Moon radiation flux measurements in infrared and visible spectral regions from Luna 1

Lebedinskiy, A. I.

Lozhnikov, A. A.

Tulupov, V. I.

English

NASA Technical Reports Server

National Aeronautics and Space Administration 
Goddard Space Flight Center 
Contract No.NAS-5-12487 
ST-LPS-RAD-10 549 
-S OF MOON'S RADIATION FLUXES I N  '1"E I N F M D  AND 
I N  THE VISIBLE REGIONS OF THE SPECTRUM ON THE 
AMs "LUNA- 10' 
by 
A. I .  Lebedinskiy 
A. A. Lozhnikov 
v. I. Tulupov 
(USSR) 
L / I 
d o  : I~AGESI 
< c 
2 
5#-cR-82438 (CATEGORY) (NASA CR OR TUX OR AD NUMBER) 
~ 
23 DECEMBER 1966 
https://ntrs.nasa.gov/search.jsp?R=19670009627 2020-03-16T18:54:23+00:00Z
ST- LPS -RAD -10 549 
MEASUREMENTS OF MOON'S RADIATION FLUXES IN THE INFRARED AND 
IN THE VISIBLE REGIONS OF THE SPECTRUM ON THE 
fws ' 'LUNA- 10'' 
Kosmicheskiye Issledovaniya 
Tom 4 ,  vyp. 6, 838-841, 
Izdatel'stvo I'NAUK"', 1966 
by A. I. Lebedinskiy 
A. A. Lozhnikov 
V. I. Tulupov 
SUMMARY 
Measurements of integral radiation flux 
been carried out on the artificial satellite 
of the Moon in the infrared have 
of the Moon "LUNA-10". The instru- 
mentation consisted of radiation receivers constituting flat plates of 15 
dimensions disposed in series. 
absorbing well the infrared radiation (85- 95 percent) and reflecting 70 to 75 
percent of visible light. 
simultaneously, the data of both receivers allow the determination of the ther- 
mal radiation flux of the Moon. 
30 mm 
One of the receivers was covered with enamel, 
The other receiver was covered with gold foil. Obtained 
* 
* * 
The temperature of the lunar surface varies within broad limits, desL{. .I 1 , 
to -150' during the lunar night and rising t83 L120° in the middle of the lunar 
day. As any heated body, the Moon emits a flux of thermal radiation, of which 
the magnitude is dependent on the temperature arid the emitting capability of the 
lunar surface. The intensity maximum of such a radiation is located in the far 
infrared region of the spectrum, 7 - ZOv, Concomittantly the Moon reflects the 
solar radiation incident upon its surface, of which the maximum is in the visible 
part of the spectrum. 
15 by 30 nun dimensions, disposed in series. 
from satellite's board to a minimum the receivers were fastened on a thermally 
insulated foundation, which in its turn was fastened to satellite's board with 
the aid of four titanium supports. 
The device consisted of two radiation receivers constituting flat plates of 
In order to reduce the thermal flux 
The scheme of the device is shown in Fig.1. 
* IZEMF,RENIYA POTOKOV 1ZLUC"IYA LUNY V INFRAKRASNOY I VIDIMOY OBLASTYAKH 
SPEKTRA NA CPUTNIKE "LUNA-10". 
2. 
The receivers were switched onto a circuit measuring their resistance. 
The latter varied as the receiver was heated by the incident radiation, which 
was fixed by the station's apparatus and transmitted to Earth. 
One of the receivers (A) is covered with enamel 
which absorbs well the infrared (85 to 95 percent) 
and reflects 70 to 75 percent of the visible radia- 
tion. 
The other receiver (B) is covered by gold foil. 
As is well known, the latter reflects 97 to 99 per- 
cent of infrared radiation and absorbs well the vi- 
sible radiation. Both the direct and the Moon sur- 
face-reflected radiation of the Sun (infrared fluxes) 
could hit the receiver. 
foil was heated by the visible radiation, whereas 
that covered with enamel was heated by both the solar 
as well as the Moon's proper thermal radiation. The 
data of both receivers, obtained simultaneously, al- 
lowed the determination of the thermal radiation of 
the Moon. AMs LUNA-10 was spinning around its axis 
with a period smaller than the device's thermal iner- 
