.8 16.2 1.5 0 0.85 i 0.11 38.2 33.8

20.6 10.3 11.8 0 1.0U ± 0.13 32.U 29.It

TABLE 20.8.— The blending and wake indices B and Was functions of the fragmentation index x for (1) <*# SuperSchmidt meteors, (2) sporadic meteors only; also shown are the percentages of meteors falling within each

group of B and W

No. _

Range of x X obs. B * s.d. B=0 0<B£ l 1<B£2 2<B*3 B> 3

1) X < 0 -0.11 69 0.29 * 0.09 81*.1 5.8

0 s X < 0.2 0.09 137 0.32 * 0.06 79.2 9.6

0.2 £ x ^ O.U 0.30 101 0.U9 ± 0.09 6l.l* 25.7

o.U s x < 0.6 0.U8 52 0.59 * 0.11 57.7 17.3

X ? 0.6 O.89 53 1.20 ± 0.18 37.7 22.6 17.0 15.1 7.6

2)

x < 0 -0.11 1*8 0.31 ± o. u 83.3 6.3

0 £ X < 0.2 0.09 100 O.38 t 0.08 77-5 8.2

0.2 n < o.u 0.29 71 0.35 ± 0.08 67.6 23.9

O.U s x < 0.6 0.1*8 33 0.1*0 ± 0.12 69.7 15.2

X 2 0.6 0.89 37 l.l l * 0.21 U3.3 18.9 16.2 16.2 5.it

TABLE 20.9.— The blending and wake indices B and W as functions of the zenith angle ZR for (/) all SuperSchmidt meteors, (i) sporadic meteors only; also shown are the percentages of meteors falling within each group

of B and W

Range of cos z ^s~ZT No. B t s.d. B = 0 0<B* l K B *2 2<B* 3 B>3 ff ± B.d. W-0 0<W* l 1<V* 2 2<W*3 W>5

R « 00S.

cos 7 < 0.1. 0.30 51 0.79 ± 0.17 56.9 21-6 5.9 9.8 5.9 0.79*0.13 1*5.1 25.5 21.6 7.8 0

O.U <• cos Zj, * 0.6 0.50 76 0.61. ± 0.12 65.8 11.8 13.2 6.6 2.6 0.73*0.12 53-9 25.0 11.8 5.3 ><.O

0.6 < cos Z^ « 0.7 O.65 88 0.56 ± 0.10 65.9 15.9 10.2 5-7 2.3 O.67±O.1O U7.7 33.O 12.5 k.5 2-3

0.7 < cos Z^ < 0.8 O.75 75 O.UU ± 0.09 68.0 16.0 10.7 5.3 0 0.62 ± 0.10 50.7 28.0 U.7 6.7 °

0.8 < cos z,, * 0.9 0.61* 77 0.30 ± 0.07 72-7 15.6 11.7 0 0 0.67*0.11 U6.7 36.1* 10.1* 2.6 3.9

cos Zp > 0.9 0.97 U6 0.32 * 0.10 76.1 13.0 6.5 U.l. 0 1.12 * O.16 28.3 32.6 26.1 10.9 Z-S

''^ cos Zp < O.I. 0.30 38 0.75*0.20 63.2 15.8 5.3 10-5 5.3 0.83*0.17 1*7.'. 18.1* 23.7 10.5 0

O.U < cos Zj, « 0.6 0.1.9 55 0.62*0.15 69.l 9-1 10.9 9-1 1-8 0.90*0.15 1*5.1. 27.3 16.<• 5-5 5.5

0.6 < cos Z,, s 0.7 0.65 60 O.Ul ± 0.11 71-7 15.0 8.3 3.3 1-7 0.78*0.12 38.3 36.3 16-7 5.0 1.7

0.7 < cos Zp £ 0.8 0.75 51 0.29*0.09 76.5 11.8 9-8 2.0 0 0.59*0.12 5"*-9 23-5 15-7 5.9 0

0.8 < cos Zp s 0.9 0.81. 60 0.37 ±0.0 8 66.7 20.0 13.3 0 0 0.65*0.11 U6.7 35.0 13.3 1.7 3-3

cos Z,, •> 0.9 O.96 26 0.37 * 0.17 80.8 7-7 3.9 7-7 0 0.95 * 0.21 38.5 30.6 I5.U 15."* 0

U.3

8.9

6.9

21.2

17.0

U.2

11.1

5-6

12.1

16.2

5-8

2.3

U.O

3-8

15.1

6.2

3-2

l.U

3-0

16.2

w

0.76

0.72

0.77

0.6U

0.79

0.81

0.70

0.77

0.70

0.9U

±

±

±

±

*

±

±

±

±

±

s.d.

