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AVSW C '-TR> !)9--3W s c;

59-39

Vol I

HEADQUARTERS

AIR FORCE SPECIAL WEAPONS CENTER

0 AIR RESEARCH AND DEVELOPMENT COMMAND

0*KIRTLAND AIR FORCE BASE, NEW MEXICO

1'

lop -

........

A STUDY OF LUNAR RESEARCHi FLIGHTS

Vol I

by

L. Reiffel

ARMOUR RES.EARCH FUDYO

of

Ullnois Jnmt~itule of cm~o
Tlt_59,, 39

_Vol 1

HEADQUARTERS

AIR FORCE SPECIAL WEAPONS C ENTER

Air Research and Development Cominand

Kirtland Air Force Base

New Mexico

Major General Charles M. McCorkle

Commander

Colonel Carey L. O'Bryan, Jr.

Deputy Commander

Colonel Leonard A. Eddy

Director, Research Directorate
T ItR _ 59- 39

Vol I

(Mnclasnified Title)

A STUDY OF LUNAR REYSEARCH FLIGHTS

by

L. Reiffel

With contributions by

R. W. Benson J. J. Brophy

I. Filosofo N. S. Kapany

D. Langford W. E. Loewe

D. Mergerian 0. H, Olson

V. J. Raelson C. E. Sagan

P. N. Slater

19 June 1959

Research Directorate

AIR FORCE SPECIAL WEAPONS CENTER

Air Research and Development Command

Kirtland Air Force Base

New Mexico

Approved-

/&rAVID R. JONES

Lt Colonel USAF

Chief, Physics Division

IEONARbD A. kEDT

Colonel US F

Director, Researlh Directorate

Project Number 5776-- 57853

Contract Al' 29(601)- 1164
""K i '.,I. M l'' E•i•N 4

We wish 'o i. , , . A>, !-k;i[r-., 1)iDrector of Yerkenrý Observatory

and consultant to the Physics Division of ARY, for a number of very

enlightening discussions of thin work centering efpecially around interpretation of various theories of the mrGn's structure a.nd origin and descriptions

of the probable nature of the Inmar s.rcface. D].ring initial phases of the

work, Dr. Kaj Strand, Director of the Naval !(esearch Observatory and also

a consultant to AR', contribdoted valuable advice, especially on spectroscopic

problems. W. E. Loewe of ARF gave halpful admin.istrative assistance.

Throughoit the project Lt. A. Guenther of AFSWC provided constant

encouragement and con-siderab)e assi stan( e.
TR- 59. 39

Vol I

Ao) ;' iJ( AC''

Nuclear detonatliozns in thc vicinity of the moon are considered in this

report along with sci entific itinor-' ation which mnight be obtained from such

explosions. The military aspe(t' is aided by investigation of space environment, detection of nucl.ear device testing, and capability of weapons in space.

A stady was condeucted of various theoiit:eq of the moon~s structure and

origin, and a description of the probable nature of the lunar surface is given.

The areas discussed in some detail are optical lunar studies, seismic observations, lunar surface and magnetic fields, plasma and magnetic field effects,

and organic matter on the moon.

PUBLICATION REVIEW

This report hz~s been reviewed and is approved.

CA .BRYAN, JR.

Colonel USAF

Deputy Commander
TALIAK 1 ( NiN

CHAPTER J. INT11 D -) UCG IO)N ....................... . ..

CHAPTER II. (See Vol, I1 of Report)

CHAPTER III. OPTICAL STUDIES REL-A.TED TO THE LUNAR

RESEARCH FLIGHTS .......................... 123

CHAP TE IV. SEISMIC OBS.RVATIONS ON THE MOON........ 153

CHAPTER V. THE HIGH ENERGY RADIATION ENVIRONMENT

OF THE M OON ................................ 179

CHAPTER VI. LUNAR SURFACE AND MAGNETIC FIELD OF

M O O N ........................................ 207

CHAPTER VII. SOME ASPECTS OF PLASMA AND MAGNETIC

FIELD EFFECTS .............................. 221

Appendix I. Acceleration of Electrons in

Mirroring Plasmas

CHAPTER VIII. ORGANIC MATTER AND THE MOON.. 262

Appendix I. Survival Time of an Irradiated

Population

Appendix II. Current Attitudes and Activities

Regarding Biological Contamination

of Extraterrestrial Bodies

CHAPTER IX. (See Vol. II of Report)
Chapter i

INTRODUCTI0N
IN I'ItODUC'TJION

!-tapi dly acce.ierating progreen in ppac e techr(o)ogy clear-ly x-equirete

evaluation of the scientific experimncto or other hurman activitiesi which

might be carried out in the vicinity of the earth's natural satellite, Among

various possibilities, the detonation of a nuclear weapon on or near the

moon's surface has often been suggested. The motivation for such a detonation is clearly threefold: scientific, military and political.

The scientific Information whicht might be obtained from such

detonations is one of the major subjects of inquiry of the present work. On

the other hand, it is quite clear that certain military objectives would be

served since information would be supplied concerning the environment of

space, concerning detection of nuclear device testing in space and concerning

the capability of nuclear weapons for space warfare. The political

motivations for and against the detonation of a nuclear weapon are equally

clear and aie, in reality, outside, the ncopeof the present work. Obviously,

however, specific positive effects would accrue to the nation first performing

such a feat as a demonstration of advanced technological capability. It is

also certain that, unless the climate of world opinion were well-prepared

in advance, a considerable negative reaction could be stimulated. Obstacles

to detonation of a nuclear weapon on the mnoos, from a Scientific viewpoint,

center around environmental dipturbances, biological contamination, and

71ý
radiological contamination, only thc ý .ofit of. which is unique to the nuclear

weapon. While the present efforts have been~ designed to explore scientific

aspects of lunar experimentation, including detonation of a nuclear weapon

aýmong other Rossibilitie -s, we nevertheless have felt some obligation to

consider the obstacles listed above and at least a beginning has been made

in an evaluation of some aspects of the contamination problems.

A central theme, which runs through many of the projected experimental

situations, envisions placing of a maximum of three identical instrument

packages at arbitrary locations on the visible face of the moon prior to any

possible nuclear detonation. These instrument packages would be equippedI

to make a variety of measurements treated in the following chapters, and,

as such, only certain operations would require a nuclear detonation. The

instrument packages, in general, would accumulate very valuable information

on the way to the moon, while emplaced on the moon before any detonation,

as well as during and after a possible nuclear detonation. The location of

the instrument packages need not be pre-determined but is presumed to be

known by virtue of suitable markers.

Clearly, the landing of three complex instrumentation packages on the

lunar surface with "state of the art" techniques, either today or in the near

future, must be considered a maximum effort. It is presumed obvious to

the reader that many valuable measurements could be performed with only

one instrument package, and for certain of the observations to be treated in

the present work, only terrestrial observations are required. in no case

have we attempted to detail the design of a suitable ;instrument package
combining the tui-. iu.i ,iIe ( C i ry C', 1,) Pe -i.),'l) the many expecilnents discussed.

Such an effort woIJ i have been l'are And pernaps entirely in appropriate at

this early stagc of overall planning f,)r possible lunar experimentation.

In conclusion, it should perhaps be emphasized that the course taken

has been the exploration of a fairly laarge number of problems and experimental

possibilities without, in any given instance, attempting to be exhaustive, It

is evident that many aspects of the problems which are treated here remain

untouched or, at best, have been only qualitatively considered. Furthermore,

it is almost unnecessary to point out that a vast number of possible experiments,

not even mentioned or perhaps not even considered by the present group,

should be carefully evaluated. The enormous effort that would be involved

in any controlled experiment on or near the moon demands nothing less than

an exhaustive evaluation of suggestions by the many qualified persons who

have begun to think about this general problem.
CHAPTER II

(See Vol. II of Report)
Chapter III

OPTICAL STUDIES RELATED TO THE LUNAR RESEARCH FLIGHTS
( l i. r 'l" r I

OPT IG A(, ,UITt NJ, P I,AAI II) TO () I i, IJIJNAP I I;AR( H I .t'.JGII'S

Opticral atidjis ,Ildereitalkell in this ana ', of a t ln ' :acoarch flights

cover the following three a mca a: (a) ,ar;(ious ob,ajeAvational p aarameters

t. ... e" ...... Y ,r" t l v W Lkc I a p ia L i Oil iiM- way to

the moon, in the vicinity of the moon or on the surface of the moon; (b)

stellar spectroscopy and high speed spectroscopy of the lunar blast using

available astronomical and high speed photographic equipment and (c)

measurements on the thermal conductivity of the lunar surface using infrared

emission inea surenments.

Visibility data has been compiled which would permit the calculation

of required target intensity in order that it be visible against a background

of known luminance. H-lowever, since the moon is not of uniform luminance, .

the results are not rigorous. Ranging from unresolvable points to large

irregular areas and front bright apots to deep -hadows, arranged in most

i- regular fashion, the moon represeueiiL a dif if d ill bha l<groiund in which to

search for a small area. 'The). edor,, ta rgt iotentitie6 must be substantially

greater than indicirate d by (-alciiJAi at),, on a Ita iln i an itlorrn bacckground. With

these con,-d,--rati ia.i ilti , 1 t-) it[Ial ex vanaaion of various types of

markers is presented.

Spectroscopy of the lanara blhist area woauld yield u1neful information

on the composition ofa' t aietciai l )it the moon'an :-a;Ictf;ice Detailed considerations

i 1/
are given to the Iio,.: ;,ý•,gI ipeed npectroscopic

parameters on the v sible higl, ema.sit~m bv tiei !),as:t. The influence of

atmospheric absoiption and to iou aori hbe fon spectrographic information

yield by existing -itellar spectrographs io presented in a tabulated form.

Balloon carried telescope and spectrograph op to an altitude of approximately

150, 000 feet is considered., Whereas, a number of practical problems are

known to exist in high altitude balloon telescopy, it in clear that an extension

of the TjV spectra, as well as freedom from atmospheric turbulances, will

be achieved by going above, say, 130 - 140, 000 feet.

In the past, thermal conductivity of the lunar surface has been

calculated by measurements in variation of temperature on the moon's

surface during a lunar eclipse. With the nuclear detonation acting as a

strong heat source and with the availability of highly sensitive infrared

detectors, it seems possible to calculate thermal conductivity of lunar

surface to a high degree of accuracy. The influence of atmospheric absorption and turbulance on these measurements is tabulated for various existing

telescopes and infrared receptors.

Section One

Marker Visibility

The problem of sending a vehicle to the moon and of landing an

instrument package on the moon raises the question of tracking in flight and

accurate location on the surface of the moon. Visual optical approaches to

the problem are preferred because of the great sensitivity of the human eye

1 z?5
and the high /)1ec-islol, in location iposoiibik In l (odern Optics. Of prime

interest is the viibihlity arid deteciahilhtv of varioul ocihie markers. These

fall naturally into two c'a ,Jec , those that are s elf Alurninoutt by virtue of

consunmption of cell co(i:ined fueo or tbIo.cd cnergcy and those that are

lumninous by virtue of reflected otunlight. The need for keeping weight and

NiL,' to a 11 IiOiilillX t I - l -it Lk i 1te opLicl pi JJ-obtJ-in to hlreshloud or as near

threshold conditions as possible.

It is generally known that threshold illumination from a point source

detectable by the eye depends upon background brightness, color and

adaption level of the eye. Three such background levels, full moon, dark

moon, and night sky 3000 miles distance from full moon are considered in

detail.

A. Visual Thresholds of Disks of Light

Two investigations of visual thresholds of disks of various brightnesses in uniform fields of various brightness levels by Blackwell1 and by

Tousey2 are of importance and form the baais of most visibility studies.

Their results agree remarkably well, although their experimental conditions

were r-.•,e different. Fig. I presents their' data in graphical fornm. It

displays threshold iiLUi nMi18 tih oi e a poiot S•oiu cC which is detectable at

**fc nt ED- a k •c T "t.I b.. gi.. ..... s. :J I I

which subtends less than one minute of arc at the eye. Based on observations

of Tousey and Hulbert3 a point sour( c is very difficult to find when the

illumination is just thre shold of even twi( e the va] e. Up to five times
"- 7

-- 8

"--9

C1

°i0

-1

-11 -10 -9 -8 -7 -6 -5 -4 -3 -2 -1 0

Logl 0 Bo (candles/cmz)

FIG. 1 .. THRESHOLD ILLUMINATION FROM POINT SOURCE

DETECTABLE BY NAKED EYE AS FUNCTION OF

BACKGROUND BRIGHTNESS
threnliold value i3 iaadovately ha rd tit '•id. L'i, (Mi\eri threoinod illumination

(vertical axin) of F ig' 1 to noul ce intenasity noceaa•a y for detection Yone has

only to o- ultiply 1,; by the ffq o of10 u the diUtaIc e, Which in thin cane in4

?.40, 000 railen), exprp csfned In eletimotors. 'ito iilti oui. ty valuea shown in

f02ig. Z were obtained in 11iit way

Iig. 2(a) proeentil average bhiightnesn values of light and dark moon

and of night oKy 3000 mileh fromh the moon's surface at full moon. The source

intensities necesnary for detection with the naked eye against these back..

grounds are also indicated.

B. Telescopes and Improvement of Visual Thresholds by Magnification

A telescope increases illumination from a point source relative

to the brightness of a uniform background and therefore makes it possible

to see some sources which are below the limit of the naked eye. Tousey and

Hulbert 3 derive an expression for the gain by the use of telescopes which

can be written an

7 7$' (44 (4 (1)

in whici' D diarnete r of objecti ie lean;,

P :2 diametoer of i'yG pI.pii,

M :m magnification,

t :2 tran ramiansion factoir of telencope,

i lflumination oar objective lens when point source appears at

thresahold,

i' :2 unaided eyc thrkeutold.

(i'/i) itproiveimett if It tlr'tsitold duc to lelescope.

! .,;,
I ight Moon Oa ik Mioni

Bo ()0, ?;5 :andler• / l 130 0. 00002.5 candles/cm

/

Source of ( /

1.3 x 10 1 3 candletr Source 1. 3 x 109 candles

visible visible

Sky 3000 mi. from moon

B0 = 0.00000 25 c/cmz

(full moon)

FIG. 2(a) - SOURCES VISIBLE, TO NAKED EYE AGAINST LUNAR

BACKGROUNDS

0. 4 mile diameter

13 miles diameter Q0

700 ft diameter

FIG. 2(b) - WHITE SPHERES VISIBLE TO NAKED EYE
thini to). told Wi ll kil 0 "o n lo e.il( lcnliltinmn l in i n awe

fIt derviw A( thuii 10P tyŽ' ce 011)1 Bil~ aill)iIoijII 1)ii Bd to Ito made( with r efipect to

tho e mb.ive oiiie of e'ye pupil ankid enId flik il Iof the teocIn(ope, Sinece the t 1ze

of Ohe Pupil. VarPien) withl adaptation It voI he ant lourn pt ionl is no~t atrUicftly true,

anid them oefome the £01o)O mux niiit he AuJ~ Ile4d only an anl approximation)

Table I) f ho-w the i1(1W nt'xge to he gnJahoeI owith the un eO of tele n copefs in thle

visibtility of point CjOUPcr CO C agalnt full moit btna ckground.

bible I f

'101 1coj)C with MI 161)(in.

Candles for Detection

D(in.) MIi/ Against Avg Full Moon

Eye 1 113, 000, 000 mega -candles

1 16 1712 75, 000 if

2 3? 630 20, 600 11

8 128 11 ,000o 1,200

20 320 68, 000 190

40 640 2,74, 000 50

100 1000 /90, 000 16.5 "

200 1000 900, 000 14.5

G . Vi C ibillity of' Dl)f~ LOttlnadSe d Sh1Pi~eie

'lous.oy banoo collsidero~ J.1thi1 pr:oWlem iii connection with earth

satellites but his findings can 1)0 eastily extendedl to inoonl orbitersl. The

angular Olistributioo of luiminosity of a nphere illuminated by the sun was

considered for. two sipecial case Cn; a per'feet nipecilar reflector', and a perfect

diffuse reflector which obeys J~amcbert'sj Jaw, The expmenrionC for

lumninous intexiflshy, f., inca- tin e 4 at a din tan)c( -whicih in; large conmpar ed to

'0
tlbe radiIis, R , a re

Specuia.': k" / 7

Diffuse: _P 3.> ..... 0) 4 .

Where 0 is the angle between the directions to the sun and the observer, E

is the solar illumination, and f is the reflectivity factor of the aphere

material. The specular sphere has a constant luminosity in all directions

since the expression for I does not contain 0. The diffuse sphere goes

through phases like the moon and is brighter than the specular when viewed

"full" but di.ninter when "new." The two types are equally bright when

viewed at 83, 7 degrees. Fig. 3 shows the angular distribution of luminosity

in the two cases.

The visibility conditions may be computed approximately by making

use of formula (2) or (3) to calculate the luminous intensity for the appropriate

conditions of illumination and viewing. Reference to Fig. 2 will determine

its visibility status for three different background brightness conditions. If

it is not visible to the naked eye, Table I may be used to determine the

apprcpriate telescope to make it visible.

Formulas (2) and (3) apply strictly to ideal specular and diffuse

spheres, respectively. Clearly, no p~ractical sphere will be ideal, either

specular or diffuse, so a decision must be made as to which is the more

appropriate formula. In genexal, this is not a difficult decision to make;

a polished metal sphere approximatcs the specular- case unless it is badly
SunJlght(

Viewed toward sun

Specular is brighter

Viewed opposite Jun

Diffv~se Is brighter

ju l t 81. 7'

FIG. 3 ANGULAR( DISTRIBU11ON OW L-UMI.NOSfI'Y 01Ok' FUJ

AND SP.ECULAR 131)11XRICAL fUE'Tl TEC'voiu JLLTJMINATEIý)
oxidized or corrodod and a opheo covered with a mat white paint approximates

the diffuso caste, 1,;xcoptional urfoface-, could make the decision more

difficult; for example, a mfetal foil which to inflated In flight. If such a

balloon were to present an uneven surface consisting of a large number of

small facets, it would probably approximate the diffuse case even if

individual facets are specular.

Fig. 2(b) shows the size of white diffusely reflecting spheres necessary

for detection with the naked eye when they are fully illuminated by the sun

and appear against the backgrounds of Fig. 2(a). Fig. 4 shows the corresponding size of spheres necessary for visibility with a 40-inch telescope. However,

the values given in Figs. 2 and 4 are based on average background brightness

and do not take into consideration the irregular background that the moon

actually presents. The values are therefore optimistic for those cases in

which the light moon forms the background. Although the average albedo

(reflectivity) of the moon is approximately seven per cent, the reflectivity of

individual. areas varies from about 4 per cent to 30 per cent or by a factor

o. seven. This, coupled with the wide range of sizes and shapes of

individual areas, makes the problem most difficult.

It should be recalled, furthermore, that the detectability data are

given for approximately threshold situations. This corresponds to the

detection of a sixth magnitude star which is just visible to the average eye

only when other conditions, such as the carth's atmoiphere, are ideal. It

should also be noted that, although telkeocopes offer a tremendous advantage
130 ft. dia eter -4 ft. diameter

Z ft. diameter

FIG.. 4 WlFLIDRXSl VISIBLE WITH 40-INCGH TELESGOPE
in visi!ibUty once an object , ,,afed ('•4i -. ( l bw I i, i < tricted field of view makes

the problem of detection tracking miore difficult

D. Identific;ition of Markers

One of the problems associated with markers on the moon is that

of positive identification, The discussion thus far has dealt with visibility

based on brightness contrast between an object and its background. rhi

values given have been threshold or just visible values and were based on

data obtained with uniform backgrounds. With the moon as a background, a

number of possible solutions of this problem will be discussed here.

1. Intense Source

One obvious method of insuring positive identification is to

increase the intensity of source to well above that specified by threshold

requirements. The associated disadvantage is, of course, greater quantities

and size requirements.

2. Color

Inasmuch as the contrasts present on the surface of the moon

are ý,Lose of brightness (white, gray, black),- it seems reasonable that a

colored object or source could be positively identified. Certain pyrotechniques

produce brilliant chromatic emission and fluorescent paints are available in

brilliant colors. Most likely the lumninous efficiency achieved with colored

materials would be lower than with white materials but some efficiency

could advantageously be sacrificed in the interests of positive identification.

Unfortunately, not enough is known about the subject of color contrast against

i;:-egular background in connection with point sources.
A° lute vi);ttellt. eQ~ucc

Ohbvioufi y, A. I'lokec.c. woould be poe iti cty identified if it

emitted lute ,m•tteoiOly ot a hnovk fx eqoeu cy . iy, eitinably, a- frequency could

be chosen) which would suffer a nidnimunm confusion with thosCe arising from

natural pheno-menao Eye re ponae to pulsed sources must be considered,

I1udsion5 givesl the sesfitivity of the vy 1 for nquare pulse of light t seconds

long by the equation

- ("g.. 4)

in which Io is the threshold source intensity for steady light, I is the

threshold intensity for the pulse under the same conditions, and tc is called

the critical duration or retinal action time. Various authors give values of

t. from 0. 1 to 0. 2 sec. If short duration pulses are used, the source

intensity requirements may become prohibitive.

E. Marker Configuration

The effect of size, shape, and contrast in detection of targets

6

has been investigated by Lamar and Associates. Their work was done at

two background levels, daylight and twilight. The average brightness of a

full moon lies within their raxige of operatio. but dark moon and night sky

levels fall far below so that their findings aire applicable only in part. In

addition, their investigation was restricted to uniform backgrounds which

further limits its applicability. Nevertheless, their results with fine line

targets suggest a promising approach to the lunar marker problem. They

found that a line target whosie width subtends only three f;econds of arc is
detectable at a cc.ctrast of i.0 1 o ?,..0 (Contrvast DB.... ). The advantage of a B

line target again'Jt a non .unifornm background like the moon is obvious

since it would generally embrace a range of background levels whereas a

point source is restricted to one ]evel which may or may not be propitious.

F. Sodium Vapor

In 1955 U.S. experiments with sodium vaporization in atmosphere

up to an altitude of 30 -- 40 kilometers were begun for studying winds at

these altitudes and the chemical reactions of gases in these atmospheric

layers with sod.ium. On January 3, 1959, the Russians set a cloud formed

of the sodium vapors in an atomic state. The sodium cloud is discharged at

a specified mement and it glows because of resonance fluorescence emitting

the sodium lines. The yellow light is preferred from the point of view of

visual sensitivity. Furthermore, use of narrow band interference filters

can enhance the contrast.

The brilliance of sodium cloud containing one kilogram of sodium

and discharged 113, 000 kms away from the earth is equal to a sixth magnitude

star which is at the threshold of naked eye visibility against average sky

background. These figures seem to agree closely with calculations based on

experience with sodium emission in flame photometry. Using these figures

it can be concluded that for detectability with naked eye at lunar distance,

the amount of sodium required is:

against sky background - 10 Kgms

against dark side of the moon -- 102 Kgrns

and against bright. side of the mnoon 105 Kgmrn.
The sodhirn V co Lit-evneC s 8 re C ! ~f lVedUdW hen approp i ate

telescope magnification is e iployed an duscuso;ned before.

One might envision a dual purponwe one of solid piropellant rocket motors

as (1) 1'etirydirective devices and (?) marking flares in the present context.

The propellant, containing sodium, would be released on firing the rockets

near the moon. it i6 quitc likely thati e know formulation can be used, thus

precluding the costly development of a new special propellant formulation.

Most likely, formulations currently undergoing development at NOTS will be

applicable. These formulations include metal additives such as aluminum,

boron, and magnesium.

Several factors would bear on the amount of light detectable such as

missile configuration, spinning or tumbling and angle of viewing.

Section Two

Spe ctrographic Studies

The performance of a given stellar spectrograph system examining

emission spectra of the lunar blast depends primarily on two factors: (1)

the amount of energy (in erghi/sec) radiated in each of the emission lines;

(2) the separation and width in angstroms of the closest lines that need to

be resolved. With these quantities known either the optimum exposure time

can be computed or a calculated compromise can be made so that the desired

exposure time is used for spectroscopy or high speed spectroscopy at the

expense of over or undet -exposing some of the lines. Tables relating the

exposure time to the equivalciit stellar magnitude of a lunar explosion are
therefore coinpiVIJ 11 (AJ(ic o ', ~ dllii al 'ho out set that the spectrL;

graphic. recerding ,I>IX, irýt Ui rio.A' i, . it- iiC IIi i ynr ie] i he ) suI stantIall\

improved in the nexi few yeats Fif Sd t hat 1his study is therefore restricte~d to

discussing the !-apabilities of apparatus already in existence at various

observatories. This study is divided into the following three parts: fir,.'1t,

to derive an expression for the speed of a given telescope -spectrograph

system; secondly, to substitute existing values for the various parameters

and, thirdly, to present the results in tabulated form.