tia, and this is why the fluxes measured constituted 
the average as a result of rotation. 
The one covered with gold 
Expounded in the present paper are the results 
of measurements. 
it will be the object of a separate paper. 
The anele with summit at the center of the Moon 0 
As to the discussion of the latter 
We shall introduce the following denotations. 
.Board of the satellite 
Fig.1. Apparatus 
1) thermal insulator; 
2) receivers; 3) grip r ing ;  
4) support 
and srdes pascing through the subsolar point C and the subsatellite point P 
will be denoted by v(Fig.2). 
kn~w the longitude 
the subsolar point taken for zero, and the 1'3 t i tude B ,  counted from the lunar 
equator 
At the beginning of April 1966 the latitude of the subsolar point was $lo, 
diminishing to 0" by the middle of May. 
be significantly greater than these quantities, the angle Y is determined from 
formula 
For the determination of the angle Y one m u s t  
of the subsatellite point counted from the longitudL CI!' 
( a  is the station LUNA-10). 
Under the condition that the angle c1 
cos y= cosa cos 6 . 
For angles y < 90" 
Graphs of receivers' A and B temperatures for three communication sessions 
the satellite is located above the sunlit side of the 
Moon, for y > 90" it is above the night side,y = 0' corresponding to terminator. 
are represented in Fig.3. 
5 .  
Temperature readings from the receivers on the satellite were taken down 
every two minutes. As may be seen from 
the graphs, the temperatures of the recei- 
ver A were negative and those of the recei- 
ver B - -  positive. During the 8th session 
the satellite passed from the night to the 
daytime side, and during the 49th session 
it passed from the daytime to the night- 
time side; during the 31st session the sa- 
tellite was located on the daytime side 
of the Moon. It may be seen from these 
graphs that during passage to the daytime 
side the temperatures of both receivers 
rise, and when passing to the nightside, 
they fall. 
It should be noted that during the 
passage of the subsatellite point through 
the terminator to the night side, the sa- 
tellite was still illuminated by the Sun 
for some time, and this is why the tempe- 
ratures of the receivers did not drop so 
sharply. Analogously, the satellite was 
sunlit during long time prior to inter- 
Fig. 2 .  Sketch illustratiiig the 
construction of the angle y .  
secting the morning terminator. 
tions of receiver A is larger than that of receiver B. 
in the shadow rejected by the Moon takes place at the angle y = 123" for the alti 
trde h = 350 km above the Moon's surface. For greater heights this angle increa- 
ses, reaching 140' at h = 1000 km. The satellite was illurninated by the Sun for 
an overwhelming number of sessions. 
In this case the range of temperature varia- 
The set of the satellite 
The temperature of the receivers is plotted in Fig.4 as a I'iiriction of the 
angle y. To that effect data of 44 lunar sessions were utilized. 
During the short 5 to 10 minute sessions temperature readings in the middle 
of the session were taken down, during those of up to 20-111i11tite cluratiori, tliey 
were taken a t  the beginning and at the end of the sessions a id  €or those of up 
to 40-minute duration they were taken down at the beginning, in the middle and d t  
the end of the session. During such prolonged sessions as the one represented i n  
Fig.3, the 8th session, the temperatures utilized corresponded to four uniformly 
distributed moment of time of the session. The angles y in the abscissa axis 
decrease at the beginning during the motion from left to right, then increase 
again. This corresponds to the cases when the satellite passes from the night 