0.11

0.08

0.10

0.12

O.lU

O.lU

0.09

0.11

0.16

0.19

W-0

UU.9

50.7

39.6

53.8

U5.3

U3.7

U9.5

39.U

5U.6

1*0.6

31.9

26.1

37-6

25.0

30.2

29.2

27.7

38.0

18.2

29.7

13.0

15.2

16.8

15.u

13.2

1U.6

15.8

16.9

21.2

16.2

8.7

5-8

3.0

3.9

9.U

10.u

6.0

2.8

3.0

10.8

1.5

2.2

3.0

1.9

1.9

2.1

1.0

2.8

3.0

2.7
1 3 8 SMITHSONIAN CONTRIBUTIONS TO ASTROPHYSICS voi

TABLE 20.10.— The blending and wake indices as functions of the aphelion distance Q for (1) all SuperSchmidt meteors, (2) sporadic meteors only; also shown are the percentages of meteors falling within each

group of B and W

Range

(a.u

3-5 < Q

5 < Q

7 < Q

Q

3-5 < Q

5 < Q

7 < 4

Q

f Q

.)

* 3-5

* 5

s 7

* 20

> 20

* 3-5

s 5

* 7

& 20

> 20

obs.

B ± s.d. B "0

2.6 75 0.70 4 0.13

U.3 122 0.55 ± 0.09

5.7 78 0.66 ± 0.12

12.1 U2 0.27 4 0.10

60 9U 0.32 4 0.07

2.6 UU 0.97 4 0.19

U.3 8U 0.U2 4 0.10

5.7 5U 0.U3 ± 0.13

11.6 37 0.31 4 0.11

63 70 0.3U ± 0.08

57.3

66.It

6U.1

81.0

1*7-7

71.U

77.8

78.it

22.7

15.6

1U.1

7.1

73-1* I1*.9

25.0

16.7

5.6

8.1

12.9

6.7

12.3

10.3

11.9

9.6

6.8

8.3

9.3

13.5

10.0

B> 3 V? ± s.d. 0<WSl

10.7 2.7 0.81 4 0.11 uo.o 3U.7

U.I 1.6 0.71 ± O.08 U6.7 3O.3

7.7 3.8 0.80 ± 0.11 U3.6 32.0

0 0 0.6U ± 0.15 52.U 28.6

2.1 0 0.72 ± 0.11 52.1 25.5

15.9 U.6 0.68 ± 0.11 U3.2 3U.I

2.U 1.2 0.79 ± 0.11 UU.O 2P.6

5.6 1.8 0.93 ± 0.15 38.9 33-3

0 0 0.68 ± 0.16 51.U 27.0

2.9 0 0.72 ± 0.12 50.O 27.1

KWS2

21.3

16.U

12.8

11.9

11.7

22.7

20.2

13.0

13.5

12.9

2<W «3

1.3

U.9

10.3

U.8

7-5

0

U.8

13.0

5.U

7 . 1

W>3

2 . 7

1.6

1-3

2.U

3.2

0

2.U

1.8

2 . 7

2 . 9

TABLE 21.—Physical characteristics of individual meteor showers

All meteors

Sporadic meteors

Shower meteors

Abrupt-beginning meteors

Short, fl=-re-like meteors

Individual Showers:

Quadrantids

Vlrglnlds

Lyrids

t\ Aquarids

{ Aquarids

0 Caprlcornlds

Southern t Aquarids

Northern i Aquarids

Perselds

« Cygnids

Draaonlds

Orlonlds

Southern Taurlds

northern Taurlds

Leonids

0 Hydrlds

Oeminlds

(tan/

35.3

33-7

39-3

28.8

36.8

U3.1

30.8

U8.8

's'

4

4

±

±

4

±

4

*

)

0 . 8

1 . 0

1 . 2

3-1

U.2

0 . 2

3.7

1.1

66.8

U2.5

25.6

3U.U

35.9

60.2

23.2

20.2

68.0

29.0

31.1

4

±

±

±

4

4

±

±

4

4

0.3

O.U

1.0

1.7

0 . 2

O.U

0 . 1

O.U

O.U

0.5

71.7

59-2

36.2

4

4

0 . 6

0 . 1

cos

O.67

0.66

0.69

0.67

0.78

0.61

0.73

0.93

0,

0.58

O.69

0.5U

0.70

±

±

±

±

4

4

±

0.01

0.01

0.02

O.OU

O.OU

0.05

0.02

0.05

.U2

±

4

±

0.03

0.03

O.OU

0.08

0.52 4 0.08

0.68

0.61

0.60

0.73

0.8U

0.

0.8U

0.86

±

±

*

±

±

4

4

0.13

0.06

0.08

0.03

0.07

0.02

O.OU

+0.0 •t

+0.1 *

-0.2

-0.1

-0.8

+0.2

-0.2

-1.0

±

±

4

±

4

-0.'