Gonside:" a telescope focusing an image of a point source at the

entrance slit of a dispersing system as in Fig. "). The formation of the

point image at S is not diffraction limited, due mainly to atmospheric

turbulences, and to a lesser degree, to aberrations and imperfections in the

telescope system. The size of the image is dependent on the seeing

conditions at the time of observation. Thus, with 3 = 0. 5 x 10-5( = I sec of arc)

the seeing is said to be good and with 1. 0 x 10-5 the seeing is said to be

fair. The size of the image in the plane of the narrow slit is 3 F 1 and, if

this is unobstructed by the slit, the size of the image at the photographic

plate is

.13 (3(5)

This is the width of the spectrum that results from the seeing conditions and

instrumental parameters alone and is denoted by Sy to differentiate it from

S11, the image size parallel to the direction of dispersion. The slit width

i 3)
010

,4V

0 ~

k 0 U

(I (I

0 4-(

q)

IL LH

U UO

0( ub ) Wf 0

g, .,u

Itu ( I (
Sl corresponding to the line., refsolutio imit, / , of the photographic

plate is given by

/•cos /A

where i and "y are the incident and the refracted angles8

The fraction of the flux transmitted, T, by the slit is dependent on

slit width and image inte~nsityi distribution. In order to derive a simple

expression, we assume a uniformly bright square image for simplicity. In

fact, of course, the intensity distribution in a star image generally follows

a bell-shaped curve, It is then given by

10 = -^ te j A5 cos (6)

The effective resolving power R=&- I, of the spectrograph is limited

by /4 when the aperture ratio of the camera is greater than f/40. Under

such conditions

Substituting (7) in (6) we have

A01~ A C4

Now the factors governing the amount of flux incident on the photographic

emulsion are

(1) the atmospheric transmission Kat

(2) the transmission of the telescope .-spectrograph system KTS

(3) the width of the spectrum S 1

(4) the linear dispersion of the spectrograph

,AA
(Gombined, these expren.¶i;ionra I cdme' thn tIix ,H ii tcd by the point o•ur ce BO

(in the solid angle s ubteiided by tbe tele scope ape r lure to the point source) to

1T the ener gy incidenit oil the photog raphi c pla te pe• renoJolution area of the

e-nulsioi.

4- /5'.&J > cos/,

DunhamI suggests that the minimum density for recording an emission line

on a photographic plate is 0.6. Eastman Kodak8 quote a figure of

3. 0 x 10"2 erg/cm2 as the energy required to produce this density in the

visible spectrum on 103a--0 emulsion, the usual emulsion used in stellar

spectroscopy. For photographic resolution this corresponds to 6.0 x 10 6

ergs/resolution area; for 103a-0 emulsion the resolution area is

1. 0 x/ sq mm where/, t 2 0ti. It should be noted that equation (5)

indicates that only for poor seeing conditions (P.: 4 sec of arc) and with the

200-inch telescope working at high resolution (F 3 - 2600 mm, see

equation (7)) does the spectrur width Sz exceed 1 rams In all. other cases,

including those considered below, Sy is aisitunied constant at 1 m-m, This

can be achieved by using such techniques as Kapany's9 Light Funnel or

Bowen's10 Image Slicerý,

Table 11 lists the exposure tintes required to record a density of

0. 6 on 1 03a -0 emulsion as a function of stellar magnitudes and spectrographic

resolving powers. The quantities assvincd constant are: the width of the

1 11
Table II

Stellar Magnitude EXPOSURE TIME IN SECONDS

Resolving Power Resolving Power Resolving Power

of 80, 000 of 20, 000 of 5, 000

-21 4.0 x 10-7 Z.5 x 10-8 1.6 x 10-9

-19. z2,5 x 10-6 1 .'6 x 10-7 1.0 x 10-8

-17 1.6 x 10-5 1.0 x 10-6 6.2 x 10-8

-15 1.0 x 1 0 -4 6 .2 x 10-6 4.0 x 10-7

-13 6.2 x 10-4 4.0 x 10-5 2.5 x 10-6

-11 4.0 x 10-3 2.5 x 10-4 1.6 x 10-5

- 9 2.5 x 10-2 1.6 x 10-3 1.0 x 10-4

- 7 1.6 x 10-1 1.0 x 10-2 6.2 x 10-4

- 5 1.0 6.2 x 10- 2 4.0 x 10- 3

- 3 6.2 4.0 x 10-1 2.5 x 10-2

- 1 4.0 x 101 2.5 1.6 x 10-1

1 2.5 x 102 16 1.0

3 1.6 x 10 3 10 2 6.2

5 1.0 x 10 4 6.2 x 102 4.0 x 101

7 .2 x 104 4.0 x 103 2.5 x 102

9 4.0 x 105 2.5 x 104 1.6 x 10 3

11 ?A.5 x 106 1.6 x 105 1.0 x 104
~pe ctrui11 ; , a't J 111111, the cct olltitoll 1110ii 7 , of the, 1 03a-0 e muilmion

at 200L; the dianwe te r of the Collimato e objecti%,e at ?00 inn); the angular

dispefClion of the greating (of 11), 000 lineiiL pe~r in1ch and used in the second

order) at t. 26 radiano/A; the transmision factor of the telescope -spectrograph

system KTs assumed to be 10 per cent and fair- seeing conditionL

(P 1. 0 x 1 0'5 radian), In order to calculate the flux required to produce a

photographic density of 0. 6, the measurements of Pettit and Nicholson11 at

the Mount Wilson Observatory were used. They found that 0. 244 ergs/sec

of radiation were incident over the aperture of the 100-.inch telescope from

a 1.0 magnitude star in the zenith for a mear wavelength of 5000 A. The

relationship between stellar luminosity and mnagnitude is given as follows:

where m 1 and m 2 are the stellar magnitudes and 11 and 12 are their relative

apparent luminosities.

The exposure times listed in Table i1 apply to three different

spectrogra'-'- systems attached to the 100.-inch Mount Wilson telescope; they

can be converted to the exposure times for a 25, 50 or 200.inch aperture

telescope by multiplying the exposure times by 4, 2, or 0. 5 respectively.

Similarly, for good and poor0 seeing conditions with the 100-.inch telescope,

the exposure times are respectively halved and doubled.

Table II does not include the variations in atmospheric transmission

(Kat which are functions of wavelength and zenith angle, Stebbins and

Whitford 1 2 have published some observed values of atmospheric spectral

144
transmnissoio aho t he Mot.j i vi. 11)Ic, -VI ~ obs, nierved ';iu

are of importance because te'!f inhlude not only molecular scattering effects

but also transinit. on l-ssqe, due io haze aid the s-eloctive absorption of the

atmosphe 'e 'hese results have been used to (leterrmine the variation of

atmosphe -ie t ransmnission with zenith angle and arc shown in Table IiI for

zenith angles of 0'°, ?0 and 400.

Table JI1

Wavelength 0. ZO 40°

3530A 64% 62% 56%

4220 78% 77% 73%

4880 86% 85% 82%

5700 89% 88% 86%

7190 95% 95% 94%

10300 97% 97% 97%

High speed spectroscopy of the lunar blast and infrared measurements

of the moon in the vicinity of the blast would yield information regarding:

(a) composition of lunar materials, (b) thermal properties of lunar materials,

and (c) the associated exciting phenomenon. High speed spectrographs, using

various types of image dissectors and rotating drums have been developed.

Some of these instruments have been used for high speed photography and

spcctroscopy of explosions on earth using speeds of the order of 107 to 109

frames per second. However, due to the complex image dissecting systems

used, the spatial resolution and light efficiency of these systems is, in genaral,

poor. Need for development of efficient high speed cameras in conjunction

with astronomical telescopes is therefore indicated. Furthermore, with
the recent em tpha si s on ha Ilooi cart I- I e t 1 le scope s, it would seem that more

efficient high speed photography systenis with widei spectral range in the

JV and TR will have to be developed.

A. Stellar Spectroscopy Above the Ozone Layer

The point of interest in high altitude spectroscopy is whether the

recording range can be extended from the visible into the atmospheric

attenuated ultra--violet as well as infrared regions of the spectrum. The

main problem here is to lift a telescope--spectrograph by balloon to a height

of 150, 000 ft., i.e. , above the ozone layer, to stabilize the motion of the

balloon and to direct the telescope so that the image of the detonation lies

across the entrance slit of the spectrograph. This presents a large number

of practical problems in precision tracking and stabilizing instrumentation as

well as development of large payload balloons.

Assum•ing this problem is solved, then the telescope..spectrograph

system is working under ideal conditions and the size of the primary image

is that of a diffraction-limited system. That is, the seeing condition P3, taken

as 10-5 radians in Table Ii is substantially reduced. Consider a 24-inch

telescope, the value for P3 in the diffraction-limited case is given by

where ) is the wavelength used and D is the diameter of the aperture.

Putting A• = 5000 A and D ý 24' we then have P3 = 10-6 radians. If, in

equation (8) the ratio of -- is kept constant and the same values for

/ed

the resolution, etc. , aic oscd al: far the 100..inch telescope, then the speed

} ,(
will be altered in the ratic

Hence, the 24-inch telescope, working under ideal (onditions, will be 2.4

times as fast as the 100--inch telescope at Mount W.lson working under fair

seeing conditionn.. if a I 2--inch telescope is substituted for the above 24--inch

telescope, then the speed is 0.6 times that of the 100-.inch telescope.

If a telescope 12 inches or more in diarreter could be carried to a

height of 150, 000 feet with a spectrographic s,, stem attached to it (it should

be noted that for a resolution of 80, 000, 20, COO, or 5, 000 the focal length

of the camera would be 2, 600 mm or 160 mm respectively for a 15, 000 lines/inch

grating in the second order) then the spectral range would be limited by the

reflectivity of the different components of the system. Aluminum is the usual

reflection coating used through the visible spectrum; it has a reflection

coefficient of over 85 per cent through the visible spectrum and down to

about 2000 A, but then the reflectivity fal.s nearly linearly to 10 per cent at

1000 A.

Section Three

Infrared Measurerrments for Determination of Lunar Thermal

Coneuctivity

The infrared measurements of the moon's surface temperature

being considered consist of collecting the radiant flux from a one square

mile area centered about ground zero, and obtaining a complete time vs
temperature record of thi, i0egion. 0 . he ifor mVation obtained from i such a

Me, aSUre0e' IO t Would 1(1ci able one to es 0timate the thewrial conductivity on the

basic of the rate of cooling, arid would yiel d the same type of inforination

13

previously obtained by infrared measurernents during total lunar eclipses

except that information could now be obtained at very much higher temperatures,

and with the additional advantage that more sensitive meaf3urements are

possible now due to the development of highly sensitive photoconductive

detectors such as the lead sulfide cell.

The measurements made during lunar eclipses have indicated a

rapid cooling rate showing that the conduction of heat into or out of the

interior of the moon is very slow. This very poor thermal conductivity

could be attributed to the layer of highly porous, dust..like material thought

to be blanketing the moon's surface. Infrared measurements made during a

lunar detonation might yield radically different results, since if a surface

burst is employed, a very large amount of thermal energy would be

deposited in the lunar material beneath this porous covering, and the thermal

conductivity of this material may be considerably greater. Thus, one might

anticipate a. slower rate of cooling to be measured under these conditions

than has previously been measured during the lunar eclipse measurements.

The sensitivity of measurements of temperature of regions of the

moon in the vicinity of the blast is a function of the absolute temperature of

the area being compared. For instance, if the area closest to ground zero

i• at a temperature of 15100C and the area flurther from the burst is at a
temperature of 1500"C, the ten dcte g' rciffe f ,in ce in temperature would

produce a difference in thle total radiation collected by a one square meter

telescope mirror of 4 x 10' 8 watts and in the lead sulfide region (1.0 - 2. 8 •)

to a difference of 1. 3 x 10(-8 watts. Since the noise equivalent power of

present day lead sulfide detectors )s approximately 10"11 watts, this signal

can be easily detected by such a phoLoconductive detector. We can see from

the very low noise characteristics of these detectors that temperature

differences of considerably less thon 10°C can be detected at an absolute

temperature of 1500°C. At an absolute temperature of 200°C, the same

10°C difference in temperature would produce a difference in the radiation

collected by the one square meter mirror of 0.73 x 10-11 watts in the lead

sulfide region. This quantity of flux is approximately equal to the noise

equivalent power of the cell, however, and would produce a signal-to-noise

ratio of one. In order to detect this 10°C difference at 200°C, one could

employ a larger telescope mirror so that the signal-to-noise ratio would be

increased .. ntil the signal could be resolved.

In the above calculations the transmission of the earth's atmosphere

was chosen as 30 per cent, and the moon was considered as performing as

a perfect blackbody with an emissivity of unity. The total flux collected

at the earth's surface from a unit area of the moon's s-trlace ic t-n given

by the expression
where a :S emi s351ity of the moon

()- =Stefan- Bolt a Hu n co 0 sta lt

t te temperaturc in °K

r, moon-earth distance

a :transmnission of the earth'si atmosphere

Ac area of the telescope mirror

The table shown below illustrates the flux collected by a one square

meter mirror from one square mile of the moon's surface which is

maintained at the six different temperatures listed. The total radiation as

well as the radiation in the lead sulfide (1. 0 - 2. Bl) and lead selenide

(1.0 - 7. 0i) regions is shown.

T'C Total (watts) PbS( watts) PbSe(watts)

200 4.66 x 10"9 Z.35 x 10o'1 1. 59 x 10-9

500 3. 38 x 10-8 3.04 x 10-9 Z 30 x 10-8

000 2.47 x 10-7 9."5 x 10-8 Z 19 x 10-7

500 9.26 x 10-7 5.46 x 10-7 8.43 x 10-7

P000 Z.47 x 10-6 1.61 x 1,0-6 Z 10 x 10-.6

•000 3. 60 x 10-5 2. 05 x 10-5 2. 34 x 10-5

The noise eq.iivalent power for each of the three types of detectors

listed above can be tak n as 10'7 w;otts ior the total radiation detector

(1,' ion. et' r), !0-,I wattsa for the lei- ,( o fide cell ýtnd 10- 9 watts for the lead

selenide cell. It can be seen, therefo1re, that t.ie lead sulfide cell gives the

hi ,he st signal iiOc, ro-.c tins o t all inl otu-es. and it ?.00'GC tLenipucatlur..

deternninatincii ;:afi o•ily inn nonde ''vith wte!h ibis nqinne the tutal radiation
detector and lead selenide cell yield siggnal-to.-noise ratios of less than two.

Thus, a lead sulfide detector is the best suited for this type of measurement.

The size of the detector to be employed will be dependent upon the intensity

distribution in the diffraction pattern in the image plane of the telescope and

will, therefore, be governed by the atmospheric "seeing" conditions and to a

lesser extent the diameter of the objective mirror of the telescope.
u E, FERE NCNES

I Blackwell, "Contrast 'Threshold of the Hurnan Eye, " JOSA, 36, 264 (1946).

2. Knoll, Tousey, HIulbert, "Visual Thresholds of Steady Point Sources of

Light in Fields of Brightness from Dark to Daylight, " JOSA, 36, 480 (1946).

3. Tousey and Hulbert, "The Visibility of Stars in Daylight Sky, '' JOSA, 38,

800' (1948).

4. Tousey, "Optical Problems of the Satellite," JOSA, 47, 261 (1957).

5. Van Allen, Ed. , Scientific Uses of Earth Satellites, University of Michigan

Press, 39 (1956).

6. Lamar, Hecht, Schlaer, and Hendley, "Size, S}- )e and Contrast in Detection

of Targets by Daylight Vision, " Part I, JOSA 37, 531 (1947); Part II, JOSA,

38, 741 (1948).

7. Dunham, Vistas in Astronomy, 2, 1Z23, Pergamon Press, New York

8. Eastman Kodak Co. , "Kodak Photographic Plates for Scientific and

Technical Use,'" (1953).

9. Kapany, Proc. Symposium on A3'-onormical Optics and Related Subjects,

Manchester University, 288 (1955).

10. Lowe•n, Applied Phys. J. , 89, 1 1 (1938).

11. Pe.ttit and Nicholson, Applied 1-1.y ..J. , 68, 27%1 (1928).

I2. Stebbins .rnd Whitlord, Ibid 98, ý. ( 19-11).

13 . Ku•:,ip{ Fr, I'h A •.uher( f t'w Etrtl; ;t.d tPlane.ts, Uriversity of Chicai.-

!'."reo!ss (I 't) i .
Chapter IV

SEISMIC OBSERVATIONS ON THE MOON
Chapte): IV

SE.ISMI(; OJ3SERVA'.IONS ON THE; MOON

Seismic observations on the moon are of great potential interest from

the viewpoint of fundamental theories of the development of the solar system

and Of tile m....itself. Deter•m.ination of th. phycical ..tru tur e of both the

outer layers and core of the moon would go far in permitting choice

between various suggestions as to the origin and early history of our satellite.

It is not certain how much seismic energy will be coupled into the

moon by an explosion near its surface, hence one may develop an argument

that a large explosion would help ensure su,:cess of a first seismic experiment.

On the other hand, if one wished to proceed at a more leisurely pace,

seismographs could be emplaced upon the moon and the nature of possible

interferences determined before selection of the explosive device. Such a

course would appear to be the obvious one to pursue from a purely scientific

viewpoint.

In the event high sensitivity seismic detectors could be emplaced on

the moon and the noise levels were sufficiently low, one might gain valuable

information either froom the impact o- rnet-orites or of iocketc undergoing

I16I .1d tIluifig Oil LI[J i' M! U 1i i fi 0 . au... .. a1 .U... I\. o0u.* -f k S C;ý

We shall outline he'e some general aspects of seismic observations

and pos sible instrumnta. cn, f.gura.iorns and also attc,,!pt a rough c-lculation

on the (1ktectability of oet 'r wcis of ,,'ari 1o' r pi-lif -.
Section One

The Nature of Seismic Observations

From the point of view of seismology, observational data indicates

that we may consider the earth and presumably the moon as large elastic

spheres that are essentially homogeneous and isotropic insofar as local

variations hn elastic properties are concerned. The mechanical energy

involved in auy local deformation of such a sphere will be propagated in part

in the form of elastic waves moving out from the focus of the deformation

to every part of the sphere. Considerations based on an infinitesimal strain

theory of elasticity lead to the conclusion that there are two possible types

of body waves in such media. One, which is transmitted with the speed

a•. 2 , is a compressional body wave designated as the P wave

in seismology. The second, which travels with a speed the S

wave of Leismology, is a transverse wave. In these equations, A and IL

are the Lame stress constants, ýi is a measure of the rigidity of the material,

and A is related to the incompressibility of the media, k, through the

equatio /- = /A j:-,A.

When these waves reach the surface they cause that surface to undergo

a complex periodic motion. A properly designed seismometer is able to

record one or more of the translational components of that motion. The two

types of body waves move with distinct velocities, and, therefore, arrive at

a djcta.it station at different times. Their arrival is usually recorded as

distiCt mo-icns in ti-n,, , 0f the rci-mic u ;ass relati,.,: to the surface.
As a prelinniiary, we alia1 first di scu.•ýs various aspects of terrestrial

sei smology and then proceed to lhe main 1

question o of scismic observations on

the moon. Within the earth's interior, there are regions wherein decided

changes in elastic properties occur. Either type of body wave incident upon

such regions of discontinuity will, in general, give rise to both reflected waves

and refracted w~tves of both canmpr-eiona! and transver'se character. The

complex system of waves arising from the reflections and refractions at the

several regions of discontinuity ultimately reach the surface to be recorded,

in turn, by the ieismometer. In addition to the body waves, the typical

seismograph r,.cords the arrival of various types of surface waves that have

travelled through the outermost layers of the crust to the station. The

complicated record of the arrival of all of these varied wave pulses constitutes

the basic observational data of seismology. Fig. I is a representation of the

ray paths for a few of the possible types of wave pulses that might reach a

station on the earth's surface from a disturbance whose focus is within the

mantle. The major zones within the earth, based on se;smic data of the

variation of velocity with depth, are indicated. The details of this pattern

will be discussed in Section Two. For our purposes here we have indicated

only the mantle which extends to a depth of 2900 km and beneath this layer

core of the earth. Withii-n the core a further subdiv'i qin occu1!rs at a depth of

about 5100 krn. This central portion of the earth is called the inner core.

The notation used to identify the various types of rays is the following: For

compressional waves within the mantle, P is used. Shear waves within the

mantle are designated by S. For coriprcssional waves within the core, we

I 1 (
p° / 0ocus OU

~ PS

7'PS

//

/ /

//

INER• "P

CORE

OUTER COR!

//MANTIE/ pK

P - rRAYS ,", O COMPREESSIONAL WA8VES

S-RAYS CWA:•VES

FIG. I - PATHS OF- S'lISivil, V-M S,: WITVi--;i',] 'lll, EARTHI.

i 57
ut-je K. No ilihar 1Wavfe have beeni oh , eVQd wilhin the core rCo that no symbol

need be specified for i;ucui a ray. ' o indicate that a ireflection has occurred

at the core a c mall letter c is placed between the capital letter s designating

the incident ray and the reflected ray in this manner. PeP.

The rshort rays moving upward to the sur ace from the focus are

designated by small letter s or p, depending up)n whether the wave is a

shear wave or compressional wave.

In the seismographs taken at stations some distance from the focal

point of a disturbance within the earth, it is possible to determine the time

of arrival of many of the waves described Above. A knowledge of the locus

of the focal point of the disturbance, the time of occurrence of the

disturbance, and the time of arrival of a given wave pulse at various stations

enables one to construct a travel timetable giving the time required-for a

given pulse to travel the distance fromn,the focus to the point of observation.

The most comprehensive data of this type for the earth have been compiled

by Guttenberg and Richter and by Jeffreys and Bullen. Travel time curves

for several of the types of wave paths occurring within the earth are

illustrated in Fig. 2.

These tables are the basic tools for the interpretation of seismic

data for the earth. With their use it has been possible to obtain an accurate

knowledge of the variation of velocity of both shear and compressional body

waves with depth within the earth. In terins of their variation, together with

some further assumptions and known properties, of the earth, it has been

I I-,H
40

t ~PKKPSKKS

10- PCP- _

0iG -30 60 90 120 liD'( 180

LPIC[TRALDIS'ANCE

FIG 2--TRAVEL- TIME CURVES FOR SEISMIC W/WES IN THE EARTH.
poosible to determine theu vari ation with depth of s uch quantities as density,

1

Dresusnre, and the elarmti( (,osiant, of thI" eath's interioro

, rC( iio,, Two

The Stru c tre of the .a r th ' Interior

If we consider the variation of velocity of Heismi.c waves with depth,

we can distinguish three major zones within the earth's interior. The first

zone is the crustal layer varying in depth between 30 and 40 km over the large

continental land masses and between 5 - 6 km under the large ocean areas.

This region is heterogeneovs in those properties which relate to the movement

of seismic waves, and velocities of both P and S waves within it are very

variable. From the lower sorface of the crust, the Mohorovicic discontinuity,

to a depth of approximately 2900 km lies the mantle. This region is

characterized by steadily increasing velocity of seismic waves with depth and

is believed to consist of dunite, a hard, dense rock made up largely of the

mineral olivine, a silicate of magnesimrn and iron (Mg, 'e) 2 SO 4 .'

At the surface olivine has a density of about 3. 3 gin/cril 3 . Since the

density of the earth oo a whole is of the orderj of !i. 52 gm! cm 3 this implies

that the interior of the earth beneath the nmantle must have a very high

density. Seismic evidence indicates for the core ef the earth a density of the

order of 10 to 12 gm/cm 3, a very low rigidity, ai(' a marked decrease in the

velocity of compre,,sional waves. The most reasonable assumptions appear

to be that the core coni;tAs largly of iron or of an. iron nickel mass in the

molten state, and inder vcry high pmess rca,
A myexo ( 'l.reid ./'I\d, (if Ic vcLocity depth curves reveals a still

finev s.,bdi, i. sion o IO.e Ui (- jor 0'.zoncfi mentioned above into regions

wherci marked c has ge u either in velocity oi- velocity gradient occur. These

subdivisions ai'e picesented in '.IIable I taken fromn I3ullen whose analysis is

based on the velocity depth curves of Jeffreys .in ,iddition, we have included

Pig. 3 which gives the velocity depth curves for t

1\e earth as developed by

Bullen. It will be observed that the curve for S waves does not continue

beyond the lower surface of the mantle at a depih of 2900 kmn. The absence

of data revealing the passage of a shear wave through the core of the earth

is one of the major facts of seismology and attests to the molten state or at

least very low rigidity of the earth's core.

This discontinuity is further rnarkei by the drastic drop in the velocity

of P waves at this same level. The minor variation in the velocity of P waves

at a depth 5121 kmns attests to the existence of an inner core within the core.

If we know the variation of the velocity of shear waves and compressional

\/-ves and, therefore, the variation of the Lame constants A and p, with depth,

then the assumption that the stress within, the earth's interior is essendhily

equivalent to a hydrostattic pressure leads to the following differential

equation relating drns.ty red the distance r from the center of the earth.

"y gravtation ,,

in 2 mars of eari: 'A. 1 re 4, r

P den Ij,, a. O -i: .

6. ,/
T"ableI

I).MINS.ONS AND I)IKSGR 0 TIOl\IS OF tN'I'EA.NA1, .1,AYtJRS 01'

TIJIE EARTHDepth to Bundaies R in; KI'i FetrofRgn

lc(rwit A 33 Gonditions fairly heterogeneou

B 413 Probably homogeneous

Mantle C 984 Transition region

D Probably homogeneous

? ,898 - -----

E 4982 Homogeneous fluid

Core F 5121 Transition layer

G 6371 Inner core
MANT11 TF G ORE INNER CORE

72

4100 cD

DF0- (KIA

FI )1X O T11 15 OF 11F V W .. ES '-M ,z,-l,-i ;\
If we add the boundary condit.,,f: implied in Ithi knjown mass of the

earth, 5.977 x 1O ; y10 s, and tinc l•hW ii•, l iniieiit of inertiia, 8. 104 x 14 4 gWi cm111

then by certain reasonilble assumplioi- toes to the nitkjre of the material of the

core and the lower layers within Ih-. nnh•. Ithe integration of this equation

leads to a detern•in ation of t he vs : sIion of d.r-a ity with depth within the earth.

since the stress in the earth's interior is essentially equivalent to a hydrostatic

pressure

/

and a knowledge of the density variation with depth allows the evaluation of

the variation of pressure with depth. Finally, since the velocities of the

compressional wave, P, and the slhear wave, S, are known in terms of the

density and the values of A and [i, then the variation of A and p. with depth

can be established. In terms of these s'ich elastic properties as the bulk

modulus of the earth's interior is obtainablo.

