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JAN 2 4 1966

^ecknical v£ote ^o. 329

THE SEASONAL VARIATION OF NIGHTGLOW Nal

5890-96 A, (01) 5577 A AND (01) 6300 A IN

THE TROPICS

L. L. SMITH and R. W. OWEN

U. S. DEPARTMENT OF COMMERCE

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technical ^ote , 329

ISSUED January 10, 1966

THE SEASONAL VARIATION OF NIGHTGLOW Nal 5890-96 A,

(01) 5577 A AND (01) 6300 A IN THE TROPICS

L. L. Smith and R. W. Owen

Institute for Telecommunication Sciences and Aeronomy

Environmental Science Services Administration

Boulder, Colorado

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TABLE OF CONTENTS

Abstract

1. Introduction

2. Observations

3- Calibration and Data Reduction

k. Analysis and Interpretation. .

5. Summary

Acknowledgements

References

Tables

Figures

Page

1

1

1

1

k

10

11

k6

13

35

1x1

THE SEASONAL VARIATION OF NIGHTGLOW Nal 589O-96 A,

[01] 5577 A AND [01] 63OO A IN THE TROPICS

by

L. L. Smith and R. ¥. Owen

A study is presented of one year (July 1961- July 1962) of

systematic zenith observations of the nightglow emissions [Ol] 5577A,

[pi] 6300A, and Nal 5890- 96A at the Haleakala Observatory (latitude

N 20. 7*). Observed seasonal variations are shown and compared with

previous investigations.

Key Words: Nightglow, Seasonal, Zenith, (pi) 5577A, [pij 6300A,

Nal 5890-96 A.

! INTRODUCTION

During the year July 1961 to July 1962, airglow data were obtained

on Mount Haleakala (altitude 10,000 feet A»S.L«, geographic latitude

N 20 .7, and longitude W 156 .3) through the cooperative efforts of the

National Bureau of Standards, Boulder, Colorado, and the Hawaii Institute

of Geophysics of the University of Hawaii, Honolulu, Hawaii. A photometer having a built-in, absolutely calibrated standard light monitored

the zenith sky brightness using interference filters centered on 5300,

5577, 5893, and 6300 A [Purdy, Megill, and Roach, I96I]

.

II* OBSERVATIONS

Observations were made on moonless nights with skies of photometric

quality between astronomical twilight and astronomical dawn during each

lunation for a two-week period centered on the date of new moon. A

total of 128 nights of useful data was obtained during the year July I96I

to July 1962.

The method of operation of the photometer is fully described by

Purdy, Megill and Roach [I96I] . Figure 1 is an illustration of the strip

chart recording from the zenith photometer.

Ill* CALIBRATION AND DATA REDUCTION

The calibration of the recordings from the turret photometer requires

a determination of the absolute brightness of the standard source. The

data reduction involves a method for the elimination of the background

contaminations in the 5577, 5893, and 6300 A filters.
The absolute calibration of the standard source in the turret

photometer was obtained by comparison with a laboratory-calibrated

standard source, as described by Smith and Alexander [1963]. The twocolor method [Roach and Meinel, 1955] "was used to eliminate the background contamination from the turret emission line filters by the

equation:

R = [(DE - F • DC) • W • I • ] / T, (l)

where R is the emission line intensity in rayleighs,

DE is the ratio of sky reading to standard light reading

of the emission filter,

DC is the ratio of sky reading to standard light reading

of the 5300 A background filter,

F is the factor to be multiplied by DC to determine the

background to be subtracted from DE,

W is the 100$ equivalent transmission of the filter in

angstroms,

I is the absolute brightness of the standard light in

rayleighs per angstrom,

is the correction factor to refer the reading inside

the earth's atmosphere to outside the earth's

atmosphere,

and T

' is the transmission of the interference filter DE at

the wavelength of the emission line.

The two-color reduction method to eliminate the background intensities (airglow continuum, zodiacal light, and starlight) must be con- sidered only as an approximate technique. The contamination of the

"^The F factor was computed by taking the ratio of the brightness

of the standard light for the control filter to the brightness for the

emission filter [Davis and Smith, 196^].