-0.1

+0.7

+0.5

+0.6

-l.U

+0.8

+0.1

-1.1

+0.5

-0.8

±

4

±

4

4

±

±

4

4

4

- 3 .

-0.7

-0.8

4

4

0 . 1

0 . 1

0 . 1

0.2

0.2

0.3

0.3

0.3

r

0.3

0 . 2

O.U

0. 9

O.U

0 . 3

0. 0

0.3

0.3

0.5

3

0 . 1

0.3

«B

(to)

100.0 4

98.8 4

102.9 4

92.5 4

9U.3 4

102.8 4

96.0 4

107.1 4

115. <

99.8 4

97.8 4

96.3 4

99-1 4

11U.1 ±

O.U

0 . 6

0.6

2 .1

2 . 7

0.7

5.U

0 . 9

1.1

0 . 8

1-9

1.5

1.1

99.2 4 0.8

103.6 4 0.2

117.0 4

100.8 4

103-3 4

127.!

111.7 4

100.U 4

0.5

0.5

1.0

3

0.3

0.3

H

2.5

(to)

99.6 4

98.2 4

103.0 4

92.U 4

9U.U 4

103.1 4

96.0 4

107.9 4

119.6

99.8 4

96.9 4

95.7 4

98.8 4

11U.8 4

97.1 4

102.6 4

119.6 4

99.6 4

103.0 4

125.9

113.6 4

101.3 4

0.5

0 . 6

0 . 7

2 . 3

2 . 8

0 . 7

3-U

0.7

1.2

0 . 8

1.7

l.U

1.1

1.1

0 . 2

1.0

0 . 6

1.2

1

1.6

0. 5

"ML

(to)

89.8 4

89.14

91.5 4

87.64

89.7 4

95.7 4

83.7 4

97.3 4

102.:

93.0 4

89.6 4

90.2 4

89.9 ±

99.0 4

88.9 4

96.7 4

105.9*

87.9±

83.2 4

89.:

92.9 4

85.6 4

O.U

0.5

0.7

1-7

2 . 0

1.5

0.8

2 . 6

L

0.7

1.1

1 . 1

3.9

1.5

2-3

O.U

1.7

0. 9

1.3

L

O.U

1.5

"E

(k»;

85.1

8U.5

86.5

81.5

85.2

90.6

77.7

87.6

4

4

4

4

4

4

4

4

O.U

0.5

0.7

l.U

1.9

1.6

1.1

2.5

99.7

88.U

86.0

86.5

8U.7

9U.3

85.5

91.0

99.3

82.2

79.5

4

4

4

4

4

4

4

4

4

4

87.:

88.8

80.0

±

0. 8

1.3

l . l

U.I

1.8

2 . 0

O.U

1.7

0. 9

l.U

>

1.8

1.8

1

O.76

0.80

0.67

0.62

0.32

0.U8

0.89

0.U3

0.

0.U9

0.70

0.58

0.57

0.67

D

4

4

4

4

4

4

4

4

)

0.02

0.03

0.03

O.OU

0.02

0.03

0.U2

0.07

• 58

4

4

4

4

4

0.06

0.08

0.12

0.02

0.10

0.9U 4 0.08

1.22

0.U7

0.91

0.97

0,

0.U6

0.6U

4

4

4

4

0.12

0.05

0.05

0.16

.6U

4

4

0.02

0.0U

-0.U2 4

-O.UU 4

-O.36 4

-0.50 4

-0.52 4

-0.58 4

-0.31 4

-0.18 4

0.02

0.03

0.05

0.07

0.10

0.09

0.31

O.lU

-0.20

-0.59 4

-O.67 4

-0.73 ±

-0.63 4

+0.16 4

-0.65 4

-0.29 4

-O.lU 4

-0.1*5 4

+0.00 4

0.11

0.12

0.12

0.2U

0.20

0.O5

0.03

0.10

0.10

0.22

+0.72

-0.29 4

-0.18 4

0.08

0.13

°»

(g)

0.80 4 0.11

0.96 4 0.16

0.U2 4 0.07

0.65 4 0.12

0.32 4 0.09

0.08 4 0.02

0.59 4 O.kJ

0.13 4 0.1*

0.0k

0.09 4 0.03

0.53 ± 0.2h

O.U 4 0.02

O.U 4 0.0k

0.27 ± 0-13

0.39 4 0.06

2.00 4 0.13

0.06 4 0.02

0.U8 4 0.13

1.01 4 0.32

0.29

0.05 4 0.01

O.76 4 0.28
ATMOSPHERIC TRAJECTORIES OF 41 3 METEORS 139

TABLE 21.—Physical characteristics of individual meteor showers.—Continued

All meteors

Sporadic meteors

Shower meteors

Abrupt-beginning meteors

Short, flare-like meteors

Individual Showers:

Quadrantids

Virginids

Lyrids

n Aquarids

6 Aquarids

a Capric imids

Southern i Aquarids

Hbrthem v Aquarids

Perseids

*•. Cygnids

Draconlds

Orionlds

Southern Taurids

Northern Taurids

Leonids

a Hydrids

Geninids

log o

, -2 2.