Table II is a compilation of the denLsity, gravity, and pressure distribution

in the earth due to Bullen,

b,. Ž( ion TB r r.

Why A Seinsmologica] :ii vestigation of the Moon?

One of the fundamental probhems of the seismology of the moon that

needs to bhe investigated is the level of ba ckgroutn.d noise or seismic activity.

This investigation would in volVe nol]y the I:>', 'lie t.,t of a single seis monieter

at a single location upon the. non'ý , •rfa , Io the earth there is a
DENSITY, GRAVITY AND PRESSIJR.E DISTR IBUTION WITHIN TIlE EARTH

Depth DensiIty Gravity Pressure x 101'2

km gin/cm 3 c Y/se c" dynesl/cmr

33 3.32 985 0. 009

100 3.38 989 0.031

200 3.47 99Z 0. 065

300 3, 55 995 0. 100

400 3. 63 997 0. 136

•'3 3,6.1998 0. 141

500 3.89 1000 0.173

600 4. 13 1001 0.213

700 4.33 1000 0.256

800 4.49 999 0.300

900 4.60 997 0.346

1000 4.68 995 0.392

1200 4.80 991 0.49

1400 4.91 988 0.58

1600 5.03 986 0.68

1800 5. 13 985 0. 78

2000 5.24 986 0.88

2200 5.34 990 0.99

2400 5.44 998 1 .09

2600 5.54 1009 1 .20

2800 5.63 1026 1 .32

2898 5.68 1037 1 .37

2898 0.43 1037 1 37

3000 9.57 1019 1 .47

3200 9.85 979 1 .67

3400 10.11 93 1 .85

3600 10.35 892 2.04

3800 10.56 848 2. 22

4000 10,76 803 2.40

4200 10.94 758 2.57

4400 11.11 716 2.73

4600 11.27 677 2.88

4800 11.41 646 3.03

4982 11.54 626 3.17

5121 14. 2 585 3. 27

5400 460 3.41

5700 320 3. 53

6000 177 3.60

6371 17.2 0 3.64
considerable background of seismic noise. This is due to such factors as

the activity associated with civilization, the movement of trees with the wind,

the movement of atmospheric storms over the surface, and possibly the

pounding of the surf along the shores of the oceans. Upon the moon all such

activity will be absent. Dr. Jack Oliver, a seismologist of the Lamont

GCoplhys;ical LaY atr of Colmbi UniVerit, NeY 0vW IU YIk %it,LL I aC

expressed the opinion to us that, as a consequence, the moon would be

expected to be seismically very quiet. The only probable sources of background

seismic noise within the moon would be the natural vibrations induced in it

as an elastic solid in response to uneven gravitational pulls of the earth and

possibly other planets within the solar system, together with the "creaking

noise" associated with the adjuSmMent of large masses of rock to the resulting

uneven stresses. The periods associated with the natural frequencies of an

elastic sphere of the size of the moon are much larger than the periods of

the usual seismic waves of interest in seismology or those associated with

explosions. Special design of instrumentation is required to achieve the

ability to record eLh waves. A profugran for the de velopment of such

instrumentation lo neipastre the co r r ie,-•ding periods for the earth are even

no.jv being catrried r ut at Lamont Geophy, ical Laboratories. The requic.ed

Ic - p•,r t t 5,.si., rt:t',ml b h yve rIUt yut 1, C11 d vibedd. ();I thie ea.ritil tLh

-;-nic noise 1w<( :,,round, usually caller.] mic rose isims, is of the ampliti a

1:N' of 0. 1 to 10. 0 microns. That back, round noise o.- the moon attf.-i .-,V',le

to tle constant rc-c i costnment of large ror.Ik strata to the uneven stressca
to the gravitational pull of the earth would then be expected to be no larger

in amplitude and is probably much lower. It will be of importance to monitor

this background level. for a period of time to determine its absolute value,

the nature of its variation with time, and the characteristics it exhibits, The

accomplishment of this phase of the investigation.,assuming that a single

functioning i.-nqtrliment package can be landed on the moon, requires the

minimum of equipment that would be involved in any seismic investigation.

Upon the basis of the current hypothesis of the structure of the

moon's interior, one would anticipate no large amount of moonquake activity.

This hypothesis assumes the moon has no liquid core and that it

consists of a layer of mantle-type rock overlying a small solid core of iron

or nickel-iron. Upon the earth the great majority of earthquakes arise

within the crustal layer as the result of volcanic activity or the adjustment

of excessive strains along fault lines. Only a small proportion have been

recorded as originating in the underlying mantle rock and these only in the

shallowest layer.

In the absence of volcanic activity and a crustal layer for the moon,

we must anticipate that a moonquake can be only a very rare occurrence.

Yet this is all hypothesis and the recording of none or little moonquake

activity is an iruporta nt experimental fact with which to judge any theory of

the structure and the formation of the moon. Upon the earth although a

major earthqcuake is fortunately rare, yet an earthquake of lcw intensity is

very common. This is a1gainst a rel l; i vely high br, akground activity. Thus,
if for any reason there should be moonqu;)lKes, then since the background noise

will be low, one would expect a conciiderable amoint of interpretable data

fro a 1 single seismxnoaete .

What has been said so far envisages the placement of a ringle

seisrnometer upon the moon and does not involve even the explosion of a

single bomb whether of a nuclear or chemical tvype

If we enlarge the scope of planned instrumentation to include the

possibility of placing three widely-spaced instrn:.ment packages, we can

expect to gain additional information. The presence of three recording

seismometers increases the possibility of obtaining usable records, increases

the possibility of verification and cross-checking of instruments and, in addition,

allows for the construction of elementary travel timetables.

It is to be remembered that the travel timetables for the earth are

the result of a long and continuous statistical analysis of a large body of

seismic data taken by a wide coverage of instruments.

Our moon tables can be only a crude beginning, yet can off(:1r a wealth

of information relative to its interior and surface layers. Assurninr-,; come

seismic activity whether due to moonquakes, or the collision of meteorites

with the surface, or for whatever causes, we could immnediately obtain some

general and far reacbing conrbliiinns fnv })p ntr ctflive of the moon, its

surface layers, and its history. The velocity of body waves and, therefore,

the elasticity of the mediums, at least within its mantle, would be an

immediate result. The existence or non--existence o., a layered structu).

I ýý f,
within the immediate ubi) su'fiac re afa of the moon could be etstablished. If

we are fortunate the existence of a core and the absence of a liquid core can

be confirmed. Some ray paths are shown in P."ig. 4.

If we have some approximation to the variation with depth, we can

obtain an idea as to density variation and pressure variation with depth. In

short, the path laid out by the analysis of the structure of the earth's interior

from seismic data becomes at least partially available for the moon. This

has hypothecated observable seismic activity upon the moon.

If we further hypothecate the explosion of a nuclear or even chemical

bomb, we then have the possibility of certain determination of at least the

immediate sub-surface structure of the moon. The existence of any

pronounced sub-surface discontinuities will certainly be revealed. The

elasticity, density, and pressures within these layers will have been determined.

The certain occurrence of surface waves will add to the information obtainable.

Section Four

The Nature of the Requirement for Instrumentation

As ordinarily constructed, a seismometer would ideally record

some component of the relative motion of the earth'.q surface with respect

to its quiescent state. In seismology the components normally measured are

oiie or more of the three translational components of that relative mc>2:'Cn.

The rotational components are so sm~ll at all obsecrvational p-sit ts ex'ccpt

within the irnm edio,. , vicinity of the focel1 point of the di sturLr• .:-.' that thcy

re not recorded. 'Yo mease thJ.i; c$)nmonent of Oii.ce:c
Zý; '331LAR W~AvL: IN MANTH'

K GOMPtRESS ION WAVE' IN C~

S' SHEAR WAVE' IN GORE

REFLEICTION OF COREr SURFACE

7' ININER

PS ~L - E__

O 500 1000 1500

P~c~P

PlCi~V :
soree point of a matcriai body ) ht) F ll- iti fixcd in s.'ilce as thel( e rtih'

surface undergoes its motion unda-r the inflieric(- of the passing seismic wave,

One way of providing such a point is to suspend or soppori a mass on a spring

from a rigid frame that moves with the earth. The softer the suspension and

consequently the longer the period of such a mass, the more nearly does its

motion relative to the frame and thus the earth represent the quantity we

wish to measure. An alternative is to use a pendulum, in the usual case for

seismological observations, a horizontal one. For a pendulum, we also

require that some point relative to the pendulum mass remains fixed in

space if the point of suspension moves with the rapid motion of the earth.

If the period of the earth's motion, normally less than 30 seconds, is much

less than the free period of the pendulum, the center of oscillation of the

pendulum system is such a point. For a physical pendulum this is that point

at which all mass may be conceived to be concentrated so that a simple

pendulum whose length is the distance from this point to the point of

suspension and with the same mass would have the same period. For

seismic instruments designed as permanent installations at observatories

on the earth, these principles have resulted in typically large installations

with relatively large masses and long beams. The instruments are firmly

anchored to large concrete pillars resting on bedrock if possible. Major

problems have involved those associated with obtaining a recording without

undue reaction by the recording mechanism upon the instrument in the form

of resistance or the coupling of the mate~rial oscil]ations of the recorder.
The chief' nwthods of :Ho.-j en I 1I. I fr d c... -I' Ioped ha\'e ihivolved either

rnechanical linka ge :3 to pen or pipe r, op caI I leve r i V rangemrents , or c(oupling

to electrical systerns through c ois ,- novii p in a m a g•etic field. Recent

developments in the fied have been- :oolI ected with such problemrs as obtaining

records from seisminoirieters placed lin remote inaccessible locations. At

Columbia University, for examnple, they have been interested in obtaining

records from seisniometers dropped to the ocean bottom from the surface.

The Air Force as part of the IGY program has been interested in obtaining

records from seismometers parachuted to the Greenland ice cap from the

air. These programs have met some, if not all, of the problems likely to

confront the development of instrumentation for the present program. The

problem of size and weight of the instrument is simply one of design and the

people at Columbia feel that a maximum of 20 pounds for the total instrumentation is not unrealistic. Whether thi; can be bettered will depend upon the

interplay of size and weight of such components ai coils, electronics, and

so forth.

The problem of coupling of inslr,.,mentation to the ground does not

appear too severe. Asqskiing no vory .lcick laver of dust or debris above the

basic rock of the surface l;iyecs we itecd not even contemplate the necessity

of anchoring the instrurnt of to tbl [ro'und. If it but rests solidly on the ground,

adequate coupling is assurd,,. 'lThi:; is, in particular, true for the case of

the long surface waves which would be an important component of the seismic

activity created by the deiiw,;o!ioor .If I ',r,1 i > hni,. The largest difference
J,eveliiii (it of fe ii).ýttru•lwii l ifter: ,di(t (J. i(H im)l expectOed to be it major

problem. The reqio reinenlt for c((ac and (Jhti ate Ieveling is connected with

the recording of Ihe horcizontal colltyoret of lonig pecio earthquake waves.

tor ei smoineters l:;ed to meat0 orce the vertic(al co()por0eo of. motion and for

the high frequency waves associated with explosive detonations near the

recorder the require nents as to leveling are much le[s severe.

A sketch incorporating those features that would be desirable in a

seismometer for exploration of the moon is included as Fig. 5, A mass is

coupled to the frame of the seismorneter through the corrugated diaphragm

providing a weak spring constant. This is to be so selected as to provide a

natural period of the mass very large in comparison to the range of periods

of seismic motion of the moon to be studied. The motion of the seismic

mass relative to the frame and also the mnoon is transduced by the motion of

the attached coils in a magnetic field. To protect the seismometer during

the high accelerations encounltered during its flight to the moon and at impact,

blocks have been provided between the seismic mass and the frame. These

blocks are chosen ",0o a1s to p-rOvidli a high p;1)riog (onosant and the resulting

combination of seismic mass and blocks constitute an accelerometer which

can provide a record of the character of the inopact of the instrument with

the surface of the moon. After impact the blocks are removed by a suitable

mechanism and the instr-ument capsule assumes its role as a seismometer.

j(/.
---SCREW THREAD

'---SCREW MOUNT

ACCELEROMETER

SIMCSPRING

MASS SIMCSRN

IACCELEROMETER

II MAGNET

Armour Research 1Fouridulonl

SMODEL OF0 AXN A(Y RoiT•H :S0JT
Al ~lt i'~ oi tih (I; jifl-- ,, ho'' ib V. pomni. of~ "I ucle'a. blast on

the moon to which the re •nibin, ,,ci .flic s ignal can be detected can be made

as follows. 'th-u have been nevcral undercgrouind nrtclear blasts that were

recorded seismically on the earth. These include detonations of Blanca,

23 kilotons; L.ogan, 5I kilotons; Rainier, 1. 7 kilotors; and Tomalpais, 0. 1 kilotons.

The amplitude of the neinrnic waven remulting from these shots was

approximately proportional to thm first power of the kiloton equivalent yield

of the bomb, The coupling of the energy of the detonqtion to the earth was

such that the resulting seismic signal for the '.rainier shot was equivalent to

that observed from an earthquake with a scale value of 4. 6 on the GutenbergRichter scale. 2 This Ficale is given by the emipirical formula

"10"

is approximately the energy involved in the smallest detectable earthquake

on earth. E is the estimated seismic energy in ergs involved in a given

disturbance. On this scale the Logan shot would correspond to a scale value

of 4.9 and the B3lanca shot to a scale value of 5, 2, The efficiency of energy

transfer into oeismic energy will not be sjo large for a bomb exploded above

ground as for one which has been buried. fn the field of seismic exploration

for oil bearing strata, for example, it han ).een noted that the transfer of

energy can be increased a hundred told by burying the charge in a water

logged strata over that for a surface exielonion, In a high energy nuclear

explosion above the ,;urface of thoe moon, it has been estimated that the

effective agency of e ergy tn fer to the rsurface of the moon will be x-.rays
produced by the explosion. The enetugy of Ihe box0mb converted into this form

is of the order of one- half its total energy of which less than one--half again

will be directed toward the nurface of the moon. 'The exact mechanism by

which seismic energy 1.j generated by an atornic explosion is not known. But

of the total energy reaching the surface a considerable fraction must be

expanded in heating and vaporization of the surface layers of rock. A crude

estimate would be that energy transfer into seismic energy is 0. 1 as large

for an above surface detonation as for the detonation of the same bomb when

buried underground. However, we have the additional factor that the moon

is expected to be seismically quieter than the earth. If we assume that

instrumentation is noise limited then we have a gain in the signal-to-noise

ratio due to this factor. A decrease in the noise level of the moon over that

of the earth of the order of 100 to 1 seems reasonable but we shall assume

a gain of only 10 to 1. The net result should then be that a nuclear bomb

detonated above the surface of the moon should be the equivalent as a source

of detectable seismic activity on the moon as the same bomb exploded

underground upon the eax:i.h. Uudcl i hese as sumiptions a kiloton bomb

exploded just above the surfiace of the mnoor woulh beh the equivalent (insofar

as seismic detonation on the moon) of an earthquake upon the earth of magnitude

Similarly, a Ynegaton bomb so detonated would be the equivalent of an

earthquake of magnitude
The kiloton bomb would be detectable at a distance of 300 - 400 miles, while

the megaton bomb would be detectable anywhere on the moon. Table III is

presented as a resume of the Gutenberg-.Richter scale of earthquake Khiensity

and the predicted equivalent seismic intensity for nuclear explosions above

the surface of the moon.

Table III

DETECTABILITY OF MOON TREMORS

Earthquake TNT Equivalent Seismographic Lunar Radius

Category (kilotons) Equivalent of of Detection

Nuclear Weapon

Great >106

Major 10 4 106

2 4 Destructive 102 10 1 MT Anywhere

Damaging 1 102

Minor Strong 102- 1 1 kT 400 Miles

Generally Felt,

Small 1 0-4 1.0
1. Bulleni, Introduction to the Theor~y ofSeisrnýjo~o~y. (Cambridge (1953).

2. Rainier, The Underground Nuclear Detonation of Sept. 19, 1 957, Univ. of

California Raiation Laboratory, Livermore, California.

I M8
Chapter V

THE HIGH ENERGY RADIATION ENVIRONMENT OF THE MOON
J,,L I(lilif iN ItO [UAI)IATION UN NVIRON (Ni UNT Of:" THE MOON

The lamding of one ot iioi-e instriurnwnt packages on the moon will

offer, in addition to other possibilities envisaged in other parts of this

program, the chaiienge of obtaimng inforrmation about radiation in space and

on the moon.

At present, the high energy cosmic radiation, say above 100 Mev,

is fairly well understood through measurements from the ground and in the

upper atmosphere. However, as a result of the shielding and particle trapping

due to the earth's magnetic field, we know little about the intensity and

composition of the low energy radiation in outer space, and no consistent

correlation can be drawn between solar phenomena and the variation in

intensity and the spectral distribution of cosmic radiation. Because of the

moon's absence of atmosphere and its possibly low magnetic field, instruments

on the moon will be in an excellent position for the gathering of reliable

information on low energy cosmic radiation.

Measurement of the intensily of co:rnic radiation at different points

of the moon's surface could provide information on which to base an estimate

of the magnitude of a possible magnetic field of the moon.

Measurement of the radioactivity of the moon's crust may give useful
information about Ohw past history of the n'oc',[ This data together with a

knowledge of the cheinica I composition of the crust could contribute to a

solution of the controversial problems of the age, origin, and process of

accretion of the moon.

The schedule and the technical facilities available will suggest what

e Ykpha:i~cOuld and _huld b- placed upon the whole problem of radiation.

There is always the possibility that some of the problems involved may be

solved in the near future through measurements performed by instruments

carried by outer-space vehicles. Therefore, in view of the survey nature

of this project, this chapter is strictly limited to a feasibility study of certain

measurements involving radiation that may contribute to a better knowledge

of the earth's natural satellite.

Section One

Cosmic Ray Latitude Effect and Moon's Magnetic Field

The magnetic field of the earth is of a magnitude not comparable with

the fields used in the laboratory for the deflection or the focusing of fast

charged particles. It extends, however, to an enormous distance and its

effect on the trajectories of the primary cosmic radiation is conspicuous and

determines an energy selection of the particles that enter the atmosphere at

different latitudes.

Tue solution of the equation of motion of a charged particle in the field

of a magnetic dipole extending to ineinity present.; great analytic difficu.•it

A simple approximate solution is; given by the th,'ory of the Stoermer cone.

1181
This theory shows that for any definite geomagnetic latitude there exists a

minimum critical energy that a particle must possesqs in order to reach the

earth. At the same latitude and for an energy greater than the critical

energy, particles can reach the ground only from a region of the sky which is

contained in a cone having its apex at the point of impact and its axis perpcndicular UC' pj.±at e tuh uugli thdltL puliuL. iarticieB not admitted

are reflected back into space and eventually trapped by the magnetic field

around the earth.

At the geomagnetic equator the critical energy for protons is 9. 3 Bev.

Neglecting the interaction of the primary cosmic radiation with the atmosphere,

protons of this energy can hit the ground only at a grazing angle from the

West horizon. Protons of energy greater than 9. 3 Bev, up to 14 Bev, which

is the magnetic cut-off for vertical incidence, are allowed only from the

Western sky. The minimum energy for the grazing incidence from the East

horizon is about 58. 5 Bev. Since this is the least avorable direction, protons

of energy greater than 58. 5 Bev are acdmitted from all points of the sky.

At higher latitudes the situation is quite similar but the critical

energies are lower in value. Thus, the intensity of the cosmic radiation varies

with the geomagnetic latitude and increases as it moves from the equator to

the polue. A bimilar iatiiude effect is to be expected on the moonis surface

if the rimoon has any appreciable magnetic field.

More than one instrument package will probably be landed on the

moon in ordor to take care of other sun;lgested -neas urements, Detectors for

) 8;,
the monitoring of natural1 or ,n-r .induced (I adiooactivity may be included in

the packages. These detectors could be designed and switched for intervals

of their service in order to measure the cosmic ray intensities. In view of

this eventuality, it would be worthwhile to investigate the feasibility of

making an estimate of the magnetic field of the moon by using the cosmic

radiation intensity as a probe.

Since the orientation of the hypothetical magnetic dipole is unknown,

it would be necessary to use at least two detectors landed at different latitudes

on the moon. We assume that the instrument packages will be scattered on

the moon either by chance or by design so that results will be obtained for

different latitudes. The two latitudes of 20' and 60' have been chosen for a

comparison of two expected intensities and. for an evaluation of the sensitivity

of this method.

For the magnitude cf the magnetic field of the moon, we may assume

as an hypothesis, a value determined by a dipole of a moment smaller than

that of the earth by a factor of 80 which is the ratio of the two masses of

the earth and its satellite.

Although the more correct Vallarta-Lcmaitre theory of the cosmic

ray trajectories will be required for a precise treatment of this problem,

th: Stoermer cone theory is adequate for a feasibility study.

The sirnple theory of Stoermer gives for the minimum kinetic energy

2 of a particle of reat-mass moc I iniidcnt on a spherical body of radius a

and magnetic mnonient M the e:p::-ession:
as a function of a variable

This parameter depends on A, the magnetic latitude, and on 0, the angle of

incidence of the particle with the meridian plane at the point of impact. It

can be shown that an estimate of the cosmic ray intensity at each latitude can

be obtained by using, as an average energy cut- off, the cut-off for the vertical

incidence. Values of the parameter K and the corresponding energy cut-offs

are shown in Table I.

Table I

Latitude K E(Bev)

200 0.441 2.05

600 0. 125 0.023

It is reasonable to assume that the instruments will be enclosed

in a convenient casing determining an in.itruxienital cut-off on the low side of

the cosmic ray energy spectrum. '11his is not, however, an inconvenience

since the measurements will then be independent of the contribution of the

low energy particles whose intensity, as has already been pointed out, is not

yet well known and is affected by temporal variations induced by solar activities.

Table I shows that a[ a 600 latitude a convenicnt instrumental

cut-eff of the orc -r of 300 L,,v for priotons will be the only limitation on the

18/j1
"ol K' (6) (nw

PBy ungthe Cal~cslae ((ft I tff.offfi, the expectedI lhI~tetlsjtieI will he:

"I'the contribution of o- partile ls and heavy ions3 will not change.

ni gni fica italy the pj) n Lt to th Ow pii t Ino hLe so part ic les reproesent only

about 10 prcentl of the. total liulnlbelv of priwoaie jo and he cats e of the ir

momenta diet. thution they will show a laituLide effect quite similar to that

of the protons.

As cot lu~sion, a 1 stitutlt efit,

should be obta ined cI'ihis -i ncay indin ohi i)It ;t is po. s ible to n-tea sure a

maginetro field ev; '';;Iat her LlJK..yo f d.hWe ve--t, [lic sentsitivity

cof thle Mnethod an.rd the 1rc,~hnln-!it~y 1)1 ft'e estults,; dinilp rapidfly with the intens~ity

of tile ins )g~letic fielId.

[the oats of Oiiel~gy fioftlt(5ft5v (I ettectoA-f 'vat] a15sui-ed in this

treatmnent of the P etihltsXii. tile caen so d aci cii ilation countersq vial )Iaio

cons ider-e d, A px'opes, choitxce it). Owli thicknes-s of the do tector s3 and a. pul so

amplitude die'ftfttof nid sestiul, IX the:555 suell:t to the iion-re.a tivifstic
part of the proton spectrom leadniug to an ihfiplove-nelent -1h the sensitivity of

the x-method. With this kind of detoectorl, howewvr, measurements of a latitude

effect will be possible only in a limnited range and for low values of a. magnetic

tield.

1,'rorn the above considerations it seems that the analysis of the

cosmic ray latitude effects can lead to an estimlate of a possible lunar

magnetic dipole as two orders of magnitude lower than that of the earth. At

lower values severe limitations upon the possibility of this method are

imposed by the need of a very high accuracy in the phenomenological and

instrumental faLctors involved in the measurements.

A special feature of this method should be emphasized in

conclusion: the latitude effect on cosmic ray intensity is due to an integrated

effect over an infinite distance from a hypothetical lunar dipole; it is not

affected by local distortion due to ferromagnetic materials (such as iron

meteorites) which would invalidate a field determination given by magnetometers.

oth t-)-.,s of rneafiiurc:•ont"• v id . ixable.

mt'-i t hi story of tlhe.c. innon ma -ýy be

foxn•'ish 'h by a ,. ,

! : v / c, ;•"i,,,; n lick o 'v~lrc ' :.' 22 tb ot':!:e _2., or.''2"n,

stu .>f, ce, • " • , . t• f ' :: ,, r .•• it I( ; .. '*- .

A A)A
depths of the moon':; suriace cou.td d help i -oivi, the probleii of the

moon's history,

Two different types of radioactivity can be ex<pected on the moon.

One will be a natural, whose level depends essentially on the con tent of the

K140 and of U and Th famiilies. The other type will be induced by cosmic

rduiati-ou and be due to unntable evaporaLion fragments, fission prodoc, and

neutron activated isotopes produced by primary cosmic radiation and by its

secondary originated in the moon's crust.

.For an evaluation of the radioactivity of the moon's crust we

may take into consideration the fact that, whatever moon theory we accept, 6

the moon's surface is believed to be covered by meteoric materials whose

natural and induced radioactivity will appear at the surface and down to a

certain depth of the moon's crust. We can assume for the moon's surface

the average measured radioactivity of meteorites found on earth; this assumption is also supported by the fact that the determ~nation of age from the

7

break-up of same meteoric material indicates their lunar provenience.