,y y For the sodium filter which includes both wavelengths of the

doublet (5890-96 A), allowance was made for a relative intensity difference between the 5890 and 5896 A lines of two-to-one.
observations, due to the OH band emissions, the assumption that the

background co-varies from 5300 through the 63OO A wavelength region, the

uncertainties in the corrections for the extinction and scattering of

the earth's atmosphere, and the uncertainty in the absolute calibration

of the standard source contribute to the inaccuracy of the reduction

method. However, over the past few years, this method has been significantly improved through the availability of extremely narrow band interference filters and low noise - high sensitivity photomultiplier tubes

and through the improvements achieved in calibrating low light level

sources.* Table 1 is a summary of the constants used for the reduction

of the turret photometer observations by (l) for the observing period

during the month of September, 1961. A change in the I and F con- stants of (l) was necessary from one observing period to the next due to

the deterioration of the radium isolite source [Smith and Alexander,

1963]. The average luminosity deterioration of the isolite source at

the four wavelengths utilized in this study was 8 percent for the year,

and to a first approximation, the F's remained constant since they were computed by taking ratios of the luminosity of the isolite source. The

total effect upon R in (l) if allowance had not been made for the

luminosity deterioration of the isolite source would have resulted in

the computed intensities at the end of the year being too low by approximately 10 percent.

Tables 2, 3> and k include the hourly average reduced zenith

intensities from the two-color reduction method for [Ol] 5577 A, Nal

589O-96 A, and [Ol] 63OO A emission lines in rayleighs, the extreme

values, and the average value for each night and for each standard time

of the observing period. The negative intensities in table 3 result

from the low intensity of the 5890-96 A emission and the inaccuracy of

the two-color reduction method. The background intensities from the

5300 A filter for the turret photometer have been previously published

[Roach and Smith, 196^].

*A study of the two-color reduction method and its limitations

has been made by Davis and Smith [196^- ]

.
IV. ANALYSIS AND INTERPRETATION

A first approach in the analysis of the data of tables 2, 3> and

k for seasonal effects is simply to plot the zenith intensities as a function of the date during the calendar year. Figure 2 is a plot of

the average zenith intensities, the probable errors'* and the extreme

values for each observing period for Nal 589O-96 A, [Ol] 5577 A, and

[01] 63OO A. Maxima in May and October for [Ol] 5577 A, May and November for Nal 589O-96 A, and in October for [Ol] 63OO A of figure 2 are

quite pronounced. Table 5> based on the averages for each observing

period, gives the least-squares solutions (treating each emission as equally independent) for the covariance of the three emissions, assuming a linear relationship.

A useful technique for combining seasonal and diurnal variations

of the emissions is shown in figures 3> ^? and 5 for 5577* 5890-9°", and

63OO A emissions, respectively. The 5577 A emission (fig. 3) exhibits

a well-defined maximum in May, and a broader maximum extends over the

observing periods of September, October, and November. The maximum of

the 5577 A emission in May occurs in the evening hours and the fall maximum near midnight. The diurnal variations (fig. 3) display the following: (l) The maximum is at the beginning of the night (May, June, and

December), (2) the maximum is near local midnight (July, August, September, and November), and (3) the maximum is at the end of the night

(January, February, March, April, and October).

The 589O-96 A emission (fig. k) has a definite seasonal maximum

at the November observing period and a broader maximum including the

April and May observing periods. The November seasonal maximum takes

place during the early evening hours, and the April-May maximum near and

after midnight. Two types of diurnal variations are apparent for the

5890-96 A emission: (1) a maximum at the beginning of the night (June,

"^The probable error computation in this study is used as a convenient method to express the intensity fluctuations about the mean

and does not infer "errors" in the measurement of the mean.
November, and December) and (2) a maximum at the end of the night

(March, April, August, and September). For January, February, May,

July, and October no distinct maximum is noted.

The 63OO A emission (fig. 5) has a well-defined seasonal maximum

during the October observing period occurring during the early evening

hours. For the other observing periods, the maximum is also at the

beginning of the night probably due to the post-twilight effect.

It is interesting to note that characteristic diurnal variations

seem to be associated with the seasonal maximums. In figure h, for

589O-96 A, the diurnal maximum at the end of the night appears as both

seasonal maximums are approached and, in figure 3> 5577 A does likewise

for the spring maximum. The diurnal maximums at the beginning of the

night occur for 5577 and 589O-96 A when both seasonal maximums have been

reached and a decrease in intensity begins. The 5577 and 589O-96 A

diurnal variations for the months December, 1961, and January, February,

March, and April, 19^2, are similar. The correlation coefficient for the

linear least square solution based on the hourly averages of each of the

five observing periods is 0.84. In figures h and 5; "the diurnal maximum

near local midnight takes place for 5577 and 63OO A as the fall maximum

is approached.