to the daytime siae [passing through the terminator at y = g o o ) ,  and then again 
drifts from the daytime to the night time side ( to the left is the "rise" of the 
satellite on the daytime side of the Moon, to the right is its "setting"). 
A temperature increase in the receivers can be clearly seen on the graphs on 
Because of thermal inertia of the receivers, their the daytime side of the Moon. 
temperatures at intersection of the morning terminator by the satellite (y = 90" 
to the left) is lower than on the evening terminator (y = 90' to the right). 
c 
c 
30 
20 
IO 
z5 
O -  
-10 
-20 
-30 
50- 
40 
30 
20 
10 
-20 
730 
4 0  
. '  
72 72 Y, deg. 
I I 
- - 7  77 74 
500 6 70 $00 lOI4 h,KM 
- 
108 103 96 90 83 
I - 
20'33 ZOh5Jm t - 350 1Jh5gm 2Qh1Jm 
" X X  X M X X ~ L a X  X M x x X y  
rgh3Jrn 
s x x ~ k ~ '  
- 
- K x X X i i ~ X X  x x m  
x x  
49th session of 4-5 May 
- 
31st session 95 20 A rkl 
.- I  
x - 2  
_- --- . '  5f- 
* . .  . '  
40 - . . . ' .  ... - 
. . . .  - 30-' . 
- 71 ? 
- M x x  X x  x x X * M X ~ x  -10 - 
20 - 
lo-70 ' ' 8 2  ' i 4 '  'lqs' * , 123 y,zpad(deg) 
- 
73 
8 80 72 0 490 350 h, KM 
O -  i $ 7 m x  llh47" a 23h2P 23hUP ~ 7 ~ 0 7 ~  t . 
-20-" 8 " x L 
' ( X  X M I S  x 
X X I  
- 
x x  
- -30 - 
- -40 - 
Fig.3. Readings of receivers A and B during 
the Sth, 31st and 49th sessions 
with enamel. The time is Moscow. 
1) receiver B covered with gold foil; 2) receiver A covered 
. -  
-UP[ 
Fig.4. 
The denotations here are the same as in the Fig.3. 
Receivers' temperature as a function 
of the angle Y. 
5. 
The influence of thermal iner t ia  on receiver temperature may be i l l u s t r a -  
ted by graphs i n  Fig. 5 hereafter.  
the time scale for  79 sessions. 
moments of time as i n  the case of  F ig .4 .  The points and the crosses without 
circles correspond to  the right-hand par t  of Fig.4. 
the median points were obtained by averaging the rea l  readings over five-day 
intervals .  
constructed by the points and crosses with c i r c l e s ,  the dashed curves were done 
from points without c i rc les .  
ones, which may be explained by the thermal iner t ia  of the receivers. 
Here receiver temperatures are  plotted i n  
The temperatures were taken down a t  the same 
The curves drawn through 
The median points are  riot shown in  the graphs. The sol id  curves are  
'The dashed l ines run everywhere above the so l id  
X 
0 e 
Fig.5. Receiver temperatures as  a function of time 
Begimicg from 2 - 3 >lay and up t o  13 May, the temperatures of both recei-  
vers decreased: 
a f t e r  which thev began t o  r i s e  again. 
explained by t h e  slow reorientation of the s a t e l l i t e  re la t ive  t o  the Sun i n  such a 
way that the incic.2xe angle 
receiver B,~ovt:.~e:. ~v gold fold,  absorbs more v is ib le  l i gh t ,  such a reorieritatioii 
has in f luexec  -*<?e receiver B more than the receiver A. 
tha t  of receiver A by 22 degrees and tha t  of icceiver B bjj 5 0 ° ,  
Such a variation of temperature may be 
or solar rays upon the receivers increase. S i n w  
Tn cc:iclusion the authors wish t o  thank A. D.  Levchenko and V. V. Vernigor 
fo r  t h e i r  --s.is:nnce i n  conducting the experiment and par t ic ipat ion i n  the pro- 
cessino, oi' -3e (:,/:a o'Jtained. 
Manuscript received on 
22 August 1966 
, 
NO REFERENCES 
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Translated by ANDRE L .  BRICIIANT 
on 23 December 1.966 
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Measurements of moon's radiation fluxes in the infrared and in the visible regions of the spectrum on the AMS Luna-10

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