It was recognized that meteoric material does not show a radio8,9

activity directly measurable with the standard techniques. However,

chemical separation and special low level counting techniques proved the

existnce i-Ln mneteorites of a natural and of an induced radioactivity. 9', i

Neutron fission and nuclear emulsion techniques were also used

recently for the detection of the natural radioactive elements in meteorites. 12

From the experimental results it seems reasonable to assume that the
average c(oliteilt ot thl-e If tI'l fao% e1 ; elete t I of ihe ot (1(e1 of 10 9 grains per

gram of o-uteeia1, with afI aetivity oC)f / - 1O di( litt (n i1 Rg, Fox the

1-,4 0 an activity of the oxdelt of 2 disint min g A can be assunmed. 13

Me a s' 0r( ent ot 0 diffe cent tnio: i e )or c o-10 tot [ a1 I[ of Ioecent fall or

14

unknown terrestrialI age proved that, accor-ding to the evaporation theory,

the low Z evaporation products are the 10or:e abundanit, the II3 being the main

source of induced radioactivity in meteorites. 15, 16

For short-lived isotopes, the activity at equilibrium, under cosmic

ray irradiation in space or at the xnoon's surface must be evaluated by the

relative yields obtained with artificially produced high energy particles. 17

Some contribution in the total induced radioactivity is due to

neutron activation. Fission products due to the possible content of uranium

mentioned above will give a negligible contribution in the overall radioactivity.

In Table II is reported a list of radioactive isotopes expected on

the moon's crust with their average activity perc grain of material.

'1 able 1.1

Isotope Mean f,.tu Activitv Disint/Min g

1 AI . ?,y 0. 5

3 d 0. 06

>el0 , 10 y 0. 005

A12 6 106 Y Fly 0. 05

Ci 3 6 3 × 05 y F3 0. 01

G060 2 , i. 0?0

K"i0 . : ", Fl (89%),y 2

U, Th n~f3,' 0 002,
Afa iii hhow Tin'ahie U, mas u i 11e isotope'; a1re Pi- e.lnIitice 1 a. An1

otiti-nate of the counting rate in a, thin counter of a unit of cross. sectional

area and 100 per cent detection efficiency niay be made assuminp that one -third

of the disintegrations gives -y's of average energy 1 1 Mev. With a total of

natural and induced -y radioactivity D) -\1 disint rmin 1 g-1 the expected

cournting rate in a medium of average atomic numbe:r Y 1 I1 will be:

7/ 7Ž , 2, V) cV t&ront - c ,; 

'It will be of special interest to comp:,.re this level of counting

rate with that expected by artificial activity nd Aced by detonation of a nuclear

weapon on or near the moon.

The measurement of the above fi.,ure ofa-, 5 counts cmry) xmnin'l

is quite low and a measurement would require at least a special low level

counting technique. A measurement of thiE kind could be a serious problem

on the moon because of the high background due to the cosmic radiation,

Section Three

Cosmic Ray Intensity on the Moon

In considering the feasibility of radioactivity measurements on the

moon, we found that the cosmic ray background may be a serious obstacle in

the measurements.

WAre atternpteor nn eval.inn 1-i o-f t-he cosmic ray flux at the surface

of the moon and under its crust, due to the absorption of the primary radiation

and to the secondary particles that will be produced in penetrating the lunar

crust.

189
.Vo0r: tlihe intemnity of the cno.i ( (adiationl at tile mloon's surface(l,

we may a.s - m-ne the value. unasouro d at, the top of the atmo ophere at high

latitule. lor an inf•.ltnlal cut -off of the or deo of 300 Mev for protons,

the primay cos•nic ray intenesity inl 0.?,5 par.ticlenj, c ec"n sterad-1

In the absence of a.n axt•incphe 1 )il , thi n io the ocxinidirectional

intoe flity and it fives Ia flu.:

i1 /

and a counting rate of 47 conunto m cmnl"

A comparison of this value with the radioactivity level of

5 counts min"-1 cm' evaluated above shows that some system of anti.-coincidence

or baclkground discrimination must be used,

An appreciable amount of albedo radiation is expected at the

moon's surface. An evaluation of this contribution for the wide energy

distribution of the cosmic ray is not so obvious, Measurements made in our

upper atmosphere18, 19 may suggest that the backward flux of radiation is of

the order of 25 per cent of the incident flux. Thin radiation ie xmnostly

composed of electrons and gfamma rays of energy below 100 Mere

3he }.,1iC mjce of the albedo r:adiation will exclude the poen;ibility

of iug Olestw th :doac .:l Ii\ty by pIac:ing on the m)oonso ,surface a d Ctector

shielded by a nc/ito s.y.jtur a of aet. -coincidennce in all. the dIirections except

toward the xnoon'i; sjur:face.

T..he re Ia. lvely high flux. of tih prirfla-y and aIbedo radiation may

lead us to the conni.u.t;io, that c , y c ft'( eoot hi cding 'I atnd , 4 nr anti coincidence
systern with an efficiency o.1 th, or-dcr of 9') pc.• cent will be necessary in

order to measure the radioactivity o)f a mooon sample. It i!s veiy doubtful,

however, if such efficiency can be obtained because of all the ionizing and

non-ionizing secondary radiation produced by the cosmic rays in the apparatus

itself.

IFor measurerrient of the radioactivity at some depth inside the

moon crust the conditions are somewhat better because of the absorption

and degradation in energy of the primary particles.

The absorption of the primary cosmic ray cannot be described

with a simple absorption process. What happens inside the moon crust may

be represented with a simplified scheme. High energy primary particles

strike the moon's surface from all directions and in their first collision

with the matter they produce showers. Proton, neutron and 7r mesons are

emitted in such collisions. Some of these particles have energy sufficient

to produce secondary showers and through several generations the energy

of the primary flux is distributed and absorbed.

A cosmic ray cascade is expected to develop through the moon's

crust, quite similar to that produced in our atmosphere. There is, however,

one great difference. In the atmosphere most of the Yr mesons, because of

their short mea.n life, decay into v. mesons before a nuclear interaction. In

the d-nset material of the moon they contribute with protons and neutrons to

the , -.veloprnent of a nuciecnic cascade.
Doe to the largte pyopooot ur4 ,1 i~n 'o ti ins the "uhowe is, a

transition effect in expected fot lhe ouclenxic component in the moon'n crust,

while in the atino sphere the nucilton( c(ioiponlsnt it; exponentially absorbed.

Gaitxa rays produced in the decay ot neutral pionn givo origin to an electro.-

photonic cascade. Mue to cxtrei ely slaowt ve an life of the u's, the gross

beha vior of thin castcade does not depend on the concentration of the matter

and is expected to le the same in our" atrnowphere and ins ido the lunar crust.

The intensity should first increase, and after a broad maximumn at the depth

of about 150 g/cmz, it should fall off exponentially with increasing depth.

As a consequence of these transition effects, the flux of the

cosmic ray through the lunar co,,unt will be down a certain depth, even greater

than at the surface.

The intensity distribution of the cosmic ray cascade through the

lunar crust can be described by equations of absorption, rate of interaction

and yield of shower particles for several, generations cn the development of

the cascade. With some assumptions, the problem can be treated in a simple

way for an approximate solution adequate for our purpose.

We can a.s;sonme equal absorption and interaction length and that

high energy pat'cie tose theitr e'or.y only by nu.I]car inletoracti ns. In a

uni..*lmnw .;norp! tre utnent of t' n,!)lc• •, ile ii-iuensj.ty of the prim-)ary

XVw A an wt"at - tn rawc 'xprt.s(d by-
ieh ycO~ v )d1.) l 0 , I ,. z5 01 1 1 .

whexre S, is thi Yield oi ý;howcv l t >l l po ille U.tion. -n 

JThe sc o dlli ý 1ý I'o fl I okq;I) 11'.( soti a xu I 1 ro 1 a-i the1 O flux

of iLe firi: genelration wvill h :

which integrated gives:

130

These particles wi].], proceed with a rate of interaction

producing the number of socondaries

"o /i . " .•

anrd so on. T in.,Jly n[he of Ohew 1)[1, i co ,og ion at ;. depth x will be:

From experime'nt with ucl' 1 ro. ion:, re tkow that the spectrum of

20

secondaries is inutependentI of tOw cwjly of the primary. 'Phen

S?. S3 .... :: , . 'lc ,.xaensit.y at it depth x is given by the summation

of the inte _sities of ali the genieration s

o /-" . -.- ),' -% .(-•. xv
With caper huentad vahte o of SI and I a(d tor a;I in-ttensity at the ,iurface of

0. ?.5 partic lee/ cm' sec stecad, we obtain:

TJMh, vailu(s of the intensity / of the nucleonic component at

ff........ entd ..... h or crust aUe shown in T'ablc III. About A0 per cent of

the particles are protons, Z0 per cent neutrons and 60 per cent charged r

mesons. The yield of tow energy evaporation particles was neglected in this

computation, Because of their short range they (1o not contribute appreciably

to the. flux.

Table 1I1

Depth Intensity

(crn) (particles/cm2 sec sterad)

0 0. 25

10 0.32

20 0. 35

30 0. 35

40 0. 33

50 0.31

70 0. 26

110 0. 16

.1)00 0.025

300 0.0034

In evaluating cosmic radi-ation as background when measuring

radioactivity it i.n3 neccssary also to take into account the electrophotonic

cascade. An approximate distribution of the electrons through the moon's

crust was evaluated from thu behavior of the electrophotonic cascade in our

Assuming a density of 33 glum
i0

attill(o sphe r c an d 01( it I I II:, -I . .t ; n r- Ih' L(, over a soli d a ngle

?,T, at different depths (0 o o md fO,- 4he. different path tength of the cascade

due to priu ar ies of differceni anglkn .; of inc idence.

Angular spread of the co:a;nei ray cascade was not included ill

the computation .An appreciable contribution to th( flux is expected from

scattered radiation. We n lreadv pointed out that atbedo radiation on the

surface of the moon may account for a contributicn of the order of 25 per cent

of primary flux. We assume that this correctior can be applied at all the

depths on the moon's crust. The final values cf the flux are plotted in Fig. 1.

We can see that the flux, even at Yreat depth, is quite large as

compared with the expected radioactivity. Measurement of the radioactivity

inside the lunar crust will require protection by background rejection

techniques. Even at a depth of several fee., the shielding provided by the

lunar crust alone will be insufficient to al?.ow a low level measurement.

The embedding of complex and delicate instrumentation at a

depth of several feet .)uld be a rather difficult problem.

Section Four

Cosm2.ic Ray and Age Determination

It may be interesting to consider if the cosmic ray effects on the

lunar crust can be used for an age of deposition determination.

We can take into consideration one particular process extensively

used for age determination in meteorites. 22 The H 3 produced in the evaporating

i95
I

o 1o~ 0O10

10"

0 50 100 150 200 250

C RRn

FIG. I COSMIC ;RAY FIJX T~iRUJ(.iH- 'rtHE LUNAR CRUST
1) OCe~O r W3⁄4( ii 11f fle If(1 do )

jiot diffutxee onu iI, If 1 j I ll ()(I ditt hoiighli te time can.

giv{ e a cosn ria ý' 11 Oit 'i ( O l y intene3ity did not

change throu •,I, e c. 1: 1 st I lt.' teit 1y e •( n

entiuxlate of I tic ipt 0 e ( ,ti'j 'iton , leowe, v(ye, I le' )-11 ri:c tItatel ial of which

the IX-Cmons crus t may 'Dc [or me(I al ir 's dini ed fn ontoer space by the saine

flI.x, of cosimic rays pre'aenlt onf the moion '; crust, Not all the meteoric material

has• size suffic lent (or an] eff.cieut production of -I3 by cos(mic rays. However,

the flux in outer space is integirated over a solid angle of 4'ir, twice the angle

at the moon's surface, and this may compensate for the lack of H3 production

in small-Asize meteorites.

in addition, the travsii ion , e .fecc of the nocleonrc component on

the moon's crust can account for a possible lack of He3 concentration gradient

on the moon's crust over a quite laxrge thickness. T'hese circumstances may

suggest that the production of H3 inr meteoritea pronceedis at the moon's

surface at about the same rate as in a.pace, thitu invalidating this type of age

of deposition determination.

Fhe Quoe si o of I oyayr Con Aiiiination

. " .... ...... ,, ... y . . .................. '. , ', i m t g it de oxf the corsm ic ray

and natural radioactivity ba c K pr oe ii nd I"lxi, tnoon, it is of intoereti-t to discuss

in this same contex!a theO 'din(-o ••r x'il' y lti e:I rx'iiht be produced by detonation

of a nuclear device. ' .ii ei p )ipr,)r,)' c! to teir: ptol.[le j"I to treat
(letonlation of o oneiicpn 101ah li(JIc oIf thie moon with the

tollowing as5Slll- 1

ptlon.t:

I) "IlThe fis•ion yield is 500 kiitis

)) One-half of the Lit;ion proidn t: are r etained by the moon and

one-~half are lost in outer spatce

(3) Uniform spreading of the fission products occurs over the entire

Assumptions (1) and (2,) are readily justifiable. The latter, in

particular, is conservative in view of the very high kinetic energies given to

the fragments relative to lunar escape requirements. It may be argued that

the third assumption is also conservative because non-tuniform spreading

over the lunar surface would imply regions of less contamination than will

calculated here.

Using the known decay characteristics of mixed fission products, it

is very simple to calculate activity deposited in disintegrations per crm2 /sec.

This is shown in Fig. ?. Yrom this curve one may make the observation that

by a month or two, for the detonation of a one megaton weapon, the decay

rate is down to roughly the oidei of the pri dnary cosrnic ray background.

This calculation r preseni;; a IAI upper kiaii h1)e cuse of at ).east two

effects: first of all, we hayvc asossn•icd 100 per cent retention of one-half the

fission fragrents. Ini acLuUal iaud howu• V ,, tilt pieullujilul•U1)gy will pro u ly

work to reduce this retained fraction very considerably. Consider a burst

occurring at about one kiloniete., above, the 1luna), saurface. At the time of

detonation the x rays f-om the bob hc, will procee to the surface of the moon
0

t- z

0

<, H

z

Ldi

LL OL

U) >-LO Lq~

0

0

IT toP. t oic 0 -N

6 _iIi v) I AH I-
and raltfe the temperatur'e otf thin layer to ver'y high values as treated in

another chaptoe of thi report. Thi, lunar gan will r0ar fy outward from the

lunarf oixr'fco and thoxc will be a gcrirai tvansfer of random thermal energy

to the directed outward velocity of the clou(d,

The problemn of expansion of an ideal ga a into a vacuum has been

treated in detail for ideal adiabatic expansions by various investigators.

Essentially what occurs isj that the gas streams out into the vacuum with a

maaximumn velocity given by

, C1 

where G, is sound speed.

A rarefaction wave moves back into the remaining gas at rest and is

important in accelerating the quiet gas into a directed motion. The fastest

moving fraction of the outward moving gas will have a thermal temperature

of absolute zero. Since we can, as a first approximation, consider this to

be a one -dimensional flow, we have the picture of the lunar material moving

upward as a gaseous piston froom the moon, On the other hand, the fission

fragments fromn the bomb are proceeding downward froom one kilometer at a

velocity of 108 cmn/eec so tlhat they arrive about one millisecond after the

x-rays have developed the lunar. gao. As a reult, the fission fragments

collide with the outward moving lunar gas which contains a large fraction

of the total momentum of the system because of the relatively high velocity

and relatively low total energy content of the fission fragments. The piston

effect of the outward moving lunar gas should impart to the downward moving

material a velocity component soch that a considerable fraction of the

A0Oo
roadioactive mate I al it) (ýcpe1.led into opace. 'V hif; entire proceeri iis s hown

schematically in .11ig. 3. A detailed treatment of this problem is obviously

quite complicated and not only momnentum transfer and questions of equilibration

times must be considered but also calculations on the range of fission

fragments through the highly ionized lunar gas plasma and the rarefaction

process in such a non-ideal medium should be m.ide, A detailed discussion

of such phenomena is beyond the scope of the present work but is clearly

indicated for the future because it appears that a marked reduction in

contamination could occur by this mechanisrr.

We can show now, however, the results of calculations on lunar orbits

for individual particles corresponding to vurious effective temperatures of

this mixed cloud of radioactive fission fragments and lunar surface material

as some indication of what might be expected. We have noted in the chapter

describing x-ray energy input calculations what sort of properties might

obtain in the lunar vapor. To any such calculations must be added energy

contributions resulting from the heating of the rarefying vapor by the Interaction and stopping of the fission fragments. Temperatures of the order of

105.K do not appear to be out of the question. If we assume, therefore, a

gas without an outward directed net velocity but at such temperatures, we

may calculate the number of particles of this gas possessing energies

corresponding to either parabolic, hyperbolic or elliptic orbits in the

gravitation field of the moon under the assumption of a Maxwellian distribution

of velocities. The results of such calculations are shown in Fig. 4 for

;0 i
(I

C)

(CC 0

I C)

A H

1)

1 Iti[1 F' rK

44U

4.

0>4CC)

(I, 

I 4 :1 Zo

7 C) JC

4

I 't-A // '4,' r CXI C

0

1L,1I- I ' CC

N

- vw I [ .,yU 

cd u

'4 / CC•C

I U) bfl

4r1:11 4 '1 S.

,-.. 0 [

I' -.44

La-iC, JtiI>

C-S

C i 

I

I I

'C
MAý';! NUJMB Ell i

L ,o • (frac thin o

, N PARABOLIC O ITS

6I / -

/

FRAC TION O)1' P ARTIC'I ,, / /

IN HYPERBOI,IC OR(BITS /

5/

5 -. / /

I1FIRACTIONO

II I / 0NPARITCLES IN

/ OBT

4 / / 

\ / /

\ \ I/ TIN O

/\/P\RICLS I

/-ELI\TC OBIT

x \ 7 /

) .... h• r

4. I

',, / 
both mass 20 paxticls, co): ref : pok1i) dig to the olivinle, and nafa 1!50 particleo,

corresponding to some average fission fragmient. It io clear from these

curves that a very large fraction of the x-adioactive material would enter

into hyperbolic orbits and thereby have an excellent chance of escaping from

the moon's surface. 'I'his effect, even without consideration of directed

velocities as discussed above, can markedly reduce the lunar contamnination.

In summary: when one considers the natural radiation it the lunax

surface, it appears clear that fairly sophisticated instrumentati!m will be

required to measure lunar radioactivity, for example, in the presence o4.

natural interferenceo Without adding a great deal of complexity, such

apparatus should be able to distinguish the modest lunar contamination produced

from a nuclear burst near the moon's surface. Such a conclusion does not,

of course, argue for the casual detonation of a nuclear weapon near the

moon, but it does appear that with instrumentation emplaced on the moon

prior to such a detonation which would, in fact, be capable of making meaningful measurements, the influence of a subsequent nuclear detonation would

not be as detrimental to the information content of the moon as is sometimes

argued. Clearly, however, it will be to the advantage of any experiment to

have data on the natural radiation before detonation of any device producing

radioactivity. When such data are available oui 'oinclusions here should be

reviewed carefully.
REFERENCCES

1. T. H. Johnson, Rev. Mod. Phys. 10, 219 (1938).

2. G. Lemaitre and M, S. Vallarta, Phys. Rev. 43, 97 (1933),

3. B. Peters, frogress.in CosmicR P sics, Interocience Pub, In(..

New York, 1 (1952).

4. B. Peters, Handbook ofPysics, McGraw-Hill Co. Inc., New York, 9,

201 (1958).

5. R. B. Baldwin, The Face of the Moon, Field Museum Nat. History Pub.

151, 211 (1911).

6. H. G. Urey, Sky and Telescope, 15, 108, 161 (1956).

7. H. C. Urey, Private Communication.

8. C. W. Beck and L. LaPaz, Am. Min. 36, 45 (1951).

9. T. P. Kohman and W. D. Ehmann, UNESCO/NS/RIG/219,

10. G. J. Wassemburg and R. J. Hayden, Phys. Rev. 97, 87 (1955).

11. G. L. Bate, H. A. Potratz and J. R. Huizenga, Geochim. Cosmochim. Acta,

14, 118 (1958).

12. S. Deutsch, E. Picciotto and F. G. Houtermans, Geochim. Cosmochim. Acta,

14, 173 (1958).

13. F. G. Watson, Between the Planets, Th'e Blakiston Co., Philadelphia (1941).

14. K. J. LeCouteur, Proc. Phys. Sot.. A63, 259, 498 (1950).

15. S. F. Singer, Phys. Rev. 90, 168 (1953).

16. E. L. Fireman and D. Scl.uldrzer, Geochim. Cosmochim. Acta, 11, 252 (1957).

17. L. A. Currie, W. F. Libby and R. L. Wolfgang, Phys. Rev. 101, 1557 (1956).

18. G. J. Perclow, L. R. DJvi.i, C. W. Kissinger and T. D. Shipman, Phya. Rev.

88, 321 (1952).

S05
19. S. E. Golian and E. H. Krause, Phys. Rev. 7,1 918 (1947).

20. U. Camerini, W. 0. Lock and D. H. Perkins, Progress in Cosmic Ray Physics,

Interscience Pub. Inc., New York, 1 (1952).

21, B. Rossi, High Energy Particles, Prentice-Hall Inc., New York (1952).

22. G. R. Martin, Geochim. Cosmochim. Acta, 3, 288 (1953).
Chapter VI

COMPOSITION OF THE LUNAR SURFACE

AND THE MAGNETIC FIELD OF THE MOON
AND 11\4 At PDKIC 1 'JJý; .1) OV .1iv: MOON

At the pre sent time tbek'o ax-e ihveo iot nece ssrai'iiy muwtually exclusive,

ideag on th mp-Tnts il i on of the 11iý l ý, f .k eface m io te k, ill:

(1) The lunar maria are of Itunac composition, being formed by

impacts of large bodies of afateroidal mass at a time when the

lunar interior was molten at some tens of kilometers beneath

the surface. Impact caused lava upflowa at the impact site by

penetration towards the lava depth and in the neighborhood of the

I

impact site by hydrostatic compensation. On this basis a cloud

produced from a lunar mare by detonation of a nuclear device

should have a chemnical composition comparable with that of

terrestrial surface material of density less than about 3. 3 gm/cc.

Consistent with view (1) is the assiumption that the mare-~less

southern highland area of the moon ,3 the old accreted crust,

exhibiting the la.Bt pieceu of oiatter to falli on the accreting protoooThio inat r ia] 0sha0- ;).1so be x'oughly of terreistr.'l ,,) c

C~rp35t10 V! t. p ~1~ asIifibt deoletion of the 1i'ýaviei e_,o-nints,

(2) Thu leone ai n alle, of kneteoriti~c cornpoestion, bcWing form-ed by

impacts of la.- ge bodice of arote rotd(al mass, the ene1ýrgy for rneitill g

and the mnoltn o en otli supplied by the ix,-qle cting object
itself. 2 On this basis a cloud produced from a lunar mare should

have a chemical composition comparable with that of objects of

asteroidal mass. The only evidence we have in this regard is

from analyses of meteorites, coupled with the probability that

meteorites are collision products from the asteroid ring. If the

masses producing the maria in view (2) are meteoritic in composition, then the cloud would have a substantially different composition

from that of view (1). In particular, more iron should be expected.

O the other hand, it is certainly possible that the impacting

oojects were small bodies accreted in the vicinity of the moon

contemporaneously with the formation of the moon; and in this

case, it is certainly possible that their composition was identical

with that of the southern lunar highlands. (Also consider in this

view an unreworked primeval area.)

(3) At least some of the lunar maria, especially Mare Imbrium, are

cometary in origin, being the result of collisions of comets and

3

the moon. In this view a cloud of mare material would possibly

contain appreciable proportions of cometary matter; in particular,

carbon, nitrogen and oxygen,

(4) The lunar maria are of meteoritic composition, being deep bowls,

filled with micrometeoritic fragments which have fallen on the

4

moon during the last few billion years. The dust may be loosely

5 packed, or, as suggested by Whipple, congealed into a fluffy

-09
rnaLrix in V,(', ', ul ( 1uW ., ,lface. lIn

this view, at least the uppei regiong of the mariaa would have

composition very-similar to that of rrncroineteorites collected

in the immediate vicinity of the earth; they would therefore have

high iron and nickel abunday ces.

(5) The lower regions of mnaria dust layers are of approximately

cometary composition, being formed early in the history of the

moon, either by infall from the solar nebula from which the moon

was formed 6, or by infall from the primitive, short-lived,

7

reducing lunar atmosphere, (There may, of course, be no

distinction between the early lunar atmospher e and the last stages

of the solar nebula in the vicinity of the moon.) The contribution

to the cloud from such material would be primarily hydrogen,

carbon, nitrogen, and oxygen.

(6) The lunar maria are of indeterminat- composition, being deep

bowls, filled with ionized dust partic]c s which have been chipped

from lunar surface ma~tc iiu, by solar electromagnetic and

8

corpuscular radiatioro. 8In his view, a cloud of mare material

might have any of the above..-mentioned cormpositions, depending

on the material from which the dust is chipped. If solar protons

have been arriving on the moon's surface at approximately present

rates for the last few billion years, the lunar surface material

might be expected to retain a saturation arrmount of hydrogen,

()
and this might be reflected in the cloud composition.

Although there is considerable overlap in the above views, the following

tentative conclusions can be drawn: if the cloud of mare material is

substantially of terrestrial surface composition, views ( 1) and (2) are

supported over views (3), (4), and (5). If the cloud has large iron and nickel

abundances, views (2) and (4) are supported over views (1) and (3). If the

cloud has large carbon, nitrogen, and oxygen abundances, views (3) and (5)

would be supported over views (1) and (2). Because of the solar proton flux

mentioned in view (6), high hydrogen abundance in the cloud v.culd not

necessarily support any of the views over any others. Of course combinations

of alternatives are possible. For example, suppose the cloud has essentially

terrestrial surface abundances of Si, Mg, Al, Ca, Na, etc. , but with

appreciable admixture of Fe, Ni, C, N, and 0. This might suggest that

views (1) or (2) are correct regarding the nature of the maria, but that the

maria are overlayed with small amounts of other material, originating as

in views (4) and (5).