The annual average diurnal variation and the probable errors for

the three emissions are given in figure 6. The probable errors in

figure 6 for all three emissions are very large. The 5577 A annual

diurnal variation result suggests a broad maximum centered near midnight,

but as has been noted from figure 3> this is representative of only k

observing periods of the calendar year. The ^8^0-^6 A annual diurnal

variation exhibits no significant variations, but in figure k- there definitely is evidence of diurnal variations as has been discussed.

Obviously, there is no single type of diurnal variation for 5577 A and

589O-96 A emissions which is representative for a period of one year.

The post -twilight effect of the 63OO A emission is apparent in figure 6

and is present during the entire year.
The average intensity of 589O-96 A and 63OO A relative to 5577 A

is

5577 : 6300 : 5893 = 1 : 0.39 : 0.22.

Figure 7 displays the ratios of monthly average intensity of 589O-96 A

and 63OO A relative to 5577 A.

Chamberlain [1961] discusses airglow annual variations and makes

the following summary statements describing the results of several

investigators:

(1) For 5577 A it is most difficult to establish a yearly variation due to the night -to -night fluctuations and the apparent sensitivity of any yearly variation if it does exist upon the latitude of the

observations

.

(2) The 63OO A emission probably possesses very little seasonal

variation after post-twilight and pre-dawn effects are eliminated. It seems likely that earlier results which reported a maximum in winter

and minimum in summer were contaminated in various degrees by OH.

(3) Several observers have found for Nal 589O-96 A a maximum in

Vinter and a minimum in summer similar to the seasonal variation of

Nal 589O-96 A in the twilight airglow. However, the OH contamination

is also serious for these measurements at 5893 A.

Roach [1955] gives a review of observational results in airglow

photometry. A part of this publication is a summary of the seasonal

behavior of [01] 5577 A, [01 ] 63OO A, and Nal 589O-96 A emissions from

two important investigations at mid latitudes [Pettit, et al., 195^j and

Dufay and Tcheng Mao-lin, 19^6 and 19^7]. Figure 8 includes the monthly

average values, the probable errors, and the extreme values for 5577> 589O-96, and 63OO A emissions from the study by Pettit, et al. [195^] at

the Cactus Peak Observatory (geographic latitude 36 °N) for the period

from November I9U8 to March 195^. Figure 9 is the comparison by Roach

[1955] of the smoothed results of Pettit, et al. [195 1!-] (CP) with the

results of Dufay and Tcheng Mao-lin [19^6] and [19^7] for the period

19*4-1-19^3 at Haute Provence (HP) (geographic latitude 44 °N) normalized

to the Cactus Peak results.
Roach [1955] summarizes the seasonal results of Pettit, et al.

[195^] as follows:

(1) For 5577 A the sporadic variations of intensity are so great as to cast doubt on the reality of any seasonal variation. If

a straight line representing the overall mean intensity (259) is drawn

through the 5577 A plot of figure 8, it departs only very slightly

from the shaded portion in three parts of the plot in March, September,

and December, corresponding to a minimum, maximum, and minimum,

respectively.

(2) In the case of 5^93 A (NaD), the seasonal variation is well

established with a maximum in November and minimum in July.

(3) The 63OO A emission shows a seasonal variation roughly

similar to that of NaD, but with smaller amplitude.

(k) The seasonal variation of CP and HP are strikingly similar.

It is apparent from these reviews by Roach [1955] and by

Chamberlain [1961] that it is difficult to determine seasonal trends

from photometric observations, since considerable night -to-night fluctuations tend to obscure seasonal variations and the spectral purity of the

deduced emission intensities is in question due to the OH contaminations.

Also, care must be taken in comparing results from other investigations

because of the possible latitude dependency of the seasonal trends.