(cm s .

-11.19 ±

-11.16 i

-11.25 ±

-11.OU ±

-11.18 +.

-11.US ±

-11.19 ±

-11.17 ±

)

0.01

0.01

0.02

0.06

0.12

0.09

0.06

0.17

-11.01

-11.Uo ±

-11.09 ±

-11.27 ±

-11.U8 ±

-11.26 i

-11.07 ±

[-1U.88 ±

-11.20 *

-11.31 ±

-11.36 ±

0.05

0.08

0.12

0.25

0.06

0.08

0.79)

0.11

0.03

0.06

-10.99

-11.U6 ±

-11.23 ±

0.06

0.07

X

0.27 ±

0.27 ±

0.27 ±

0.25 ±

0.27 ±

o.uu +.

0.15 ±

0.08 ±

0.01

0.02

0.03

0.05

0.06

0.11

0.03

0.09

0.09

0.52 ±

0.38 ±

0.18 ±

0.10 ±

0.28 ±

0.11 ±

1.89 ±

0.U6 t

o.ou ±

0.03 ±

0 .:

o.ou ±

0.21 ±

0.08

0.07

0.09

0.26

0.10

0.09

0.57

0.06

0.05

0.07

!7

o.ou

0.05

A lo iI 0

(g/cn3)

0.00 ±

0.00 ±

0.00 ±

-0.18 ±

0.15 ±

0.03 ±

-O.36 ±

-0.10 ±

0.01

0.02

0.02

0.08

0.12

0.08

0.12

0.09

-0.21

0.03 *

0.15 ±

-0.05 ±

-0.2U ±

-0.03 ±

0.15 ±

U.61 *

O.lU ±

-0.00 ±

-0.06 *

O.OU

0.03

0.06

0.28

0.05

0.06

0.85

0.08

0.03

0.07

-0.23

-0.10 ±

-0.39 ±

0.12

0.06

r

0.7U

O.77

0.67

0.59

O.83

O.Uo

1.15

0.U3

V

± 0.05

± 0.06

± 0.08

± 0.13

± 0.30

± 0.19

i 1.15

± 0.30

0 . 0

0.21

0.7U

0.33

0.50

0.96

1.00

0.00

0.3U

O.lU

0.72

1

0.33

1.U8

± 0.12

± 0.27

± 0.21

± 0.50

* 0.35

* 0.20

± 0.00

± 0.25

± 0.08

± O.U3

i.O

± 0.33

± 0.26

B

0.51 ±

0.U7 ±

0.63 ±

1.35 ±

0.57 ±

0.80 ±

0.25 ±

0.50 ±

0.05

0.05

0.06

0.2U

0.23

0.11

0.25

0.50

0 . 0

1.55 *

1.00 *

0.83 ±

0.50 ±

0.03 ±

0.50 ±

U.00 ±

O.Ul ±

0.00 ±

0.06 i

0.27

0.3U

0.5U

0.50

0.03

0.50

0.00

0.19

0,00

0.06

0.0

0.00 ±

0.U7 i

0.00

0.17

D/D,

0.61 ±

0.60 ±

0.65 ±

0.U5 ±

0.35 ±

0.61 ±

0.67 ±

0.6U *

th

0.01

0.01

0.02

0.03

O.OU

0.03

0.17

0.11

0.63

0.50 ±

0.58 ±

0.53 ±

0.63 ±

0.56 t

0.69 ±

0.50 ±

0.55 *

0.8U ±

0.77 *

0.05

o.ou

0.10

o.ou

o.ou

0.03

0.02

o.ou

0.02

0.05

o.uu

0.87 ±

0.69 *

0.10

0.03

i'«2

+0.3 *

0.0 ±

+1.0 *

-5.1 ±

-7.0 ±

•0.3 *

-3.0 ±

-0.7 *

•5.:

-3.1 ±

+2.U ±

-3.2 ±

-1.2 *

•0.8 ±

•U.I ±

•9.5 *

+U.8 ±

+2.2 *

•2.7 *

+5."

•2.1 ±

-0.5 ±

.5

)

0.5

0 .6

0.7

2 . 3

2.8

0.7

3.U

0.7

i

1.2

0 . 8

1.7

l.U

1.1

1.1

0 . 2

1.0

0 . 6

1.2

I

1.6

0,5

Bo.ol

U13

290

123

26

12

10

2

3

1

11

1U

6

2

11

u

2

8

18

5

1

3

20

U.S. SOVUNMENT niMTIRS OrriCI : 1M7 O-Uf-t M