Spectroscopic observations of the general sort discussed elsewhere

in this report could provide data on these questions of composition.

Magnetometric observations, and possible directed motion or trapping

of ionized detonation products in the lunar or lunar -terrestrial magnetic

field, would give information on the lunar magnetic field and possibly on the

interior structure of the moon. It is generally expected that the field will

be small but various views will be summarized here. Reference should be
made to the Chapter on the interplanetary environment for very recent

comments in the light of Russian reports of lunar eruptions. (See also the

translation of N. A. Kozyrev's Prioroda article in Information on Soviet

Bloc IGY Cooperation, PB 131632-63 U. S, Dept. of Commerce, April 24, 1959,

p. 2. )

If a field of the order of the earth's (0. 1 - I gauss) is detected, this

will be taken as strong a pri-ori evidence for the existence of a liquid iron

core. There is some evidence that the earth's magnetic field arises from

hydromagnetic motions in a terrestrial liquid iron core, 9but it should be

emphasized that no satisfactory theory for the origin of the terrestrial field

exists, 10 there is direct seismological evidence for the existence of a liquid

terrestrial core, but of course no present lunar seismological information,

and there exist theories for the origin of planetary magnetic fields which do

not involve liquid cores. 9Consequently, conclusions on the structure of

the lunar interior proceeding from evidence on the presence or absence of

a lunar magnetic field should be treated with some caution.

Since the mean density of the moon is comparable to that of terrestrial

surface material, an extensive iron. core within the moon would seem to be

immediately excluded. However, there is an interesting difference of

opinion on the possible existence of a. small liquid iron core, hinging on the

question of whe ther the moon was ever molten on a large scale. If there

were appreciable melting at some time in the moon's history, a differentiation

of irons and silicates would be expected, forming an iron core and a silicate

Z212
mantle. This is substantially the view o,.f Kuiper. 1 Urey, 12on the other

hand, believes that neither the earth nor the moon was ever extensively

molten. The earth's core is attributed to a slow trickle of irons to the

terrestrial interior throughout geological time, the earth's gravitational

field and some internal heating being the primary causal factors. With a

smaller gravitational field, much less internal heating, and a smaller

proportion of iron to begin with as is evidenced from the density, Urey

anticipates no liquid iron core on the moon. Finally, the Soviet school

associated with the name of Schmidt 1 3 holds that the earth's core is not

liquid iron at all, but rather a hypothesized high-pressure modification of

* We are indebted to Professor H. C. Urey for the following comments made

after review of a draft of this report: "The composition of the old accreted

surface, if indeed there is any present on the moon, should be of cosmic

composition rather than of the earth's surface. The material of the earth's

surface has been highly differentiated by partial melting and flow of material

to the surface of the moon. ( . .. ) (Kuiper) has silicates floating on the

liquid materials below. The moon accumulated at low temperature but heating

in the interior melted the whole interior leaving an accreted crust floating

on the surface. We have here the curious situation where a solid floats on

its liquid, water being the only common example of this situation. Your

statements in regard to my views on this subject axe correct if we go back

to The Planets, but you will find a later discussion of this subject in the

Proceedings of the National Academy of Sciences, Vol. 41, 127-144, see

particularly page 140. The abundance of the radioactive elements in this

paper is incorrect and this was corrected in Vol. 42, 889-891."1 Reference

to W. H. Ramsey MNRAS 108, 406 (1948), and MNRAS Geophys. Supp. 6,

409 (1949) should be made in connection with the high pressure modification

of silicate theor'y of the earth's core.

213
silicate with about the viscosity of tar. However, it is also believed that

the moon was extensively molten, while the earth was not. Hence, if there

are any magnetic consequences of a liquid iron core, they would be expected

on the moon, but not on the earth. A summary of various views is given in

Table 1.

Measurement of the magnetic field on the moon may also provide

information about fluctuations in spatial magnetic fields due to ionized

particle streams from the sun and similar effects due to plasmas originating

in a nuclear detonation near the moon. The same instrumentation may be

modified to determine residual rock magnetism of the lunar surface which,

as indicated above, will be important in theories of the moon's origin.

213a
Table I

LUNAR MAGNETIC FIELD

Source of Field Magnitude Remarks

10-5 oersteds

Liquid Corea 50,000 Considered unlikely

Measurable by lunar satellite .------...............................................................

Moon once part of earthb 40 FieId arises from cooling in

earth's field

Moon formed from

condensed gasc 0

Moon formed from Intensity of magnetization of

accumulation of meteoric unknown, but existing meteorites hasn't

materiald small been determined

Mechanical rotation of

moone 7

Thermoelectric origin Field due to cooling in

in early lifec 100 self-field

Solar Windf 20 Magnetic noise

(RMS', Sets limit of required

instrumental sensitivity

a. S. Chapman and J. Bartels, Geomagnetism, Oxford University Press (1940).

b. G. C. Darwin, Scientific Papers, Cambridge (1910) and H. Jeffreys,

The Earth, Cambridge (1924 2nd ed. (1929).

c. E. H. Vestine, "Utilization of a Moon Rocket System for Measurement

of the Lunar Magnetic Field," RM-1933, ASTIA No. AD 133008, July 1957.

d. H. Urey, Sky and Telescope, 15, 1 (1956), and H. Urey, The Planets,

Their Orijn and Development, Yale University Press (195Z) Also ref. c.

e. P. M. S. Blackett, Nature. 159, 658 (1947). and H. A. Wilson,

Proc. Royal Soc., 104, 451 (1923). (Blackett is quoted as having

abandoned this theory by H. C. Urey, private communication

September 4, 1959).

f. E. N. Parker, Phys. of Fluids, 1, 171 (1958), and P. Meyer, E. N. Parker,

and J. A. Simpson, Phys. Rev., 104, 768 ý1956).

214
Although it is likely that the most important question, presence or absence

of a substantial lunar field per se; will be at least partially answered by

presently contemplated lunar probes in advance of any nuclear detonation

experiment, it is worthwhile to consider briefly the entire experiment here.

From Table I we note specifically that in the absence of a present

liquid core, a field of the order of 5 to 100 gammas is predicted, depending

somewhat on the assumed origin of the moon and conditions during its early

history. If a present liquid core exists, the lunar field may be taken to be

of the order of the present earth's field, 50, 000 gammas.

A special source of magnetic field in the region of the moon and

especially germaine to the measurement problem is the Solar Wind 1 4

which is predicted to cause an rms magnetic field fluctuation of the order of

20 gammas. This value appears to be confirmed by indirect experiments 1

and the same measurements also show that the average field in interplanetary

space is about one gamma. In the present context, the 20 gamma fluctuation

must be considered a noise signal, but obviously measurements confirming

this value will be of interest with respect to the solar wind phenomena. A

related effect may occur following a nuclear detonation due to the ionized

plasma produced. It is obviously of interest to measure this also.

From the above brief summary, it is clear that magnetic field

measurements are of considerable importance in determining the present

state of the lunar core. A field greater than, say, 500 gammas would imply

a liquid center. Caýr ef al measuremnents with an expectedi nr-' ý--itude of about

21-15
10 gammas may provide information about the moon's origin and the solar

wind phenomena. It would be highly desirable to obtain data over a relatively

long time interval - of the order of three months - so that temporal effects

might be determined, One such effect is that possibly due to electric

16

currents in the lunar atmosphere, which would have a 27-day period.

Measurements taken prior to landing a lunar prpbe on the moon are

likely to be unsatisfactory if the moon's field is below about 50 gammas.

Presently contemplated lunar satellites will have an altitude of a few hundred

kilometers and may be useful if the field is in the range 200 - 1000 gammas.

Thus, to obtain information beyond the primary question of presence or

absence of a strong lunar field, it will be necessary to put the instruments on

the moon's surface. In order to realize some information concerning the

shape of the lunar field, at least three widely separated instrument packages

are desirable. If possible, continuous signals during flight should be undertaken in order to compare with present earth sitellite magnetometer

measurements relating to the earth's field and ring currents near the earth. 17

The instrumentation required to carry out such measurements must

have a sensitivity approaching one gamma and be of small size and

18, 19.

lightweight. The proton precession magnetometer is being used for

current earth satellite experiments. It has the necessary sensitivity and the

considerable advantage of not requiring calibration. Furthermore, the

signal is an easily transmitted audio tone whosefrequency is a meas.ure of

the field. Thus, the precision measuring instrument (a frequency meter)

need not be a part of the airborne instrumentation. The instrument has the

216
disadvantage that it measures the magnitude of the field and provides no

directional information. It inherently is not a continuously indicating device,

which means short time fluctuations in the field cannot be measured. On the

other hand, power requirements are reduced by pulse operation.

Since the frequency of the signal is directly "?roportional to the field

strength, frequencies of the order of 0. 4 cps are expected for a lunar field

of 10 gammas. This is an inconveniently low fr:.quency to transmit and

measure, but probably can be used. However, it may be put into a more

suitable range with a small permanent field sipplied by a magnet. The

accuracy of the instrument is sufficient to e;,sily read a 10 gamma departure

from a 10, 000 gamma steady field, in whica case the signal frequency is in

the range of 40 cps.

20

A more recently developed device, the Rubidium vapor magnetometer

also appears to have promise. It, too, :equires no calibration and is likely

to be lightweight. The signal does not appear to be as convenient, however,

and the device has not been miniaturized for satellite applications.. In

addition, tb-re is some question about its operation in fields as low as 10

gamma.

A rotating coil. technique has also been considered 1 and has been

employed in rockets for earth's field measurements. In this case a 27, 000

turn coil on a mu-metal core generates an a-c voltage when rotated in the

field. The rotation is supplied by spin of the vehicle itself and is about 10 cps.

In the earth's field a signal of 0.2 volt is observed. In the lunar application

a 40 microvolt signal would be generated, which is rather low.
The signal could be increased by greater spin frequencies of the

carrier. This tachnique has the considerable advantage that stray fields

generated within the miss-ile do not influence the measurement since they

rotate with the coil. Also, the systemn is inherently simple and lightweight

since all that is required is a coil, plus perhaps a transistor amplifier.

However, it is incapable of operation from a stationary vehicle as one landed

on the moon. Spinning the coil independently of the carrier leads to commutator

noise difficulties and is considered less desirable than some of the other

techniques available.

The classical earth's field magnetometer is the well-known fluxgate

device. Although of sufficient sensitivity, it requires calibration and does not

appear attractive on a weight basis. In light of present information, it

appears that the precession magnetometer developed for earth satellite use

may prove most suitable for the lunar probe if a bias field can be used.

2,1
REFERENCES

1. R. B. Baldwin, The Face of the Moon, ,Chicago (1949); G. P. Kuiper,

Proc. Nat. Acad. Sci. , 40, 1096 (1954).

2. H. C. Urey, The Planets, New Haven (1952); Observatory, 76, 232 (1957).

3. Z. Kopal, Colloquium at Yerkes Observatory (1958). Kopal pointed out

that statistically one would expect two or three collisions between the

moon and a comet in 5 x 109 years.

4. See F. L. Whipple, Vistas in Astronautics, 3 (1959), in press.

5. Ibid.

6. See F, Hoyle, Frontiers of Astronomy, New York (1955).

7. "Some Speculations on the Possibility of Organic Matter on the Moon"

ARF A 119 Report (1958).

8. T. Gold, Royal Astronomical Society Monthly Notices, 115, 585 (1955).

Sky and Telescope, 15, 161 (1956).

9. See E. Bullard, The Earth As A Planet, Chap. 3, G. P. Kuiper, ed.,

Chicago (1954).

10. Ibid. However, a recent successful model of a self-sustaining

hydromagnetic dynamo is due to G. Backus, Annals of Physics, 2, 180 (1958).

11. Ktiper, loc. cit. See also Bullard, loc. cit. A detailed and impartial

discussion of the possibility of extensive melting of bodies in the solar

system is due to D. W. Allen a.nd J. A. Jacobs, Nature, 177, 155 (1956);

Geoch. et Cosmoch. Acta, (1956); Science News, 45, 61 (1957).

12. H. C. Urey, The Planets, New Haven, (1952); Proc. Nat. Acad, Sci.,

41, 127 (1955); Vistas in Astronomy, 2, 1667, A. Beer, ed. , London (1956).

13. For articles in, English, see B. J. Levin, Colloque International d'Astrophrsique, Iiege (1957) p. 186 and subsequent discussion; B. J. Levin,

The On - of the Earth and Plan\ets, Moscow (1956).

1 .. E. N. 'Parker, Phys. of Fluids, 1, 171 (1958).

15. P. Meyer, E. N. Parker, and J. A. Simpson, Phys. Rev. , 104, 768 (17j56-).

219
16. E. H. Vestine, "Utilization of a Moon Rocket System for Measurement

of the Lunar Magnetic Field," RM-1933, ASTIA No. AD 133008, Jvly 1957.

!

17. J. A. Van Allen, Scientific Uses of Earth Satellites, Univ. Mich. Press,

Ann Arbor, Znd ed. (1958).

18. L. J. Cahill, Jr., J. A. Van Allen, J. Geophys. Res., 61, 547 (1956).

19. G. S. Waters, P. D. Francis, J. Sci. Instr. , 35, 88 (1958).

20. T. L. Skillman and P. L. Bender, J. Geophys, Res., to be published.

21. T. Bergstral, Aeroneutronics, Inc., private communication.

U2
Chapter VII

SOME ASPECTS OF PLASMA AND MAGNETIC FIELD EFFECTS
Chapter VII

SOME ASPECTS OF PLASMA AND MAGNETIC FIELD EFFECTS

In this chapter we shall consider the effect of the environment on the

phenomenology of a nuclear device detonation occurring in the vicinity of the

moon. The discussion will, at best, be of an exploratory nature since the

problems involved are very complicated and, in some cases, insufficient

data prevent any analysis in detail. We shall first wish to establish, as

best we can, the properties of the interplanetary medium in the vicinity of

the earth's orbit where a detonation may be considered to take place. We

shall be specifically concerned with the natural particle population in

interplanetary space, the magnitude and shape of magnetic fields and the

effect of various solar radiations, both electromagnetic and corpuscular,

on the material produced in the detcnm.on. Ln considering the magnetohydrudynamics of the resulting plasmas (that rarefying off the surface of the

moon or coming from the bomb directly) one encounters a problem beyond

our cap.bility for detailed consideratior '.i the limited time available. We

will therefore concern ourselves with sir' Ie particle dynamics and a bri.ef

discussion of the overall phenomena. Cl.•arly, there are areas here x- -er'e

considerable additional W'ady is necessary to get even relatively crudýe

qoantitative irh•.rnation.

We will also con-cider the effects of solar plasmas on inqtrument;ai

i.,;c:: other than the 1., r-)b %%ihich might be invoiv1.- in sci *ntific e:perL:::-

n:-r or on the moor.
Section One

The Quiescent Solar Plasma and Solar Streams

There exist a variety of observations which lead to the conclusion that

interplanetary space out to somewhat beyond one astronomical unit

(1 A.U. = 1.5 x 10 3cm - radius of earth's orbit) of the sun is occupied by

a tenuous highly-ionized gas. Details as to the composition, temperature,

and the possible presence of non-Maxwellian components are not completely

certain and such knowledge must presumably await the results of space

probe experiments, some of which are now underway. Strong evidence for

the presence of an outward streaming component from the sun has, however,

been presented by Biermann 1 ' 2 in early papers and more recently. 3 He

shows that the accelerations and radial alignment observed in type I comet

tails containing CO+, NZ+ etc. cannot be explained in terms of solar

radiation (light) pressure. These accelerations ordinarily appear to be

i00 to 200 times as large as solar gravity but may reach 1000 times solar

gravity under very active conditions on the sun. A streaming solar hydrogen

plasma would produce the observed accelerations because of electric fields

set up by the greater stopping power of the cometary material for electrons

relative to the protons. Neutral ionized streams having velocities of

about 1000 Km/sec and densities of the order of 103 - 104 particles/cm3 at

the orbit of earth were suggested to account for these observations. Biermann

points out that the highest accelerations can be related to interactions with

individual solar corpuscular beams of still higher density presumably
connected with discrete geomagnetic storms. On occasions of high solar

4 O5

activity, the suggested density of the streams may reach 10 protons and

electrons per cm 3 at 1 A. U. while velocities might be upwards of 2000 Km/see,

Similar values may be obtained from observations on changes in solar

radio noise.

For a quiet sun, Behr and Siedentopf6 have examined the polarized

component of the zodiacal light and find an electron density at 1 A.U. of

3 700 particles/cm . Electrical neutrality would then require an equal

number density of protons. In a discussion of Biermann's early papers,

Kiepenheuer7 derives a lower limit for the particle density of about

six particles/cm3 assuming a velocity of 1000 Km/sec for the solar plasma.

8

Recently, Kuiper has suggested that a reasonable average density

3 for quiet conditions might be about 600 protons/cm

9

In a series of papers, Parker has summarized various geomagnetic

effects which are assumed to be associated with discrete solar streams

from an active sun. He goes on to suggest possible mechanisms for suprathermal particle generation as a possible sou- ce of auroral effects and

considers cosmic ray modulation by solar plasmas as well as magnetic

storm effects. From these considerations, densities for quietest conditions

S~3

appear to be at least 101 ions/cm with a minimum velocity of 500 Km/sec.

Under active conditions, densities of 105 ions/cm3 and velocities of

1500 Krn/sec or more are obtained.

10

Russian workers studying the dissipation of a high temperature nornZ24
stationary solar corona in the presence of a directed stream of matter also

conclude that the density of particles in solar streams near the earth is

between 103 and 105 particles/cm3. Summaries of observation3 together

with some views on the nature of the solar plasma prior to the launching of

11

the Russian space probe of January 2, 1959 have also been given.

Velocities of between 1000 and 3000 Km/sec are suggested with stream

3 3 concentrations ranging from 10 to 103 particles/cm . With the low density

stream, a background gas at about 104 degrees Kelvin is also considered

to be present.

It should be emphasized that the properties of the solar plasma under

didcussion pertain to conditions away from the perturbing influence of

planetary magnetic fields, Such fields will shield out or markedly change

the influence of the solar plasma in nearby regions of space. In the case of

the earth, we may compute the approximate distance beyond which solar

effects to be discused will be active. Roughly, the requirement is that the

plasma kinetic energy density exceed the magnetic energy density and we

may write this condition as

In the equatorial plane of the earth, assuming a pure dipole field, we have

from which the minimum distance for onset of the effects is

025
Assuming the earth's surface field (horizontal component) as

Bo = 0.4 gauss, setting ro = 6.4 x 108 cm as the terrestrial radius and

taking the stream density n to be 103 particles/cmr3 with v = 103 Km/sec

and m appropriate for protons, we find R = 2.9 ro. For this illustrative

case, we would expect effects beyond 8, 000 miles from the earth's surface.

This is to be taken only as an order of magnitude figure for a variety of

reasons, particularly because of the perturbation of the earth's dipole field

by the plasma itself and possibly by a radial solar magnetic field. It does

appear that "stationary" satellites orbiting at 22, 000 miles might be affected.

Note that r varies slowly with n and v.

In the case of the moon, as discussed in another chapter of this report,

it is not known what magnetic field to expect and so it is not possible to

calculate the region around the moon which would be protected from solar

streams. We do, in general, expect the lunar magnetic field to be low, and

it might be mentioned here that the recent Russian observations on gaseous

emission from the moon have been interpreted as being due to excitation

from the solar plasma during interaction with gases released from the

lunar surface. That these gas releases are not volcanic and therefore do

not imply a liquid core has been suggested by J. H. Fremlin of University

of Birmingham among others. If these interpretations are correct, it

would re-enforce the argument that the lunar magnetic field is indeed very

small.

Before leaving the matter of the density and velocities of the solar

2.2A
streams, it should be mentiomjd that two groups have raised objections to

the general magnitudes chosen here. Lars Block, in a series of papers in

12

Arkiv f6r Fysik, has suggested that the gas densities required for

explanation of certain of the effects observed are much lower than those

suggested by Parker, for example, although no specific reference is made

to Parker's work. On the other hand, Block does not consider the observational data on the behavior of cometary tails. Furthermore, it has been

suggested that the Alfven field which Block employs for his calculation does

not fit the data currently being obtained by Babcock and Babcock but requires

larger fields than have actually been observed. The Block model has not

been pursued to the point of fully evaluating it, but it does appear at first

glance rather difficult to reconcile the cometary information with this

model which is based primarily on zodiacal light observations.

13

A second study which should be mentioned is that of E. J. Opik

made in 1956. Opik concerns himself with detailed calculations on the

interplanetary dust and the terrestrial accretion of meteoric matter. In

the process, he has made calculations of the rate of sputtering of

meteorites by the solar plasma. Such calculations as a basis for objection

to relatively high interplanetary stream densities was revived recently by

14

Bergstrahl. Opik's data both on the drag and sputtering from fast

corpuscular radiation of low temperatures may be summarized in Table I,

taken from his paper.

227
'A 1

C)

C0 N) 0

C) 10

k 00

A0 

o o 1 x a,

> 0. LO 0na,0 0

0

4)4

o )b

41 4.I

-1 0 0 0)XC

o : p~ N 0 0 ý 0 . 0. U. 0 C0

00

0 0

U 0 4 0;

0d C) 0) 0' (d0

U 0 00~

o

H 'd- ;ý I >- ; r 0

(d. U ~ mC&
His drag data are included for completeness only and are not particularly

germane to our discussions. Two points are to be noted from this table:

the average transit time, 0, refers to the timie required for particles moving

in nearly circular orbits to travel inward from two to zero astronomical unitsdistance. The time for destruction by sputtering is calculated on the basis

of a yield of five atoms or molecules for each impinging proton. Subsequent

to the Opik calculations, it has become clear that the sputtering of oxides by

ions rather than neutral a~toms of this energy is probably two decades lower

than the yield 15assumed by Opik. The calculations that we will make in

subsequent sections are concerned with metallic surfaces or, at worst, surfaces

with very thin oxide coatings so that we will take a yield of one in such cases

even though the yield for a sputtering of meteors might be 0. 05 to 0. 01.

Clearly, this is a highly speculative matter and points up the need for good

sputtering measurements on both me(teoritic materials and materials of

construction such as those treated in later sectior. s. In any case, with a

reduction of the order of one or two o.-ders of magnitude which could come

at least in part from a lower sputtering yield, the time of destruction by

sputtering as calculated by Opik becomes of the order of the transit lifetime.

The excposure time to sputtering which is appropriate for calculations

of lifetime is, of course, in part determined by the origin of the meteorites.

If one assumes that the meteorites are a result of a grinding process in the

asteroid belt, then the times of exposure appropriate for such calculations

are of the order of the transit lifetimes rather than the cosmic age of the

229
material in the meteorite. In general one must be very cautious in assigning

an effective time for the sputtering process to occur. Urey 16has recently

suggested from a considerable body of data oný meteorites that an effective

age of the order of millions of years rather than billions of years for the

stone meteorites is correct, whereas the irons range around 10 9years. He

discusses the possibility that the stone meteorites originate fromn the moon

rather than from other possible sources in which case transit timnes could be

quite short. A few last comments might be made concerning the instability

of the solar streamn somewhat beyond the orbit of earth as will be alluded to

again in the next section. Both this instability and some sort of self -shielding

might be possible explanations for the survival of iron meteorites. It is,

at present, not possible to decide what the sputtering ratio should be after

the solar streams become unstable and perhaps change their velocity distribution appreciably. It is interesting to note that this instability could occur

before interaction with the asteroid belt, e,_j. a little beyond I A. U. Opik's

calculations also ignore both the existence of a very low threshold for some

sputtering processes and the possible existence of elements heavier than

hydrogen in the solar streams. It is possible that both of these effects could

be used to force the effective velocities on his model to such low values as to

endanger the entire structure of his theory. These points will be treated

further elsewhere. 1

3O0
Section Two

The Interplanetary Magnetic Field

Measurements on the actual magnetic field existing in the apace will

become available in the very near future. In the meanwhile, however, the

magnitude and the nature of these fields must be inferred from other observations. For purposes of this discussion, we shall assume a picture of the

interplanetary field due essentially to Parker and described in references

already noted. These ideas suggest a radial solar field falling off as R-2

as a result of protons streaming from the solar surface. In this picture,

one imagines 3 dipolar field which has been stretched into a perfectly radial

one because of the outward high velocity stream of plasma. Somewhat

beyond the orbit of earth, instabilities in the radial streaming can ozcur and

a disordered entangled field of rather low magnitude results. It is not

completely definite in this model where such disordering would occur and the

general location of these instabilities is inferred from observatx..as on cosmic

ray data and solar flares. In any case, if the moon is embedded in the wellbehaved radial solar field, it becomc• poriible to discuss single particle

dynamics in a definite manner. It is clear that such an assumption is

speculative.

At one astronomical unit from the sun we desire now to calculate the

magnetic field strength on the assumption of a completely radial field. For

this purpose we, of course, need informat'on on the general solar field a•t

the surface of the sun. Data reported i- thc litqrature indicate that Xhe
average surface field could be anyo.h,,te t iom 0. i gauss to 10 gauss. Recently,

however, Babcock and Babcock have continued their measurements on the

nature of the average solar field and it appears that a figure of approximately

18

one gauss is realistic. The picture of the sun emerging is one of equatorial

disorder overlayed by a well.-behaved dipolar field near the poles. The average

field in the disordered region is consistent with tle figure we have taken, but

there are clearly local details in the structure n.-,ar the equator. Because of

the general configuration of the solar system, 'f one assumes a perfectly

dipolar field coupled with perfect radial strea ning, one would arrive at

essentially zero field in the plane of the earta with, however, very high

gradients. We shall assume that the mixing is sufficient to allow us to

ignore this consequence of perfect symmetry and shall take a field strength

appropriate to points somewhat away fromt the plane of symmetry of the dipole.