Probable errors and extreme values have been given in this study

to substantiate our described trends. The seasonal variations, from our results, are within the probable error of each of the emission's nightto-night fluctuations . However, the annual average diurnal variations of

this study for 5577 and 5^90-96 A are not representative of even the

monthly average diurnal variations. The 63OO A annual average diurnal

post-twilight characteristic unquestionably is a general feature of its

diurnal variations, but any other maximum is a function of the season. The OH contaminations of deduced emission intensities from

photometric data have been treated quantitatively by Roach [1963] and

Davis and Smith [196k]. The 5577, 589O-96, and 63OO A emissions can be

significantly contaminated by the OH bands (7 - l), (8 - 2), and (9 - 3)

7
with the band heads near 5562, 5886, and 6256 A. Krassovsky, Shefov, and

Yarin [1962] give estimates of the mean zenith intensities for the OH

bands (7 - l), (8-2), and (9 - 3) as 20, 60, and 1^0 rayleighs, respectively. Also, they tabulated the relative intensities for the R, Q, and

P branch lines for the OH bands. An estimate of the OH contaminations

for the three airglow emissions under consideration was determined by

utilizing these absolute intensities for the OH bands, the relative intensities for the Q branch at the Q-, and Q2 lines, for the R branch at the

peak line, and for the P-, and P2 branch lines, and the transmission

characteristics of the interference filters . The OH contamination com- puted in this way was 5 > 7, and 17 rayleighs for the 5577, 589O-96, and

63OO A emission data, respectively. According to Bates [i960] and

Chamberlain [1961], several investigators have found little or no sea- sonal variation in the OH emission intensities. However, night -to -night

variations may occur by as much as a factor of two. Since the annual

average deduced intensity of 5577> 589O-96, and 63OO A was approximately

190, k-0, and 70 rayleighs, the OH contamination at these wavelengths

could be, on average, 3 percent for 5577 A, 18 percent for 589O-96 A, and

2k percent for 63OO A. The 589O-96 and 63OO A contaminations are serious

for the low intensities, but it is not likely that the contaminations

could have seriously affected the seasonal trends indicated in figure 2

since the maximums are several times larger than the minimum intensities.

It is the opinion of the authors based upon the above discussion that the

seasonal variations described from figures 2, 3> h, and 5 for the three

emissions are valid.

The airglow data reported in the IGY Annals, Volume 2k (1962)

includes 5577, 589O-96, and 63OO A data for the calendar year 1958 at

Tamanrasset (geographic latitude 22.8°N) which provides additional information for seasonal variations in the tropics. Figure 10 shows the

average monthly intensities for 5577, 589O-96, and 63OO A emissions at

Tamanrasset for the calendar year 1958 and the results of this study.

The Tamanrasset observations were obtained in the direction of the celestial pole and referred to the zenith. Consequently, assuming a height of

8
100 km for the 5577 and 5^90-96 A emissions, the observations would "be for an effective geographic latitude of 25 °N and geomagnetic latitude

27°N and assuming a height of 300 km for the 63OO A emission gives an effective geographic latitude of 28°'N and geomagnetic latitude of 31°N.

The agreement is very good between the seasonal variation at the two

tropical stations, Tamanrasset and Haleakala, for 5577 and 589O-96 A

emissions. However, the Tamanrasset seasonal variation for the 63OO A

emission is not similar to the results of this study. Figure 11 shows

the good agreement between the mean diurnal variation of Tamanrasset for

the year 1958 and the mean diurnal variations of this study (196I-62) for

the three emissions

.

In comparing the absolute intensities of one station with another,

it is difficult to rationalize the agreement as real or as a coincidence.

Each station*s absolute intensities may be significantly affected by

errors in the absolute calibration, different geographic or geomagnetic

positions or because the data were obtained at different epochs of the

solar sunspot cycle. Table 6 summarizes the information that may be pertinent to this study for the two mid-latitude and two tropical stations

being considered.

One similarity in the seasonal variation of the three emissions at

all four stations is an apparent fall maximum. The tropical seasonal

variation for 5577 and 5^90-96 A emissions exhibits a spring maximum

which is not conspicuous in the mid-latitude results. The 63OO A emission seasonal variation in the mid-latitude stations suggests a minimum

in summer and maximum in winter. The Tamanrasset tropical station also

indicates a winter seasonal maximum and summer minimum, but the contrast

is much more pronounced than the mid-latitude results . The Haleakala

tropical station indicates only a fall maximum for the 63OO A emission.

Possibly the difference in the two tropical stations for the 63OO A

emission is because the data from Tamanrasset were obtained near sunspot

minimum.

The mean diurnal variations for the tropical stations are similar.

Both tropical stations indicate a second broad maximum for the 63OO A
emission after local midnight. This tropical 63OO A emission maximum in

the mean diurnal variation after the post-twilight effect is due to the

tropical 63OO A emission activity observed and reported by several investigators [Barbier, Weill, and Fafiotte, I96IJ Roach, Steiger, and Brown,

1964; and Davis and Smith, 1964]. For the Haleakala station, it has been

shown to be associated with the equatorial (geomagnetic) anomaly in the

ionosphere [Roach, Steiger, and Brown, 1964]

.

V. SUMMARY

During the year July 1961 to July I962, at the Haleakala Observatory, evidence from this study suggests that the tropical [Ol] 5577 A,

[01] 63OO A, and Nal 5890-96 A emissions exhibited seasonal variations.

All three emissions indicate maximums in the fall and the 5577 A and

5 89O-96 A emissions suggest maximums also in the spring. From the com- parison of the results of this study and those from Tamanrasset with the

mid-latitude results from Haute Provence and Cactus Peak, it appears that

the fall maximums are not dependent upon geographic latitude but the

spring maximums for 5577 and 589O-96 A emissions do appear to be only a tropical phenomenon.

The covariance in the seasonal trends of the three emissions,

table 5 > seems to be statistically significant and due primarily to the

common fall maximum. However, it is difficult to rationalize a physical

significance in the statistical covariance of table 5 between the three

emissions. A possible explanation could be that the atomic oxygen abundance at heights from approximately 80 to 300 km covary, on a gross scale,

with season. Reactions involving atomic oxygen [Chamberlain, I961] could

then result in emissions at these three wavelengths. The Nal 589O-96 A

emission seasonal variation is very similar to that found by other

observers, and there is little doubt that the fall maximum is a common

feature reported by almost everyone who has monitored this emission in

the northern hemisphere, regardless of the observer T s latitude. The

spring maximum found by this study and indicated in the Tamanrasset

results, however, may have a latitude dependence since the mid-latitude

stations considered did not have this second maximum.

10
The apparent seasonal diurnal dependency for 5577 A and 589O-96 A

Is an interesting result of this study. The 5577 A and 589O-96 A high

correlation coefficient In the covariance of the hourly averages for

observing periods December 1961 through April 1962 could be significant

because this suggests a common effect somewhere in the chain of events

which ultimately results in the emission at these wavelengths.

ACKNOWLEDGEMENTS

We are especially indebted to Walter Steiger of the University of

Hawaii for his cooperation and assistance in obtaining the data and

for the invitation to work at the Hawaii Institute of Geophysics for

the academic year 1963-6^ during which a significant portion of this

analysis was completed. Also, we are indebted to Herbert Mann, Edward

Marovich, and Charles Purdy of the National Bureau of Standards for

their part in the acquisition of the data. We are extremely grateful

for the criticism during the preparation of this paper by Franklin E.

Roach of the National Bureau of Standards. Finally, a significant part

of the financing of the project has been through NASA grant R-l8.

11
12
Table 1

Summary of the constants used for the reduction

of the turret photometer by (l) for the

observing period in September, I961

Filter F W I T

5300 — — 8.93 1.053 —

557T I.83 29.4 4.88 1.038 o.64o

5890-96 6.08 15.5 1.47 1.047 0.375-0.607

6300 24.8 25.5 O.36 1.033 0.695

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32
Table 5

The least -squares solutions based on averages

for each observing period for the

covariance of the three

emissions in Figure 2

5890-96 = 0.66 x [rayleighs 5577] - lk.6, R = 0.57 (all data)

5890-96 = I.39 x [rayleighs 63OO] - 53-4, R = O.59 (all data)

5577 = I.98 x [rayleighs 63OO] + k2.f, R = 0.62 (all data)

33
Table 6

STATION

GEOGRAPHIC

LAT : LON

GEOMAGNETIC

LATITUDE

Haute Provence : Kk°N : 6°E 46°N

Cactus Peak i 36°N 118°W if3°N

Tamanrasset 23°N : 5°E ; 2 5°N

Haleakala 21°N I56°w 21°N

34
3

O

O

UJ

UJo

uu

1 1

(\(\ Z = ZERO

SL = STANDARD LIGH

SK = SKY

yu T

onoU

7ft (U

r.n 5300 6300 | 5893 5577

uu 1 1 '

1

1 1 1 1

Cft III 1 II 1 00 1 '

At\ p

<»U i h n

nn n SK

JU

1 1 S -

i(\ n

c;l

i-\)

!

i J

i n n n n A

SL

n \F\

J 10 in

TV n r -t L r n

A. II . A i J i^rA Z

J 1

2036 2031

150° W STANDARD TIME

2026

Pig. 1 - Illustration of a strip chart recording from the zenith

photometer

.