Under these circumstances, a simple ca'.culation shows that a field of

approximately 2. 2 x 10-5 gauss is appropriate. This field is sufficiently

small so that one must be concerned with fields of other origins. For

example, it might be mientioned that Hoyle has suggested a field of l0-3

gauss for regions beyond 10 earth radii. 19

These large uncertainties in both the nature of the solar plasma and

the magnetic field make us clearly dependent on future measurements before

quantitative results can be obtained.

z32
Section Three

Single Particle Dynamics

In other chapters we have discussed the formation of a plasma cloud

due to x-irradiation of the lunar surface by the detonation of a nuclear device.

Calculations were made on the energy deposition in various layers of the

lunar surface for typical weapon temperatures. The resulting rock vapor will,

of course, rarefy out into space from the lunar surface. Since it will have

appreciable conductivity it will distort and perturb markedly any magnetic

field and plasma which might be pre-existent. The interaction of a single

typical particle from this rarefying cloud calculated on the basis of no

perturbation of the environment will, however, be of interest because it can

provide feeling for some of the effects which might be encountered and might

relate to the real motion of particles in the high velocity tail of the rarefying

cloud which could precede the main body of the bomb-produced plasma. For

these fast particles, hydromagnetic disturbances would not yet have upset

the environment. We shall assume the materia' of the rarefying lunar gas to

be olivine with an atomic weight of 21, an average atomic number of 10.5

and we shall assume, quite arbitrarily, an effective charge for a typical

particle of unity. For such a material, the rms velocity as a function of

temperature is given by

Pi'==,3,.5 x /0 7-"" c 1sec.

We may take the appropriate velocities for various temperatures and

calculate the Larmor radius, rl, corresponding to these velocities in the

233
unperturbed solar magnetic field. These data are shown in Table II.

Table II

Temperature, *K RMS Velocity for Larmor Radius

Olivine for Olivine

v (kmn/sec) r 1 (cm)

104 3.45 3.4 x 10 6

105 11.5 11.5 x 106

106 34.0 3.4 x 107

1017 15.0 11.5 x 107

108 340.0 3.4 x 108

Since we have assumed a radial solar magnetic field to be the only one

present in this exploratory calculation, we may compute the transit time for

a typical particle moving in the direction of the sun to the position in this

radial field where mirroring will c-ccur. In general, the field at the mirror

point Bm is given by

_ /

Bi is the field at the point of injection and 6i is the angle of injection. Since

our magnetic field goes as i/r2 this expression is exact rather than dependent

upon adiabatic invariance as shown as early as 1896 by Poincare who

calculated trajectories in a monopole field. We may immediately write the

mirror radius in terms of the injection radius as

1 4 = -i 04

Taking the injection radius to be one astronomical unit and considering the

3. 4
particle injected at 60 degrees, one finds that the mean length of the trajectory

to the mirror point is approximately 2 x 1012 cm. We use a particle injected

at 60 degrees as a typical case since contained within a cone of this angle will

be one-half of all the particles, assuming that the injection is isotropic.

We may obtain a lower bound to the time requi ed,for travel to the

mirror point by using the initial velocity along the solar radius. A more

detailed calculation would consider the transfer of energy from transverse

to radial components but, as will be seen, this lower bound calculation is

completely adequate to establish the point we wish to make. In general, a

lower bound to the mean time to the mirror point is given by

and if we set 0 equal to 60 degrees and take a temperature of the order of

105 °K, we find this time is of the order of 40 days at a minimum. Now this

is to be compared with times req'.ired for other aspects of the interplanetary

environment to have their effect on this single particle. In particular, the

outward streaming solar plasma electrons will be de-celerated in the

rarefying lunar cloud and set up electric fields which will drag on the clouds

travelling toward the sun in precisely the same way that drag is produced on

cometary tails. The ratio of solar gravity to this drag has been computed

for the cometary case by various investigators. In particular, Kiepenheuer 2 0

gives for this drag ratio, p., the expression

,6x/O 6= ',

Z35
where n is the particle density for the solar stream and v is the relative

velocity. Although our materials are somewhat dissimilar, we may use this

expression to compute to order of magnitude the time required for the

relative velocity of the two systems to change from v. to vf. This time is

simple

where g. is the solar acceleration.

If the change in relative velocity, AV, is small this may be written as

while if the change in velocity, AV,, vo, this expression becomes

Now if we wish to stop a lunar particle moving with an initial velocity

corresponding, let us say, v to rms velocity at a temperature 10 5 °K, then AV,

the change for relative velocity is small and for solar stream conditions

corresponding to i± = 100, we find that the stopping time is of the order of

104 to 105 seconds. If one is dealing with an intense solar stream so that

ýL = 1000, this is reduced to 103 to 10 seconds. If, on the other hand, we

wish to actually turn the particle which initially started toward the sun and

have it attain the velocity of the solar plasma stream, the times required

are of the order of 105 to 106 seconds for 4± = 100 and proportionately less

for conditions when ýL = 1000. We might note here that at one astronomical

unit gs, the acceleration due to solar gravity, is equal to

236;C ec.

236
Therefore, for ýL 100, the plasma acceleration is of the order of 67 cm/sec

and for p. = 1000 the plasma acceleration is of the order of 670 cm/sec.

These figures are to be compared to accelerations due to lunar gravity of the

order of 167 cm/sec at the surface of the moon. Thus, if p. = 1000, lunar

gravity will be small from the beginning, while if 1. =100, the effect of lunar

gravitation will be small after three or four lunar radii have been traversed

by the escaping particles. This woul.d take only a few minutes at the velocities

under consideration. In any case, it appears thiat the perturbing influence of

collisions for the outward streaming solar gaf, will completely override any

effects directly due to the solar magnetic fieid so that attempts to calculate

single particle orbits and mirroring points ~n the absence of collisions with

the solar streams are pointless.

In passing we might note that the effects we have been treating :have

also been suggested as active in reducing the normal steady-state lunar

atmosphere. This possibility is mentioned among others by Kozyrev. 21The

Russians have also suggested that a lunar cloud, produced by artificial means,

could aid in soft landings on the moon. They suggest tests to determine

22 settling times using special rockets to produce the clouds. Such ideas

might be worth further thought in the present context.

It is of some interest to consider the time required for ionization of a

neutral particle originating in the detonation by electromagnetic radiation from

the quiet sun. If we take a cross section for photo ionization of the order of

5 x 10- 8 cm 2 and consider photons of 10 electron volts as effective with this

237
cross section, we find tha~t the time required for ionization is of the order

of 10 t~o 106 seconds by this process. In this calculation, a flux of

6 erg/cm/sec is assumed as indicated by the measurements of Byram et al. 2

This ionization process is, of course, only one of a number of mechanisms

which will be operating. The mean time to ionization by solar protons, however,

assuming a cross section of 10- 18 cm 2 with a velocity of 1000 Km/sec. and a

density of 10 3 particles/cm 3is one order of magnitude longer than that

required for UV ionization. From such calculations as these, it appears that

single particles which are neutral at the beginning of the process might remain

neutral long enough to travel of the order of the earth-moon distance without

acquiring a charge. Before such a conclusion can be definitely established,

it would be necessary, however, to consider other mechanisms than those

discussed above including stripping reactions, charge exchange and other

possibilities.

If single particle calculations were to be taken seriously, we could, in

principle, calculate the shape of the cloud of lunar material released by the

detonation and from such calculations decide how visible such a cloud would

be and for how long. In fact, taking a particle injected at an angle e as

representative of the behavior of the entire system, one may readily show

that the volume enclosed by the orbit of such a particle in a time t is given

by the expression
If one assumes that this volume is then filled with lunar debris, one may

make calculations on the question of visibility. Taking a temperature of

105lK, taking 0 as 60 and using a time of 105 seconds after the burst, one

finds the volume, V, to be of the order of 10z cm 3 . If we assume 106 kilograms

of matter have been injected as a result of the bomb x-ray pulse and uniformly

distributed in this volume, we find a particle density of the order of

106 particles/cm3 which is perhaps two to three orders of magnitude larger

than the density normally present in interplanetary space. If a cloud is

singly ionized we may compute a lower bound to the brightness by considering

only Thompson scattering. The number of electrons along the diameter of

14

the cloud is about 10 so that the system is optically thin and one finds a

scattered solar flux of the order of 107 photons/cmZ/sec, which is a

significantly high number and is equivalent to 5 x 10-13 lumens/cm-2 /sec.

This would be visible with a 16 x telescope with one inch aperture. To this

scattered solar flux must be added orher scattered radiation and especially

resonance fluorescence light.

It should be mentioned that many observational techniques on the bomb

cloud may be suggested by drawing an analogy with work on the solar corona.

Possibilities which come immediately to mind are:

(1) Observations on the scattered Fraunhofer lines of the sun. The

spread in such lines is proportional to V of the bomb

cloud electrons so interesting temperature histories could be

obtained. Severe broading occurs at I05-K.

(2) Doppler shifts in lines. Such data might permit detection of

ordered motions in the cloud.

(3) Polarization measurements.

23QI
Parenthetically, we may calculate the solar radiation pressure on the

assumption of pure Thompson scattering. At one astronomical unit, per

electron, the radiation pressure from radiation h is given by

7' C cz2' 0- 3 ( W,- 21-

P at I A. U. is equal to 3 x 10-2-9 dynes. The force of solar gravity for mass

21 particles is 2 x 10-23 dynes and since polarization forces keep the plasma

acting as one body, it is clear that gravitational effects overwhelm light

pressure effects and one is left with solar stream and magnetic interactions as

the dominant factors. It becomes clearly necessary then to reconsider all

of these qualitative estimates in a more realistic way, taking into account

the magnetohydrodynamics of the situation. The degree to which such a

treatment will differ from the single particle trajectory picture may be

readily indicated by a trivial calculation of the spherical volume of the

rarefying lunar vapor when the magnetic pressure from the solar field equals

the material pressure. Although a sphere is assumed, it is evident that

expansion will be anisotropic and probably a "sausage" would be a more

realistic model. in our illustrative case of a 10 5 .K gas and a mass 106 kilograms,

the radius computed on this basis is of the order of 1010 cm. On the other

hand, such an estimate as this ignores the presence of the already existing

24

interplanetary plasma. For a system volume corresponding to a radius

10

10 cm, the mass of lunar material results in a particle density of only

10 lunar particles/cm3 whereas the background gas might be two orders of

Z40
magnitude higher than this. It is apparent that engulfing of the normally

present interplanetary medium will reduce the overall radius of the cloud

and change its composition as well. In this process various sorts of hydromagnetic instabilities could also result. It may be, therefore, that the

picture developed on a single particle model is not quite as far off dimrensionally

as one might first assume. Clearly, however, the phenomenology should be

treated in more detail before any firm conclusions can be drawn.

An individual aspect of the behavior of the lunar plasma whicl; deserves

attention and which can be treated in a somewhat realistic way is discussed

in an appendix to this chapter. It is concerned with production of relativistic

electrons as a result of plasma interaction with inhomogeneous magnetic

fields by mechanisms other than the usual Fermi acceleration. If such a

mechanism is operating, it may lead to interesting observable effects not

only for detonations near the moon but also elsewhere in space.

Section Four

Influence of Solar Plasrnas on Experimental Apparatus

During the course of the present considerations as well as in many

other investigations of this general topic, the need has arisen for optical

tracking aids and for other experimental structures to be erected in space

or on the lunar surface possessing large surface area and low total mass.

The desire for such structures is discussed in the chapter on optical

problems in this report as well as elsewhere. With these types of structures

in mind, it is of interest to compare the force per unit area exerted on a
material body by solar plasma streams with that produced by light pressure.

The latter, in general, is given by the sum of rnementa carried by incident

solar radiation minus the parallel component of reflected or absorbed and

subsequently re-radiated flux plus the anti-.parallel component of momentum

from re-radiated f].ux. if we assume a perfect reflector, no re-radiation

can occur, and the force per unit area at I A. U. reaches a maximum value

5 2 of about 9 x 10- dynes/cm

If we assume a solar plasma containing let us say 600 particles/cm 3

and travelling at an average velocity of 1000 Kmn/sec we obtain a force of

0-5 sc2

10 dynes/cm if the beam is simply stopped in the material. For an

active sun during a severe storm, with stream densities of 105 particles/cm 3

and velocities of, say, 2000 Km/sec, 2 we obtain 6. 7 x 10-3 dynes/cm . Thus,

for quiet conditions the plasma produces 0. 11 times the maximum light

pressure, but during a storm, it may exert perhaps 75 times the solar

radiation pressure on a perfect retlect-or at I A.U. from the sun.

The very difficult problem of locating and tracking a small instrument

package in the vicinity of the moon, for example, has led to the very

interesting suggestion that highly reflectiveh balloons be periodically

discharged from the package. 25 According to this suggestion, dispersion of

these balloons by light pressure would theo produce an advancing line of

objects of high. visibility. If such a systmn) were indeed employed, it would

be of interest to attempt to observe additional accelerations above the

light pressure value which could be ascribed to the solar plasma. Conceivably,

1-11,
some information on the fluctuations in momentum transfer due to changes in

solar plasma velocities and densities could also be obtained from such

observations, No telemetry of data would be required. Consideration should,

however, be given to possible destruction of the balloons or their reflective

coatings by the plasma. This will be discussea more fully in the next pages

since these effects are also germane to questions of long-lived passive

communications reflector satellites and durability of balloon m~arkers 26

for the lunar surface assuming the absence of a lunar magnetic field 2 7 and

to power generation equipment using thin films.

Before leaving the subject of the forces exerted by solar plasmas

mention may be made of an apparent revival of interest in the idea of using

light pressure for propulsion. Originally suggested in the literature of

science -f iction, it has received attention in the serious lay press?9and in

the American Rocket Society Journal. 30The practicality of these ideas has

already been questioned on other grounds by Greenwood 31and there is no

need to repeat his criticisms here. To the list of problems may be added

the -thought that in the presence of a strong solar plasma stream, the forces

on the shrouds of a "solar sail" will be orders of magnitude greater than the

results given by Garwin, for example. The latter author, in arriving at his

conclusion that light pressure propulsion is practical, proposes the use of

commercially available metallized plastic film of 0. 1 mil thickness and

suggests, as an improved design, that film of thickness 2 x 10- cm be used.

Assuming such a structure could be built, if it were struck by a solar plasma

243
stream, considerations to follow show that its function might be seriously

impaired In a short time.

When high velocity ions or atoms impinge on a solid surface, momentum

transfer processes or, in some cases, chemical processes lead to the

ejection or sputtering of atoms from the surface. For the case of physical

sputtering of metals, the threshold energy Vo for particles of atomic weight

M impinging normal to a surface of atomic weight M., is given by

where 0 is the heat of sublimation of the surface material in kcal/mol and

W is the bulk sound velocity for the material in cm/sec.

This semi-empirical expression was obtained by Wehner 3 2 and fits

experimental observations obtained with thick samples at room temperature

or above. Applying these results to the sputtering of very thin structures or

coatings by the hydrogen-rich solar plasma stream can only give very

approximate results because of: (1) the possibility of chemical sputtering

through metal hydride formation which would require much lower threshold

energies, (2) the difference between thin film properties and bulk mechanical

properties which can change the kinematics of momentum transfer -

empirically, this might be accounted for by changes in 0 and W, and (3)

differences between ionized and neutral atom sputtering mechanisms.33,34

For protons on aluminum, the calculated threshold for perpendicular

incidence, using 0 = 75 kcal/mol and W = 5. 1 x 105 cm/sec, is Vo = 560 electron

244
volts. The energy of solar protons may be readily computed and, for

1000 Km/sec streams, is •-.'5100 electron volts. Thus, even for considerably

slower streams than suggested by some of the observations, sputtering

thresholds at normal incidence are likely to be exceeded by large margins.

The yield of sputtered atoms per incident particle is a more difficult

subjcct and observations as well as theoretical predictions vary widely,

Depending on the circumstances, yields ranging from 0.05 to well over 1.0

might be appropriate for ou- situation on the basis of the measurements

35

reported by Weiss and by Wehner and the calculations of Whipple. Still

higher yields would presumably be observed at other than normal incidence;

36

Goldman and Simon suggest a secant 0 dependence hi the theoretically

simple case of high energy sputtering with the yield going with energy as

lnV/V. In view of the uncertainties involved, we shall assume a sputtering

yield of unity and note that the destructive effects to be computed can be

readily scaled to other values.

Consider now a reflective structure consisting of metallized plastic.

In order to achieve high visible opacity, a metal thickness of the order of

300 A will be required which, in the case of aluminum, would weigh about

52 17 2

10- grams/cm and contain about 2 x 10 atoms/cm . Supporting the

metal coating would be a plastic film which, in the case of marker balloons

or focusing collectors, might be 0. 1 mil to 0. 25 mil thick and which would

weigh between 25 x 10-5 grams/cm2 and 6U x 10-5 grams/cm 2. Thus,

metal thicknesses in excess of 13 times the assumed value (e.g. 3300 A

I A I
of aluminum) begin to cost heavily in payload for fixed structural area. For

light pressure propulsion, where plastic film thicknesses of 2 x 10- 5 cm have

30 0 been proposed even the 300 A coating adds one-third to the mass per unit

area.

Comnplete stripping of a coating by sputtering would occur in a time t

given by

where N is Avogadro's number

L is coaling thickness

cr- isa spu ;tering yield assumed independent of L but averaged over

angLe and weighted according to the incident velocity distribution

M is coating atomic weight and d is density

<n v>lsa the solar flux averaged over the exposure time

Optical properties will, of course, begin to change well before complete

removal is effected. This expression does, however, ignore atoms removed

from one part of the structure and deposited on another region either because

of the physical design of the structure or by virtue of image charge forces.

Most sputtered particles are neutral. We also ignore atoms ejected in the

forward direction through the structure. Mass losses or atomic displacements

from this latter mechanism could be quite important especially for very thin

films.

The time required for solar protons to destroy a 300 A coating, on the

basis of an average yield of unity, a density of 600 particles/rm 3and a

2 46
velocity of 1000 Km/sec would be less than one month of exposure. For

densities and velocities corresponding to an intense storm

(v = 1500 Km/sec and n = 10 5 /cm 3 ) the coating would be completely removed

in about 104 seconds. This time is within an order of magnitude of that

required for an average beam from a single solar event to pass the earth at

a velocity of 1000 Km/sec. A beam length in space of about 1011 cm is

suggested by Kiepenheuer 3 7 to account for the time dependence of geomagnetic

effects while Uns6ld and Chapman give a beam length of 1.2 x 1012 cm. Thus,

depending on how literally one takes the assumptions, a single encounter with

a beam ejected from an active sun could conceivably destroy the reflective

coating. Scaling to other assumptions about proton densities,. velocities,

and yields is direct and obvious.

We turn now to an aspect of the solar plasma usually ignored - the

presence of elements heavier than hydrogen. Except for Uns6ld ane. Chapman's

attention to possible Ca II content of a stream, a plasma consisting purely of

protons and electrons is generally assumed. However, since the corpuscular

beams appear to be merely segments of the solar corona blown out bodily,

-one should expect both helium and higher Z elements to be present. If one

assumes no fractionation occurs during acceleration, an assumption which

might be mtore applicable to individual streams from an active sun than to

quiet conditions, it would be reasonable to expect a plasma composition

similar to that of the corona itself, by weight roughly 75 per cent hydrogen,

38

23 per cent heliumn and, Z Fer cent :C',y elements. For the l.st v.- ma7

? !.7
39

take an average atomic weight of around 3Z. In the plasma a population ratio,

H:He:Heavy, of about 75:6:0.06 might then be expected. Charged heavy

species would travel at the same velocity as the general proton stream

because of polarization fields and would therefore possess correspondingly

higher energies and momenta. From the viewpoint of any impulse delivered

to a structure, the influence of all but the heliurm is negligible (and, in fact,

is partially taken into account by the methods used to calculate stream

properties from observations in the first place). From the viewpoint of

sputtering, however, the presence of these components could lead to

appreciable effects. In comparison to protons, momentum transfer from

such particles to atoms of a surface is more efficient, differences

between charged and neutral components not so marked., and a variety of

chemical sputtering mechanisms possible. For example, the work of

Weiss et. al. for silver shows a sputtering yield for He+ higher than for

H+ by a factor of about nine in the 10 key region, This al.one would make

the sputtering by solar He+ about equal to that by solar protons.

The heavy component in a 5 kev proton stream would have an average

energy in the vicinity of 160 kev while the sputtering threshold for such

particles incident normally on an Al surface would drop to the order of

94 electron volts because of higher momentum transfer efficiency. it might

be noted that if such particles were present even in the form of a cold

stationary gas, perhaps the remanents of previous solar streams, and the

structure uLnder consideration was moving along with the earth (but outside

248
the magnetic shielding limit), the equivalent energy of the gas Impinging on

the surface would be about 180 ev - well above the sputtering threshold.

Similar considerations to the above may be made concerning the

longevity of thin coatings of prescribed emissivity applied for purposes of

temperature regulation of extra-terrestrial structures.

If the surface of the plastic film itself, rather than an overlying metal

coating, were exposed to the solar plasma, radiation damage effects over

and above those caused by solar ultra-violet and x-ray emission are to be

expected. Hydrogen evolution jnading to charring and carbonization at

exposures of rrore than 1010 Rad (1 Rad= 100 ergs/gram) should occur. If

the reflecting film were behind the plastic, a marked crop in albedo would

presumably precede final destruction by some sort of sputtering away of the

carbon skeleton of the polymer.

Radiation damage produced by relatively slow, heavy particles of

the kind present in solar plasmas has not been extensively studied. As a

first approximation, we shall assume the dose to be delivered uniformly

over the range of the incident particles. This is justified because multiple

scattering and similar effects will smear any strong dependence on details

of the primary energy loss mechanisms. Since hydrogen evolution results

from molecula>" excitation and ionization, direct conversion from energy loss

to chemically effective dosage should be permissible down to a limit below

which elastic collisions predominate as a result of the incident particle

velocity dropping below the pertinent orbital electron velocities. Seitz.40

2419
suggests, for this limit, the point at which the incident particle velocity is

that of an electron with about one-eighth to one-quarter of the required

excitation energy Et, If Et^ 4 ev, the proton energy required for excitation

would be 1 to 2 key. For the heavy element component, the lower limit would

be around 30 to 60 key. In both cases, the velocities associated with the

solar plasma are well above the required limits. For a rough estimate we

shall compute the range of the particles and then convert the energy loss

sustained up to these limits to Rads.

41

For solar protons, the range measurernents of Cook at.l. may be

used along with a range-energy relation of the form R = kE 2 / 3 to obtain a

range ofA-'l0-5 grams/cm for a velocity of 1000 Km/sec. For a density of

600 particles/cm3 the dose would be about 5 x 105 Rads/sec. Carbonization

requires of the order of 1010 Rads and hence would occur in about

2 x 10 4 seconds. For a beam from an active sun, the time required would

be about 100 seconds or less than the exposure time provided by a single

major event.

For the heavy elements disuussed earlier, the range may be computed

from the expression 4 2

where Z , A 1 and Z , A2 are th, ,,niic number and weight of the absorbee

a;-d stream particles respectivly P, is stream energy in key.

250
The range of this component in plastics is thus calculated to be

5 to 10 x 10-5 grams/crm2 for velocities presumed appropriate to a quiet sun.

For storm conditions, with velocities of 1500 Km/sec or more, the range of

the particles would exceed 25 x 10" grams/cm 2 allowing them to completely

penetrate a 0. 1 mil structure. The dose delivered to these thicknesses of

material is of the order of 3500 Rads/sec for the quiet sun, assuming

8 x 10-4 heavy particles per proton., and might rise to perhaps 5 x 10 5 Rads/sec

due to an intense beam. The corresponding time to deliver 1010 Rads from

the heavy component alone is aboint 40 days in the former case. The dosage

from the heavy component is naturally small compared to the proton

component but is effective over larger thicknesses. It does not require any

sputtering away for total penetration of sufficiently thin sections.

The detrimental effect of solar plasmas on the performance of various

thin, lightweight structures which might be erected in space has been shown

to be potentially serious. The precise magnitude of the problem cannot be

established with certainty, but assumptions which appear reasonable in the

light of present knowledge lead either to very low durability or to high

payload penaJties. For certain effects, even a reduction of plasma density

by one or more orders of magnitude, as a result of more complete data

collected in the future, would still imply a considerable problem.

251
REFERENCES

1. Biermann, L_, Za. f. Ap., 29, 274 (1951).

2. Biermann, L,, Z, Naturforsch., 7a, 1Z7 (1952),

3. Biermann, L., Observatory, 77, 109 (1957).

4. Untiold and Chapman, Observatory, 69, 219 (1949).

5, Hey, Parsons and Phillips, MNRAS, 128, 35,i (1948).

6. Behr, A. and Siedentopf, H. , Zs. f. Ap., 32, 32 (1953).

7. Kiepenheuer, K. 0., The Sun, G. P. Kuip-r, ed. Univ, of Chi. Press,

p. 440 (1953).

8. Kuiper, G. P., Private Communication, December, 1958.

9. See particularly Parker, E. N., Phys. )f Fluids, 1, 171 (1958). AlsD

Astrophysical Journal, 128, 664 (1958), and Phys. Rev., 110, 1445 (1958).

10. Vshekhsvaytskiy, S. K. et. al. , "Fizika Solnechnykh Korpuskulyarnukh

Potokov i ikh Vozkeystviye na Verkhn)uyu Atmosferu Zemli" (Physics of

Corpuscular Streams and Their Effec'. on the Upper Atmosphere of the

Earth), pp. 51-57, 57-58, and 76-86 (1957). Quoted from Referativnyy

Zhurnal - Astronomiya i Geodesiya, No. 7, July, 1958, Abstract No. 4459

by Soviet Bloc IGY Information, U. S. Dept. of Commerce PB 131632-32,

p. 14, September 19, 1958.