35
400 1 1 1 . i i i , . ^

A (Oil 5577A • I /— — ~' \ ^~~ » -

/

/ - /

\ / \

300 / . /X * ^ ~J /

A . , , _ \ xA y/O /V>\ V- x^ 1/ / ^vA^ y/////\ * 1 -X^^/Y/>>~rv/^/v ? vrXA

200 l/f/ /

X^'/ // / /^^ v/\ •*"—\ 1

100 ^--'

^C- / ' "-^-^

\ ^-^ / s _ V •

1 1 !

HAL 1961 -1962

No I 5890- 96A */\

?00

'ftA »-

100

~ A /-"A// /^AV-

/ _-—. /

y ii" / i 'S'~' ^C^^^eSS^^^ ' N

—^> ^0=f«=z^ ^ N

*^

600

1 1 1 i i 1 1 1 i i [0I16300A

soo

1 |

1 \

1

| / | 400

/

\ ~~

/ |

/ .

/

(

300 -

/ )

/ I

/ 1 t . I 200 — / A , _

/ f/\ i /\ * r / A

/ N /xZkk -

/ 1/ s)\./\ N

100 V ////// z>

n —T"'

, "T" i *"*r" i "~"i i i i

J FKA HJjJA S NO

1962 MONTHS 1961

Fig. 2 - The average zenith intensities, the extreme values, and the

probable errors for each observing period for [Ol] 5577 A,

[01] 63OO A, and Nal 589O-96 A.

36
[01] 5577A

UJ

o

<

o

z

CO

Fig. 3 - The 5577 A intensities plotted as a function of local time

and month. Isophotes are in rayleighs

.

37
No I 5890 -96A

Fig. k - The 589O-96 A intensities plotted as a function of local

time and month. Isophotes are in rayleighs.

38
19 —

21 —

22

uj 23

Q

a. 00 <a

z

<w 01

02

03

04

05

06

[01] 6300 A

•75-"

* 50

50

100^

'• 75 -\V/ \

s \ /" /'

\

i } ) J

/ '

75

i /

50-

Fig. 5 - The 63OO A intensities plotted as a function of local time

and month. Isophotes are in rayleighs.

39
300

200

100

[Ol] 5577A

100

No I 5890-96A

200

100

[Ol] 6300A

19 20 21 22 23 01 02 03 04 05 I50°W STANDARD TIME

06

Fig. 6 - The average diurnal variations and the probable

errors for [Ol] 5511, [Ol] 6 300, and Nal 589O-96 A.

^0
1 1 1 1 1

1 y^ 1 1

C_3

s y S

y

/ s y s \ \

Z

— — O

x N

>v \\ — N \

\

\

— CO

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\ _ \ — «X

1

\

\

1

/

/

/

/

m

d

LU

C\J d

LU

J

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/

/

/ — <

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o

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(0 mm

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m «s

If) A

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1 1 1

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Z

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C\J CO

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o00

a3

On

I O

ON OO

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s

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0) LT\

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0) O

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0) A

EH

o

•p

t-

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in
i

1

1 1 1 1 1 1 r

[01] 5577A

J I I

I I

J L J 1 I I JFMAMJJASONO I I

MONTHS

Fig. 8 - Seasonal variations of [oi] 5577, [oi] 6 300, and Nal 589O-96 A at

Cactus Peak for the period November, l$kQ to March, 195^. The inner curve represents the averages, the center curves represent the probable errors,

and outer curves represent the extreme values. After Pettit, et al. \i95k]

.

I

k2
400

1 1 1 1 1 1 1 1 1 1

[01] 5577A — A "

300 / V

y \ \ ^^~ ^^ \ v ———^__^^^ / —~ —s "V^V

\ / V /

200 ^^/ —

100 HP 1941 - 1943 CP 1948-1954

1 1 1 1 1 1 1 1 1 1 X Na I 5890-96A /"* >*

LU /

_I /

< N

S.