11. Soviet Bloc IGY Information, U. S. Dept. of Commerce PB 131632-51,

p. 15, Jan. 30, 1959.

12. Block, L., Arkiv for Fysik, 14, pp. 153-193 (1958).

13. Opik, E. J. , Irish Astronomical Journal, 4, 84 (1956).

1 . Bex'fŽtrahl, T., AFSWC Meeting, Feb. 21, 1959.

15. See atnong others, Wood, J. A., Astrophysical Journal, 127, 241 (L952ý.

He suggests a yi.ld of 0.01.

252
16. Urey, H. C., "Primary and Secondary Objects" delivered at the Symposium

on Problems in Space Exploration, Washington, D. C. , April 30, 1959.

Also private communication.

17. Reiffel, L., to be published.

18. Babcock and Babcock, Private Communication to L. Reiffel via E. N. Parker

19. Hoyle, Phys. Rev. 104, Z69 (1956).

20. Kiepenheuer, H. 0., The Sun, G. P. Kuiper, ed. Univ. of Chi. Press.

p. 439 (1953).

21. Kozyrev, N. A., quoted from earlier work in Information on Soviet Bloc

IGY Cooperation, U. S. Dept. of Agriculture PB 131632-63, p. 3,

April 24, 1959.

2Z. Pakrovskiy, G. F. and Molodezhi, T., quoted in Information on Soviet Bloc

IGY Cooperation, p. 3, November, 1958.

23. Byram, et. al., IGY Rocket Report Series No. 1, Nat. Acad. Sci., p. 190,

July 30, 1958.

24. This point was made by Maj. L. Allen during discussion at the AFSWC

Meeting on this subject in February 1959.

25. Johnson, M. H., Denver Astronautics Symposium, April 28, 1958.

26. Reiffel, L. and Kapany, N. S., to be published.

RAND Memorandum RM-1900, ASTIA No. AD 133032, May 27, 1957.

27. Recent Russian observations on gaseous emission from the moon have been

interpreted by D. H. Menzel of Harvard Observatory as giving evidence that

the solar plasma can indeed reach the lunar surface - private communication

February 26, 1959. There are a number of widely accepted reasons to

expect a very small lunar magnetic field as discussed previously.

28. The author is indebted to a number of his colleagues for general information

on the history of this idea in Science Fiction and to the Editor of Astounding

Science Fiction for providing the most pertinent reference entitled

"Clipper Ships of Space" by Russell Saunderý, Astounding Science Fiction,

47, 136 (1951). In spite of the nature of the magazine, it is a detailed

technical evaluation.

Z 53
29. Cotter, T. P., Time, 72, 35 (1958). See also Tsu, T. C., Industrial

Laboratories, 16 (1958).

30. Garwin, R. L., Jet Propulsion, 28, 188 (1.958). Entitled "Solar-Sailing -

A Practical Me thod of Propulsion Within the Solar System," this article

was apparently written in unawareness of the earlier history of the idea.

31. Greenwood, S. W. , Jet Propulsion, 28, 765 (1958).

32. Wehner, G. K. , Advances in Electronics and Electron Physics, Academic

Press, New York, p. 289 (1955).

33. Moore, et. al., J. Chem. Phys., 29, 3 (1958).

34. Weiss, et. al., J. Chem. Phys. , 21, 7 (1958).

35. Whipple, F. L. , Astrophysical Journal, 121, 755 (1955). See also

comments by Wood, J. A. , Astrophysical Journal, 127, 241 (1958).

36. Goldman, D. T. and Simon, A., Phys. Rev., 111, 383 (1958).

See also Henschke, E. B., Phys. Rev., 106, 737 (1957).

37. Kiepenheuer, K. 0., or. cit., p. 449.

38. Stromgren, The Sun, p. 79 ff.

39. Struve, 0., Stellar Evolution, Princeton Univ. Press, 62 (1950).

40. Seitz, F., Disc. Faraday Soc., 5, 277 (1949). Also Seitz and Koehler in

Solid State Physics, Academic Press, New York, 347 (1958).

41. Cook, Jones, and Jorgensen, Phys. Rev., 91, 1417 (1958).

42. Schmitt and Sharp, Phys. Rev. Letters, 1, 445 (1956).
Appendix I

ACCELERATION OF ELECTRONS IN MIRRORING PLASMAS
Appendix I

ACCELERATION OF ELECTRONS IN MIRRORING PLASMAS

In this appendix, we wish to describe briefly a possible mechanism for

the production of fast electrons, in the mev range of energy, from a nuclear

burst and specifically not involving nuclear beta decay. The existence of a

very simple and general mechanism for generating fast electrons, which

has remained unnoted in much of the weapons effects literature, but which

has been described qualitatively for the case of cosmic rays by the Russian

scientist Veksler, I is the basis for this discussion. Veksler has suggested

that relativistic electrons in cosmic space can be generated by thi motion of

a small neutral cloud of ionized plasma in an inhomogeneous magnetic field.

We shall repeat here the essentials of his argument and then apply the ideas

to the behavior of a nuclear bomb case plasma.

Consider a small cloud of neutral plasma moving as an entity with a

velocity vo. For simplicity, let us assume that the inhonmogeneous field has

a symmetry axis and the neutral cloud is moving along this axis which we

will denote by z. W'hen the cloud enters the field, the radial component of

the magnetic vector s..,Ljects the electrons and ions to an equal, but

oppositely directed, Lorentz force. Under this force the particles are

accelerated in the plane perpendicular to the motion of the cloud. The

resulting currc~its cause the clou'd b,- Loeconme polarized since the resulting

de-celciating force acting on electroi-s is greater than that acting on ions

Z56
by the ratio of the masses. The polarization field binds the electrons to the

ions and the plasma as a whole is de-celerated and, during the process,

energy is extracted from the iona by the electrons. This process continues

until the forward motion of the ions is stopped or reverses and the entire

plasma rebounds from the magnetic mirror.

Following Veksler, aince the forces of polarization which arias will

not allow the ions to break away from the electrons, we have, for anytime,

the equations

From which it follows that:

where v6i and v~e are the mean ion and electron velocities in the plane

perpendicular to the velocity vector of the cloud as a whole, and Hv is the

radial magnetic field component. From this, it follows that when the forward

motion of the plasma has stopped, the kinetic erergy of the ions is mnuch

smaller than the kinetic energy of the electrons. Thý kinetic energy of the

ions is given by

Nhvh 1.-rrp1ie• that the electron energy will be

Z57
since the ýadial kinetic energy of the ions is negligible and the cloud is

essentially stopped. If we define -y by the equation

and we ha)-vh the energy of the electrons as

in which cade the energy of the electron m3y be vrtAite9

neglecting sihall terms, Thus, an average energy of each electron will be

We -% MO C41-J~

Now let Us assume that the bomb casa in a naclfear dwOtnation has an

average atomic weight of approximately 60. It.iAlknown-from various

calculations that the case disassembles w.ith a. valoceitý of the order of

Z to 3 x 108 cmYli~ec. 'Parenthetically, it might.,b, MpFnt•o•ed hat'Argo et.a&.

have caiott'lated that the outer portion of the cafe:!aay attain velocities of

the ordetrtof-4 x 10 8 cm/sec due to radiation pressure and secondarily to

hydrodyzaThics. Under theme circumstances, y, Ain the expressions above,

is approxmaintely seven and the average energy of the a1'O.ztron in the

plasma ap it is stoppedby the mirror field reachep appr ectna'tely 3 may,

it is interesting to note that the fraction of the .hoxob yield gbirig Into case

motion ma-y thus, in principle, be converted into a good iourae di high

speed electrons comparable to those released by high energy fission product

258
decay but appearing over a much shorter time. Furthermore, the influence

of the magnetic field. before mirrcring occurs might well keep the source of

fast electrons fairly localized even though the burst is some distance away.

Whether measurable effects from a space or lunar burst due to this

mechanism can be observed remains to be explored. However, it would

appear that some of the high altitude, aad especially the ARGUS series of

nuclear detonations, might show phenomena w1lich could be interpreted on

the basis of this mechanism. The appropriate data relating to this question

are not available to us at present. Parenthetically it might be mentioned

that if this mechanism does indeed operate successfully, it becomes of

possible interest in connection with certain auroral phenomena3 and also

possibly in the matter of detecting nuclear bursts in space.

It is interesting to note that in the ARGMA Anti-Missile Research

Meeting for April 21-ZZ, 1959, K. M. Watson suggested the salting of

weapons with Boron- 11 to obtain a faster beta ray emission rate that is

produced by oridinary fission product decay. By this means, he suggests

that beta jets could be produced reaching powers of the order of a few hundred

watts. If the mechanism suggested in the present discussion were operable,

such salting might not be necessary to get the effects. Watson also has

suggested that F'ermi acceleration mechani'sms, occurring in turbulent

regions arouncl a burst in space, might produce electrons of the energies of

the order of 100 mev. It seems possible that the efficiency of the present

mechanism might be comparable to the process suggested by Watson.

259
The arguments put forth for the existence of the mirror accelerating

mechanism are certainly not rigorous ones and it may well be that other

factors enter which reduce, in a fundamental way, the effectiveness of the

energy transfer. Then too, even if the arguments are valid, due consideration must be given to energy loss processes, scattering and other complications.

In view of the relative complexity of the phenomenon from an analytical

viewpoint, it might be worthwhile to appeal to laboratory experiment to

establish the existence of the process.
REFERENCES

1. Veksler, V. I., Soviet Physics - Doklady, 3, 84 (1958).

2. Argo, et. al., "Nuclear Explosions in Space for Scientific Purposes,"

The Second Plowshare Symposium on Industrial and Scientific Uses of

Nuclear Explosions, San Francisco, May 13-15, 1959.

3. Reiffel, L., to be published. See also P. Kellogg, Phys. Rev., 108, 1093

(1957).

zI 1
Chapter VIII

ORGANIC MATTER AND THE MOON
Chapter VIII

ORGANIC MATTER AND THE MOON

Since the deposition of an instrumented package on the lunar surface is

implicit in many of the experiments discussed in thiE report as well as being

imminent as a result of other U. S. or Russian activities, there has been considerable recent concern that terrestrial organisms and organic matter,

deposited with the package, may obscure detectioni of possible organisms or

organic matter indigenous to the moon. 12If su(:h a biological contamination

of the moon occurred, it woul~d represent an un7,iaralleled scientific disaster,

eliminating several possibly very fruitful appr.)aches to such problems as the

early history of the solar system, the chemical composition of matter in the

remote past, the origin of life on earth, and the possibility of extraterrestrial life. Because of the moon's unique situation as a large unweathered body

in the middle of the solar system, scientific opportunities lost on the moon

may not be recouped elsewhere. Accordingly, it is of interest to determine

(a) the survival probability of a terrestrial life-form on the moon, and (b)

the possibility that organic matter was produced during the previous history

of the moon, has survived to the present epoch, and could be confused with

the remains of contemporary terrestrial life-forms.

Section One

Survival of TerrestrialOrganism-s-on the Moon

There -seem to be three major hazards to survival of terrestrial life

on the moon - - the temperature variation, corpuscular radiation, and solar

electromagnetic radiation - - which we consider in turn:' The probable absence of oxygen, water and other substances from the moon's surface is not,

2 63"
of course, evidence against survival, particularly of dormant anaerobic microorganisms; but it does preclude the possibility of their reproduction.

Temperatures range from about + 100 C. to about - 150 C. during a

lunar day and night, but since many microorganisms, and especially bacterial spores, can survive temperatures in this range, we neglect the debilitating

effects of the temperature variation.

Cosmic rays, charged particles emitted by the sun, and continuous, and

discrete solar electromagnetic radiation are all incident os, the moon. Whether they arrive at the lunar surface, however, depends on the existence of a

lunar magnetic field and a lunar atmosphere. At the present writing, the

strength of the lunar magnetic field is not known (except perhaps in the U. S. S. R.).

However the mean density of the moon is comparable with terrestrial surface

material; this has always been understood as indicating the absence of an extensive liquid iron core, and presumably the absence of an appreciable lunar

magnetic field as well. On the other hand it is not definitely ruled out that the

field strength is comparable with the terrestrial value. By terrestrial ex3

perience, and from the Stormer theory, energetic charged particles arriving

from great distances would be constrained to strike the surface at high magnetic latitudes; cosmic rays and the solar proton streamn would then be primarily

excluded from a wide band around the lunar magnetic equator.

The work of Biermann on the acceleration of comet tails indicates a flux

i10 -Z -l

of solar protons in the vicinity of the moon of about 5 x U protons cm- sec ,

and a mean particle energy of a few key (v., e. g., 5). Charged particles will

ce excluded from region3 w,., e 6ite mnagnetic energy density is greater than

Ihe particle kinetic ene f V J:. Fcti or the surfacc of the moon, then, the

Xw-•r magnetic lield wl, otoi.et, ,, exceed about 10-* gauss for these solar

?64
proton streams "or wind" to be deflected.

From lunar occultations of cosmic radio sources, it can be estimated

that the lunar atmosphere contains less than 10 molecules above each square

4

centimeter of surface. Ultraviolet absorption cross-sections for all mole-

-16 2

cules likely to be in the lunar atmosphere are generally less than 10 cm

-2

at all wavelengths. Hence the optical depth in the ultraviolet is less than 10 ,

and there is no attenuation of incident Rolar ultraviolet radiation by the lunar

atmosphere. For the solar proton wind, a 1 to 5 key proton has a range of lbu 0-2 mamshr,6 18-2

about 12cm. atmosphere, or, roughly 3 x 10 18/ ýL molecules cm for a

lunar atmosphere of mean molecular weight )x. Consequently, if the lunar

magnetic field itrength is less than about 10-2 gauss, the solar proton stream

strikes the moon's surface with negligible loss of energy due to its passage

through the tenuous lunar atmosphere. The same conclusion applies to the

more energetic cosmic rays.

Now what is the effect of these radiations on terrestrial microorganisms

deposited on the lunar surface? We consider microorganisms because they

8

are known to be much less radiosensitive than other life-forms, at least in

part because there is less which can go wrong in a simple organism than in

a complex one. In addition, the accidental deposition of many microorganisms

on the lunar surface is a much more likely contingency than the accidental

deposition of largre numbers of other life-forms.

In Appendix I, expressions are derived (eqs. 7 and 8) for the time in

which a population of D.1 organisms, having a mean lethal dose, D, for a

0

given radiation, and characteristic dimensions, a, is reduced to N organisms

by radiation of intensity I. In Table I, these lifetimes are tabulated for a

number of values of N/N and a. The intensities are those appropriate to

0

265
the lunar surface for negligible atmosphere and magnetic field strength, and

so are equally appropriate to interplanetary space in the vicinity of the earthmoon system. Conisequently the derived lifetimes are also those of an unprotected microorganism in free space, and so have a bearing on the panspermia

or cosmozoa hypothesis (v. , e. g., 1, 22). The X-ray emission in Table I is

7

taken from a theoretical study of the solar corona and is consistent with

rocket observations at quiet sun; the continuous uvintensities are computed

from an integration of the Planck equation for appropriate ultraviolet blackbody temperatures; and the cosmic ray flux is adopted from the flux inferred

to exist at the top of the earth's atmosphere.

For a given organism, the mean lethal dose in roentgens is approximately invariant, under the same environmental conditions, for all ionizing

radiation, corpuscular and electromagnetic. Data are not available however

for the mean lethal dose for the relatively slow particles in the kilovolt solar

streams. For the larger organisms these streams will destroy surface structures rather than irradiate the bulk of the organism. Such a situation might

lead to marked changes in the mean lethal dose. It is difficult to know the

direction of change. Viruses chaxacteristically lie in the range D = 105 to

106 r; protozoa generally have the same range. 8,11Bacteria usually have

3 4 somewhat lower mean lethal doses, 10 to 10 r for E. coli, for example, and

4 5 12

104 to 105 r for the spores of B. mesentericus and A. !L'er. However,

there has been no systematic search for radioresistant microorganisms, and

it is possible that microorganisms having mean lethal. doses as high at 107 r

exist. In addition, D in general has some functional dependence upon such

factors as the temperature, the oxygen tension, the time interval in which

the killing dose is applied, and the presence of an external aqueous medium.

266
The dependence is in different directions in different organisms, and the interaction of the various effects is quite complex; but the resulting variation

in D is rarely as great as a factor of ten. Considering all these points, then,

it appears that a conservative estimate for an average mean lethal dose due

to ionizing radiation is 107 r.

For the non-ionizing ultraviolet radiation, D has a strong functional

dependence on wavelength, corresponding to the wavelength variation of molecular absorption cross-sections. The.tre Is an absorption maximum at roughly

N 2600 due to the biochemically ubiquitous purines and pyrimidines, and

another, more pronounced, maximnumn shortward of 'A. 2300, due to simple

diatomic functional groups, such as N-H. Ultraviolet mean lethal doses are

-2

given in ergs cm , and are generally measured at A 2537. To obtain a mean

value of D appropriate for a wide range of wavelengths we must know the

wavelength variation of D. For common strains of E. coli, for example,

5 - 2 4-2 D( & 3000) = 10 ergs cm , D( ý. 2537) = 104 ergs cm , and D( )\ Z300)

3 . - 2 12 10 ergs cm. . Considering the decrease of D shortward of 7. 2300, a

conservative (i. e. , upper limit) mean value of D for the wavelength region

7\ 3000 to 7\ 2000 appears to be the value at 7j, 2537; this should be roughly

applicable for an ultraviolet black-body spectrum with a Wien peak longward

of - 3000. The mean lethal dose at Y\ 2537 for the more radioresistant bacteria, such as B. subtilis spores, Sarcina lutea. and the B/r strain of E.

5 -Z 12

coli, are approximately 10 ergs cm- . An unusual case is the protozoon

Paramecium multimiicronucleatum, n for which D( A 2537) = 106 crgs cm-2 .1

Considering, finally, the environmental dependences of D mentioned in the

preceding paragraph, and the possibility of undiscovered microorganisms of

extreme radioresistance, we adopt ,,s a mean value of D for ultraviolet

',', 7
radiation in the region k 3000 to X2000, D = 107 ergs cm-2. For the region

shortward of A2000, D is certainly less than 106 ergs cm-2.

Where the computed lifetimes are greater than a month, they have been

divided by two - except for the cosmic ray lifetimes - to allow for the lunar

night. For times shorter than a month, continuous solar illumination has

been assumed, but of course, all such times may be as long as a month if the

organism is deposited in a region soon after the terminator has left the region.

A 1 kg. instrumented lunar package may easily contain 1010 microorganisms;1 it is very unlikely that any packages for the immediate future

will contain as many as 1020 microorganisms. Accordingly, we see from

Table I that all microorganisms deposited and exposed to the sun will be

killed by uv in a few hours. Similarly, fully illuminated microorganisms

in cislunar space will also survive only a few hours. Hence the panspermia

hypothesis is untenable for unprotected microorganisms of comparable radiosensitivity to terrestrial microorganisms. ' On the other hand, suppose some

microorganisms somehow survived in space and are deposited in a lunar

crevasse or other depression, always shielded from solar radiation. Then,

killing will be effected only by cosmic radiation. Because of secondary

cascade, cosmic radiation reaches an intensity maximum slightly greater than

the surface value at a depth of about 10 cm on the moon, according to recent

work. 13 It is reduced to 10-1 the surface flux at a depth of about one meter,

and to terrestrial surface values at a depth of a few meters. Hence, microorganisms shielded from the sun, but just beneath the lunar surface will not

be killed by cosmic radiation for several hundred million years; microorganisms

at greater depths will have even longer lifetimes. Similarly, cosmozoa imbedded in, fo

2Q
LA LA rn (71 00 00 LA 4

-4

0 'n fn 0 0 0 0n

LA LA o Ln

1 O00 0 00 -4

oi000 0 0 0

0 0U Ir ~ r~4 fn0; A N N r' 0 o0

v 0n 0n 0 0 0 r- 1 0- Ln D o c, C) 0

o4t

LA xA x k 00~ H 4 4 -4 -4 -4ý U)0 )I

0 4

000

01 N~~- r N 

-444- 09)

Ci) 0 C 0~ 

14

0.4 b j0 U 4 -40 04tj~

-4 00

0 u u 0 k 1

~x440

..- N

(u u '' '

UD

0 0)

(d i g o c l0 (4, > 1 4

0 0O -ý k >sO 0)0

54,(0 td0 0 ;-4. LA40 - N ~~ ~ '4U'- E OJ Cj)~ 
example, a meteorite would have lifetimes comparable to the age of the solar

system, and the panspermia hypothesis cannot be ruled out under these circurmstances.

Now what is the possibility that microorganisms deposited on the moon

will actually be shielded? The nature of the lunar surface is a complex and

14

much debated problem, which need riot be reviewed here. But it is of interest to call attention to a few points. From eclipse temperature measurements

and radio observations it is known that there is a dust covering on the moon,

but estimates of its depth range from millimeters to miles. However, Whlpple1 5

has called attention to the experimental fact that dust, in a vacuum, and irradiated with a corpuscular and electromagnetic flux of approximately solar

composition, will congeal, forming a low-density, semi-porous matrix. If

the lunar surface material has a similar structure, it would appear very possible for microorganisms to be lodged in the interstices of the matrix, in

such positions as to be shielded from the sun's rays at all angles of insolation. Under these conditions, the survival for very great periods of time of

dormant anaerobic microorganisms deposited near the surface would seem

to be a possibility which cannot be neglected. A determination of the microstructue of the moon's surface material is therefore of great importance.

The killing of an organism, of course, does not necessarily involve

its chemical dissociation, and long after death occurs, in an anhydrous

osep1.ic environment, many aspects of the organism's characteristic biocCbtn3fical -tuctuure will be maintained. After long periods of continued

iirradial-i;n, enough bonds would be broken to destroy most of the long-chain

biological polymers such as proteins and nucleic acids. The problem is

compli'7ab d by the existence of radiation protection devices (ca.talase,

270
cytochromes, sulihydryl compounds, photoreactivation mechanisms) in most

contemporary organisms. Because of the Franck-Rabinowitch cage effect,

the collection of dissociated molecules arising from the original organism

would tend to remain in close physical contact. Ionizing radiation is very

much more efficient than non-ionizing radiation in depolymerizing and dissociating organic molecules. Breaking of all hydrogen molecular bonds and

charring occurs at about 10 10r (v., e. g. , 5). Charring by the solar proton

wind occurs in from months to years, depending on the size of the dissociated

organism. If, however, the lunar surface magnetic field exceeds 10-2 gauss

and the proton wind does not penetrate to the surface, it may take as long as

several thousand years for charring to be induced by soft solar X-rays. Thus

the value of the lunar magnetic field strength has great relevance for the question of possible biochemical contamination of the moon.

As dissociation advances, lunar temperature effects would become more

important, small molecules being readily dissociated at 1000 G. For example,

the most thermostable amino acid, alanine, has a thermostability half-life at

i00° C. of approximately 103 years, 16 with most other amino acid's having halflives not less than ten years. Molecules shielded from dissociation by radiation

would be relatively unaffected by lunar temperatures, and if lodged beneath a

few centimeters of insulating lunar surface material, could have very long lifetimes.

Section Two

Production of Organic Matter in the Early History of the Moon

There is reason to believe that the moon, along with other bodies in the

solar system, was formed some 5 to 6 x 109 years ago from the solar nebula,

a vast gas and dust cloud of essentially cosmic distribution of the elements. 17

2 7 1
The contraction timescale for the solar nebula was the Helmholtz-Kelvin

period, approximately 108 years. At the end of this period, the sun approached the main sequence in the :Ilertzspx-ung--Russell diagram, thermonuclear

reactions were initiated, and solar electromagnetic and especially corpuscular radiation dissipated the nebula from around the iorotoplanets and their

atmospheres. The dissipation timescale for the solar nebula is estimated

by Kuiper as between 108 and 109 years. ].8 After taie clearing out of interplanetary space, hot exospheres established in t-e protoplanetary atmospheres

led to efficient evaporation of the planetary envelopes, a process aided by the

long mean free paths in interplanetary space and the low escape velocities

(due to smaller mass/radius raios for the prtoplanets than for the present

planets). The time for the evaporation of the prototerrestrial atmosphere appears to be roughly 108 years. 19

During the events just outlined, chemical compounds and condensates

were raining down on the protoplanetary surfaces, forming the outermost

layers. After the evaporation of the atmospheres of the terrestrial protoplanets, internal heating must have vaporized much of the condensates,

thereby forming secondary atmospheres of similar chemical composition to

the initial protoatmospheres. The present Martian, Venusian and terrestrial

atmospheres are believed to be ultimately of such secondary origin. Similarly, the moon must have possessed a secondary atmosphere at one time, which,

however, since has been lost to space because of the low lunar escape velocity. If not replenished from the interior, a lunar atmosphere will escape to

space in roughly 103 years, as can be conmputed from the work of Spitzer. 20

Hence the lifetime of the secondary lunar atmosphere depended entirely on

the supply rate of gases from the lunar interior. This is difficult to estimate,

27?.
but it is not impossible that extensive lunar vulcanism lasted for 107 or 108

years. Although it is unlikely that the lunar craters are volcanic in origin,

32

other lunar surface features exist which are of undoubted volcanic origin.

We now consider the penetration of solar ultraviolet radiation into the

various gaseous envelopes which surrounded the moon in its early history.