HP/

/

CP>^ z 200

CO X\ 1/

COLU . 1/

z.X

\ ^^ F

o \ \ /

or VV \\. A/ 00

100 ^^<^ \ /

S y

1 1 1 1 1 1 1 1 1 1

[01] 6300A

200 Vs _^

S.N

S ^——->«£^"

- >yN

V- _ —' HP ,.*" ^» *^

">. ^

100

1 MAHJJAS0ND 1 1 1 1 1 1 1 1 1

MONTHS

Fig. 9 - The comparison by Roach [1955] of the seasonal smoothed results

of Cactus Peak (CP) with the results from Haute Provence (HP) normalized

to the Cactus Peak results for [Ol] 5577, [Ol] 63OO, and Nal 589O-96 A.

^3
JUU

1 1 1 1 1 1

[01] 5577A

1 1 i i TAM — /Ahal\ 1

200 — •/ s \ „Sl A —

/ / s ^^ ^ \

s

' // v^

"^ —^ / \

- / / \ / x^ >

/

100 ^^s/^ —

TAM 1958 HAL 1961- 962

1 1 1 1 1 1 1 1 1 1

Mo I 5890-96/V

A

/ \

200 tam/ \

/

/

/

A x hal/ \

100 '-/—'"A

\ S \ *s \1 s -^ ^- *v V,-'

I I I i i ^T" 1 1 1 1

[01] 6300A

A 300 / X

J -

TAM ^^" r

200 _ ^ i \ i \

\ i \ i \ i y. \ i j

100 \ j / \ \. ^^ 0- 1 1 1 1 1 1 i i

1

1 J F M A M J J A S N MONTHS

Fig. 10 - Seasonal variations of [Ol] 5577, fol] 6 300, and Nal 589O-96 A

at Tamanrasset for the calendar year 1958 and at Haleakala for 1961-1962.

kk
300

200

100

[01] 5577A

HAL

TAM 1958 HAL 1961-1962

LU

_l

>-< 100

IEz

CO

to

Ulz

1-X

COK

CD

200

100

No I 5890-96A

TAM

[01] 6300A

\

TAM

•HAL

18 19 20 21 22 23 00 01 02 03 04 05 06 STANDARD TIME

Fig. 11 - The average diurnal variations for [Ol] 5577, [Ol] 6300, and

Nal 5890-96 A from Tamanrasset and Haleakala.

^5
REFERENCES

Barbier, D., G. Weill, and M. Fafiotte, (1961) C. R. Acad. Sci., 252, 3102.

Bates, D. R., (i960) The airglow, In Physics of the Upper Atmosphere

(J. A. Ratcliffe, ed.) Chapter Y, 219, Academic Press, New York.

Chamberlain, J. ¥., (1961) Physics of the Aurora and Airglow, Academic

Press, New York.

Davis, T. N., and L. L. Smith, (196k) Geophysical Research Report No. 10,

University of Alaska, College, Alaska.

Dufay, J., and Tcheng Mao-Lin, (l9*+6) Ann. Geophys., 2, 189.

Dufay, J., and Tcheng Mao-Lin, (l9*+7) Ann. Geophys., 3, 153

Krassovsky, Y. I., N. N. Shefov, and V. I. Yarin, (1962) Planetary and

Space Science, 9> 883.

Pettit, Helen B., F. E. Roach, P. St. Amand, and D. R. Williams, (195*0

Ann. Geophys., 10 , 326.

Purdy, C. M., L. R. Megill, and F. E. Roach, (I961) J. Res. NBS 65C

(Eng. and Instr.), 213-

Roach, F. E., (1955) Ann. Geophys., 11, 21*+.

Roach, F. E., (1963) The Nightglow, Advances in Electronics , 18, 1.

Roach, F. E., and A, B. Meinel, (1955) Astrophys. J., 122 , 530.

Roach, F. E., and L. L. Smith, (196*0 NBS Technical Note No. 21*+.

Roach, F. E., W. R. Steiger, and W. E. Brown, (Sept. 196*+) Technical

Report HIG-6*+-l6, Hawaii Institute of Geophysics, Honolulu, Hawaii.

Smith, L. L., and R. B. Alexander, (1963) IQSY Instruction Manual, No. 5,

Part II, Airglow, IQSY Secretariat, London.

k6

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