The absorption cross-section of ammonia, the most prominent nitrogencontaining molecule in cold cosmic gases, shortward of ý2600 is greater

than 10 cm . Hence, as long as the mean density of ammonia exceeded

106 molecules cm-3 between the moon and the sun in the solar nebula, solar

uv shortward of ;1 2600 did not reach the lunar vicinity. This ammonia den9 -3

sity correspon(Ls to a hydrogen number density of about 10 molecules cm

for cosmic abundances; i.e., about 10 gm cin . Interplanetary densities

18

of this order were reduced rapidly, and we conclude that during most of

the 108 to 109 years in which the solar nebula was being dissipated, solar uv

shortward of 2, 2600 was reaching the protoatmosphere of the moon. Because the lunar protoatmosphere had not yet begun to escape, due to the

short mean free paths within the solar nebula, the lunar protoatmosphere

remained opaque to solar uv during this period. After the dissipation of the

solar nebula, the lunar protoatmosphere was opaque in the uv for most of

its lifetime. In this same period, the moon must have been situated within

the protoatmosphere of the earth, and so the moon's surface must have been

protected from solar uv by lunar and terrestrial protoatmospheres for almost

108 years. Af-;er the evaporation of these protoatmospheres, apd the origin

of the secondary lunar atmosphere, it is not clear how long the secondary

atmosphere was maintained at sufficient density to absorb all incident solar

radiation shortward of ' 2600. The true time may be anywhere between 103

273
and 10 8 yearsB, depending on the rate of gaseous exhalation from the primitive

lunar interior. But from terrestrial experience, one might expect the larger

value to be nearer to the truth.

The later solar nebula in the vicinity of the moon, and the primary and

the secondary lunar atmospheres, all having cosmic composition, were composed largerly of CH 4 , NH 3H20,with smaller amounts of H 9He, Z

Go, G0 2, A, Ne, and the interaction products of these molecu~les. The effect of solar ultraviolet light (and electric discharges) on such an atmosphere.

is well known; organic molecules of fair complexity (up to molecular weight

-100) are produced efficiently, almost independently of the relative proportions of precursors. Arnino and other organic acids, pyrroles, pyridines,

and simple hydrocarbons Lind their polymers are among the synthesized

21, 22 molecules. The syntheses are in general non-equilibrium processes;

radiation both produces and destroys the organic molecules, but the net

production rate is proportional to the photon flux. In addition, because the

molecular weight of these molecules was greater than the mean molecular

weight of the nebula or atmosphere, they diffused to the surface under the

influence of the lunar gravitational field. The time for such molecules to

diffuse to atmospheric depths where photo -dissociating uv does not penetrate

can be shown to be of the same order as the time between absorptions of

photo -dissociating photons. 23Consequently, with reaction products. being

removed from the system, the quantum yield in the primitive lunar envelopes

must have be en greater than that in contemporary laboratory experiments in

which reaction products are not being removed from the system.

Recently a series of experiments on uv synthesis of organic molecules

which permits quantitative conclusions has been performed by W. Grt in
Bonn. 24 The overall quantum yield, 0, for the production of amino acids

alone from a gas mixture of ethane, ammonia and water is between 104

and 10 -5. The value appears to be approximately independent of wavelength

between -A 2537 and 'A 1470. Because of the rapidly decreasing NH 3 absorp-.

tion cross-section longward of ?\ 2600, radiation of much longer wavelengths

should be synthetically ineffective.

In the primitive lunar envclopcs, methane, not eLhane, was the principal carbon molecule. The quantum yield for the photoproduction of ethane

from methane is about 10-1 at N 1470. 25 Assuming the synthesis of amino

acids from methane, ammonia and water is a wavelength-independent as the

synthesis from ethane, ammonia and water, we conclude that the 0 appropriate to primitive conditions is about a factor of ten less than Groth's

laboratory value. This point should be checked experimentally. Since the

time between collisions is much shorter than the time between absorptions

23

of uv photons in the primitive lunar atmosphere, the differing pressures,

temperatures, and densities should not significantly alter the overall quantum yields. It is difficult to estimate by what factor the overall quantum

yield should be increased to allow for the gravitational diffusion of the synthesized molecules out of the radiation field. Simultaneous irradiation over

the whole range of w'avelengths shortward of J>\2600 should also increase 0.

Provisionally, let us take an overall quantum yield for the photoproduction

of amino acids in the primitive lunar atmosphere or neighboring solar

nebula of 0 = 10-6 between ý, 2600 and \, 1470, remembering that there is an

uncertainty of at least a factor of ten. If we knew the flux of solar radiation between these wavelengths in primitive times, we would be able to

compute the arrival rate of amino acids on the ancient lunar surface.

275
The present solar flux at 'A 26U0 is that of a black-body of temperature

26

about 5000 OK. 6 We are interested in the radiation flux after the sun's

evolutionary track in the Hertzsprung-Rua sell diagram has joined the main

sequence, and the dissipation of the solar nebula has begun. At the juncture

with themain 4equence some 5 x 109 years ago,. the luminosity was about

half a bolometric magnitude less than at present, and the radius about

0.87 R. 0' 10, years0 later, about 4 x 10 years ago, the solar

radius was about 0. 90 RO , while the solar luminosity had increased from

about 0. 69 L to about 0.73 L . 29 We write L and R for the present

solar luminosity and radius. Knowing the luminosities and radii at these

two representative times, the ultraviolet black-body temperature and geometrical dilution factors can be computed, and the radiation flux shortward

of a given wavelength at the two times obtained by integrating the Planck

equation. The ultraviolet temperatures were about the same at the two times

(0. 975 the presernt temperature) as are the dilution factors (about 0. 8 the

present value). The quiet solar ultravolet photon fluxes of wavelength

shortward of A 2600 in the vicinity of the moon at these times is then computed to be Q = 7 x 1014 photons cm" sec -, rougidy the present value.

Assume now that uv radiation of intensity Q falls for t seconds on an opaque,

gaseous envelope surrounding the moon, and produces molecules of molecular weight ý with quantum efficiency 0. Let r be the distance from the

center of the moon such that all molecules of molecular weight produced

at distan'ý2z less that r are gravitationally captured by the moon, whels those

produced at distances greater than r will escape. Tie synthesized mr.Ieculos

w7ill be distributed over a moon of radius R. The mean surface dencity of
deposited material will then be

where NA is Avogadro's number.

Because of the moon's proximity to the more massive earth, much

material produced in the lunar vicinity must nevertheless have been captured

by the earth. We adopt as a minimum value of r, r = R; i. e., we neglect

lunar gravitational capture of molecules produced outside a cylinder of

lunar radius extending from the moon to the sun. This approximation is,

of course, very nearly exact for the secondary lunar atmosphere; but it

gives only minimum values of r for the times of the solar nebula and the

original lunar protoatmo sphere.

In Table 31 we have listed values of O'computed from the above equa014 -2 -I

tion for Q = 7 x 10 photons cm- sec , andi' 100, for various values of

t and 0.

Table II

LUNAR AMINO ACID SURFACE DENSITIES IN gm cm

t-5 10 6 -7 Envelope 0 1 0 16 0-

103 10-2 10-3 10-44

14 I0-1 i0-2. i -3

10 410- 10- 10-3

-1 2 sc'•ondary

10 1 10 100 

lunar

106 10 1 10- 10 710 .101 ztrno spb ere

1.08 103 10 lu-iar prc.toatmosp..

10 10 10 solar nobula

Z77
We see that very considerable amino acid surface densities were produced

from the solar nebula and lunar protoatmosphere (t = 107 to 109 years). However, most of this material rained down while the moon was still being formed,

and therefore must either be buried at great depths below the present lunar

surface, or have been thermally dissociated in the volcanic processes which

evolved the secondary lunar atmosphere. Organic matter produced in the

secondary lunar atmosphere appears to have a much better chance of residing

near the present lunar surface and ha-ng avoided dissociative processes (see

below). Miller21 and Grolh24 find effi,-ient production of other substances

besides amino acids, some with greater quantum yields (especially formic

and acetic acids) and many with lesser quantum yields. The overall deposition of organic matter after the moon's formation may well have exceeded

-2

10 gm cm . This figure is greatly in excess of any possible accretion of

23

cometary or interstellar organic matter. During the time of deposition,

the lunar atmosphere would have inhibited thermo.- and photo-dissociation

of the deposited molecule.

As the secondary lunar atmosphere gradually escaped to space, and replenishment from the interior eventually fell off, the rate of atmospheric

organic synthesis decreased and the penetration of short wavelength radiation

to the surface increased. In addition, the surface temperature gradually rose,

due both to the loss of !he insulating atimosphere, and to the concentration of

radioactive elements towards the surKace as a consequence of the formation

of the lunar mantle. The effect of heat and uv on the molecules described

above is most remarkable. Although the second law of thermodynamics is

obeyed, a large fraction of the molecules, with activation energies supplied,

partake in organic syntheses of a higher order of complexity. Polypeptides
arise from amino acids, hydrocarbon dimers and trimers form long-chain

polymers, and in general very complex organic molecules are constructed

(almost all of which, incidentally, are utilized by and are part of contemporary

22., 30

terrestrial organisms). Finally, because complicated molecules are

more resistant to heat and radiation than are simpler molecules (at least in

part due to the Franck-Rabinowitch cage effect), the syntheses are biased

towards the net production of the most complicated organic molecules

(v., e.g., 31).

Although continued radiation and high temperatures would lead to the

eventual destruction of all these molecules, we must remember that meteoritic matter vac falling into the lunar atmosphere throughout the period of

organic synthesis. Whipple15 estimates that about 50 gm/cm2 of meteoritic

matter falls on the moon each 108 years at present rates of infall. In addition, it is almost certain that the rate of meteoritic infall on the moon in

32

primitive times was much greater than today. For example, Kuiper believes the moon, receding from the earth because of tidal friction, passed

through a sediment ring of silicates and ices which encircled the earth. As

one consequence of this meteoritic infall in primitive times, the moon's

surface must have received a dust cover, probably composed primarily of

silicates and ices, which can be identified, at least in part, with the present

lunar surface material. The organic molecules would then be covered by a

protective layer insulating them from the extremes of lunar temperature and

absorbing the incident solar radiation and subsequent meteoritic infall. The

laying down of the initial protective covering could have itself caused some

destruction of the molecules because of heat generation during impacting of

the initial meteoritic infall. For a sufficiently dense atmosphere during

279
this initial phase such an efiect would not be serious. Provided that no large

scale destructive events have subsequently occurred, it is therefore not unreasonable to expect the presence of both simple and complex organic

molecules on the moon, beneath the dust layer, and with an average surface

density of as much as 10 gm cm -2.These remarks apply properly only to

regions on the moon where it is certain there have been no extensive lava

flows; the southern highland appears to bc ouch a region. 3

A sample of appropriate lunar sub-surface material should then have

an organic fraction easily detectable by simple chemical analyses. When

compared with suitable laboratory results, a quantitative and qualitative

analysis would give important clues on the early history of the solar system.

Because of its great potential importance, the admittedly very speculative possibility must be raised that life arose on the moon before the secondary

lunar atmosphere was lost. There is considerable likelihood that conditions

on the moon 5 x 10 9 years ago were not very different from conditions on the

earth 5 x 10O9 years ago. Recent thinking on the origin of life on this planet

is increasingly inclined towards a very rapid origin for the first selfreproducing system. Z231If a similar event iso occurred on the moon,

natural selection may be expected to have kept pace with the increasingly

more severe lunar environment, at l.east for some period of time. Although

the chances of extant life on the moon seem exceedingly remote, there is a

finite possibility that relics of past lunar organisms, if any, could be preserved indefinitely if sequestered well beneath the protective cover of the

upper lunar surface material.
Section Three

Conclu sion

Due to the possible similarity in primitive organic syntheses on the

earth and the moon, assurance cannot be given that organic matter indigenous to the moon will be distinguishable from accidentally deposited

terrestrial organic matter. However, indigenous organic matter will be

primarily localized beneath the congealed lunar dust layer; while deposited

terrestrial organic matter should be primarily localized at the surface.

Even microorganisms in dust matrix interstices shielded from solar illumination would probably be far above any indigenous lunar organic matter.

If the lunar maria are frozen lava fields, a landing on them would be greatly

preferable to a landing on non-lava areas such as the southern highlands.

Before any moonfall is attempted, the microstructure of the lunar surface

material and the lunar m~agnetic field should be studied as effectively as

possible. In spite of the unlikeliho-)d of biological contamination difficulties,

it is still probably good scientific c&1.ution to make the instrument package

as aseptic as practical considerations arrived at after serious evaluation

will permit.
Appendix I

SURVIVAL TIME OF AN IRRADIATED POPULATION
Appendix I

SURVIVAL TIME OF AN IRRADIATED POPULATION

We consider a population of N organisms, each having mean 0

-3

density e gm cm , characteristic size a cm, and mean lethal dose

of a given kind of electromagentic or corpuscular ionizing radiation,

D roentgens. The population is irradiated with an intensity of

-2 -1

I erg cm sec of the given kind of radiation, which has a mass

absorption coefficient in organic matter of _U// cm2 gm We are

interested in the time, t, in seconds, for the population to be depleted

from N to N organisms. 0

Let J be the energy absorbed by unit cross-section or organism

due to a dose of d roentgens. Then, since one r corresponds to the

absorption of 93 ergs/gm,

t/ '3 (od-d (1)

On the other hand, if the ene'rgy incident on unit cross-section of the

organism is E , then, by Beer's Law, the energy transmitted througl- 0

the organism is

Consequently, the energy absorbed by the organism is

2 =2Z -2 (,/3)°

Now if E ergs absorbed by 1 cm corresponds to a do!ýe of d roentens,

E = J, and frnrn eqs. -)) an.id (3), a

283
Consequently, the time, ? , for one organism to accumulate D roentgens

-2 -1

due to an incident flux of I erg cmn sec is

-7-= "D (5)

Assuming an exponential survival curve for the population of organisms,

the number surviving after time t will be

//V. e (6)

Solving eq. (6) for t, substituting from eqs. (4) and (5), and converting

from natural to common logarithms, we )btain for the time in which the

population will have been depleted to N organisms,

In the case that the mean lethal dose, D, is given directly in

units of erg cm"2 instead of roentgens, as is the case for ultraviolet

irradiation, eq. (7) is replaced by

~~j4~~~ (5eQ7 / A,) Nr{ (8)

Table I was constructed from eqs. (7) and (8) with the following

simplifications. was taken as unity throughout.

For an organism opaque in the given radiation,

and eqs. (7) and (8) reduce respectively to

=,;A e:InII ,I'),., f' r, (9)

and

)A,'v) (10)

284
For an organism which is almost transparent in the given radiation,

and a Taylor series expansion of the exponential reduces

eqs. (7) and (8) respectively to

5/0 /0/

and

"re r~,:-~o •+,, (12) ,.
REFERENCES

1. Lederberg, J. and Cowie, D. B., Science, 127, 1473 (1958).'

2. CETEX Reports, Science, 128, 887 (1958).

3. Stormer, C. The Polar Aurora, Oxford U. Press (1955).

4. Costain, C. H., Elsmore, B. and Whitford, G. R., M. N.

Roy. Astr. Soc., 116, 380 (1956); Edwards, W. F. and

Borst, L . S., Science, 127 325 (1958).

5. Reiffel, L., Structural darnage and other effects of solar

plasmas, Armour Research Foundation Report ARFDA-6

(1959); and J. Am. Rocket Soc. , in press.

6. Das Gupta, N. N. and Ghosh, S. K., Rev. Mod. Phys.,

18, 225 (1946).

7. Elwert, G., Z Naturforsch., 9, 637 (1954).

8. Bacq, Z. M. and Alexander, P, Fundamentals of Radiobiology,

Butterworth, London (1955).

9. Lea, D. E., Actions of Radiations on Living Cellc.

Cambridg(. U. Prces (1955).

10. Luria, S. I-,, In Radiation Biology, vol. 2, ed. A. Hollaender,

McGraw-4iJl, (1955) chap. 9.

11. Kimball, R. F., In A. Hollaender, op. cit., chap. 8.

12. Zelle, W. R., and Hollaender, A., In A. "'Ilaender, op. cit.,

chap. 10.

L 3. See Chapter V of this report.

14. Baldwin, R, B., The Face of the Moon, U. Chicago Press,

(1949); Kuiper, G. P. , Proc. Nat. Ac. Sci. , 40, 1096 (195-1);

Kuiper, G. P., In Vistas in Astronautics, Pergýamon Press,

in press (1959); Urey, H1. C., Ir- Vistas in ýAstroncur-, vol. 2,

ed. Beer; A. . :-ergrnaron Pxes- 5 (1956), p. 1667: Urey, 1-1. G.

Observatory, 76, Z32 (1956); Gold, T., 1". N. Roy. A-tr. Soc.,

I15, 585 ()95 5

15. Whipple, F. L. , In VitFLJs in Astronaut'c.p. Perganon P-eas,

iAfl pre:c s { :,-)
16. Abelson, P. H., Carnegie Inst. Wash. Yr, Bk. No. 53, p. 97

(1954).

17. Kuiper, G. P., In Astrophysics, ed. A. Hynek, McGraw-Hill

(1951) chap. 8; Kuiper, G. P., Atmospheres of the Earth and

Planets, U. Chicago Press (1952) chap. 12; Urey, H. C.,

The Planets, Yale U. Press (1952).

18. Kuiper, G. P., Mem. Soc. Roy. Sci. Liege, 8, 401 (1953).

19. Kuiper, G. P., Proc. Nat. Ac. Sci. , 37, 383 (1951).

20. Spitzer, L., In Atmospheres of the Earth and Planets,

ed. G. P. Kuiper, U. Chicago Press, (1952) chap. 7.

21. Miller, S. L., J. Am. Chem. Soc., 77, 2351 (1955).

22. Oparin, A. I., The Origin of Life on the Earth, Academic

Press (1957).

23. Sagan, C., unpublished; a detailed discussion of the photoproduction of organic molecules in reducing planetary atmospheres

is in preparation.

24. Groth, W., private communication (1959). We are indebted to

Prof. Groth for supplying the results of some of his recent

experiments in advance of publication.

25. Noyes, W. A., and Leighton, P. A., Photochemistry of Gases,

Reinhold (1941).

26. Tousey, R.., In the Sun, ed. G. P. 1(uiper, U. Chicago Press,

(1955) chap. 9.

27. Henyey, L. G., LeLevier, R. and I. evee, R. D., Pub. Astr.

Soc. Pac. , 67, 396 (1955).

28. Schwarzschild, M., Howard, R. and Harm, R., Astrophys. J.,

125, 233 (1957).

29. Hoyle, F., In Stellar Populations, ed. D. J. K. O'Connell,

Interscience, p. 223 (1958).

30. Fox, S. W., Am. Sci., 44, 347 (1956),

31. Sagan, C., Evolution, 11, 40 (1957).

32. Kuiper, G. P., Proc. Nat. Ac. Sci., 4Q 1096 (1954).

287
Appendix II

CURRENT ATTITUDES AND ACTIVITIES REGARDING

BIOLOGICAL CONTAMINATION OF EXTRATERRESTRIAL BODIES
Appendix II

CURRENT ATTITUDES AND ACTIVITIES REGARDING

BIOLOGICAL CONTAMINATION OF IXTRATERRESTPIAL BODIES

A. Organizations Active in the Field

(1) Ad Hoc Committee on Contamination b) Extraterrestrial

Exploration, International Council of Sciei.tific Unions

(CETEX)

For membership and recommendations, see Science, 128, 887 (1958),

and Nature, 183, 925 (1959). The organization is now defunct.

(2) Eastern and Western Ad Hoc Advisory Groups to Committee on Long Term Projects, Space Science Board,

National Academy of Sciences (EASTEX and WESTEX)

EASTEX has had one meeting, WESTEX three. Present membership

of WESTEX is R. N. Bracewell, Stanford, Astronomy; M. Calvin, U. of

Calif., Berkeley, Chemistry; R. Davies, Jet Propulsion Laboratory, Space

Vehicles; N. Horowitz, Caltech, Mi.:robiological Genetics; R. M. Badger,

Caltech, Chemistry; J. Lederberg, Stanford, Microbiological Genetics;

D. Mazia, U. of Calif., Berkeley, Zoology; A. G. Marr, U. of Calif.,

Davis, Bacteriology; A. Novick, U. of Oregon, Biophysics; C. Sagan, U.

of Chicago, Astronomy; G. Stent, U. of Calif., Berkeley, Virology;

C. B. va.n Niel, Stanford, MicrobiologJcal Biodiemistry; H. F. Weaver,

U. of Calif., Be:rke&-y, Astronomy. Views of these organizations are

uascussed below.

(3) Panel on Extraterrestrial Life, Armed Forces -

National Research Council Committee on BioAstronautics, Nai,-0-ii?1 Academy of Sciences
This group has just been formed. The first meeting is scheduled for

July. Present composition is M. Cal•in, U. of Calif., Berkeley, Chemistry,

Cbairrman; J. R. Platt, U. of Chicago, Physics; Cmdr. M. Ross, ONR,

USN; C. Sagan, ARF - Yerkes, Astronomy; G. Stent, U. of Calif.,

Berkeley, Virology; R. Vishniac, Harvard, Microbiology; H. F. Weaver,

U. of Calif., Berkeley, Astronomy.

B. Present Climate of Opinion

From informal meeting notes and personal communications we have

formed some idea of the prevailing climate of opinion. Naturally any summary statement cannot be uniformly supported by all individuals, but a

definite view does exist both for groups a and b.

CETEX feels that the likelihood of any biological contamination of the

moon is very small, since the possibility of reproduction of a deposited

terrestrial microorganism is taken to be negligible. The possible confusion of deposited terrestrial organisms with indigenous lunar organic

matter is considered to exist; but if the number of moonfalls is kept within

bounds, CETEX feels that the contamination will be quantitatively small,

and restricted to a limited fraction of the moon's area,

On the other hand, contarmination is considered to be a much greater

hazard for Mars and Venus, and CETEX urges the development of decontamination procedures to be used on all lunar probes in order to test later

decont.amnination techniques for Mars and Venus.

;ASTEX and WESTEX agree that a deposited terrestrial microo-ganisrn would ptobably be unable to reproduce on the moon, since there

aPr,-,ears to be an absence of biochermrcal precursors. On the other hand

we do not know the lunar sub-surface conditions; Frenmlin has recently

-n7K
pointed out that temperatures a few meters below the lunar surface may be

many hundreds of degrees centigrade, and it is not impossible that subsurface organic matter exists. Under these conditions reproduction of'

terrestrial microorganisms might occur- In view of the geometrical reproduction rate of terrestrial microorganisms under suitable conditions,

and the absence of greater knowledge of sub-surface conditions, EASTEX

and WESTEX urge that no moonfall be attempted until more information is

available and that all lunar probes be rigorously decontaminated.

EASTEX and WESTEX consider the possLble confusion of deposited

terrestrial organic matter with indigenous lwuar organic matter to be a

greater danger than does GETEX. They poiat out that a hard lunar landing

will probably deposit contaminants over a 1;irge fraction of the lunar surface, not a very restricted region as CETEX seems to assume. In addition

there is the possibility that life arose in ancient lunar history. If a viable

organism were recovered on the moon - - it would probably be detected by

clone formation in a suitable medium - - the problem would arise as to

whether it was lunar or terrestrial in origin. Similarities in biochemistry

and/or morphology with contemporary terrestrial organisms would not

necessarily indicate contaminatory origin, because primitive life-forms on

other planets might very well resemble primitive life-forms on the earth.

EASTEX and WESTEX a]so emphasize that deposited microorganisms could

easily be shielded from solar radiation by lunar surface material, and so

rapid radiative killing cannot be relied upon. They stress the imrpor,..ce

of bic I ogic.l and astronomical infcrmation which ia` ght be destroyed by

contam ination.

291
It is interesting to note that CETEX contains no micro-biologists, and

that membership was not made on the basis of applicability of the members'

research to the problem at hand, but on the basis of representation from

each of the constituent organizations of the ICSU. In addition there exists the

statement by a CETEX member that CETEX was afraid to state the contamination case too strongly for fear its advice would not be heeded at all.

It might be argued that since the first moonfall is very likely to be by

a Soviet vehicle, the concern of EASTEX and WESTEX is somewhat academic.

There have been no Soviet scientists calling attention to the contamination

problem, and U.S.S.IR. representation on CETEX could not be secured.

However, concerted effort by the American scientific community might bear

fruit. For exý.mple, much of the pioneer work on the origin of life problem

is by the Russian biochemist, A. I. Oparin, who might be expected to have

an interest in pre-biological lunar organic molecules. Attempts are being

made to contact Oparin. The U. S. propaganda possibilities following a

U. S. S. R. lunar contamination - - or vice versa - - should not be overlooked.

C. Future Work

Work already initiated and expected to continue into the near future

includes (1) development of automatic devices for detection of microbiological reproduction on a suitalle prepared medium, and (2) testing of

decontaminarts, especially ethylene oxide and radiation, to determine

whether a6dequate dc contamrnin.3ion. is possibJe without destroying instrume••ation. F.)r radiation, at least, the situation appears marginal. Later

work might include the standardization of organic components - - e. g.,

plastics - - of mis3i~e systeris intc a few characteristic, biochemically

292-
unlikely compounds.

Research on the infrared reflection spectra of a variety of solid organic

molecules is underway at the U. of Calif. , for future comparison with satellite telescope and lunar and planetary probe spectrograms. ARF work on

visible and near IR absorption spectra of gaseous organic molecules for

comparison with spectra of the Jovian planets will also be continued on a

larger scale at Berkeley.

Publications may be expected within the next year or two from both

EASTEX-WESTEX and from the Armed Forces - NRLC panel on the question

of biological contamination of extraterrestrial bodies. WESTEX is contemplating the writing of a handbook on the whole question of extraterrestrial

organic matter, extraterrestrial life, and contamination; while the Armed

Forces - NRC panel is considering monographs on individual subjects. The

Bio-Astronautics Committee feels that such monographs might clear the air

on controversial issues, saving much needless and repetitious argument in

other committees and agencies.

7-,7
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