INFORMATION ON SOVIET BLOC INTERNATIONAL GEOPHYSICAL COOPERATION - 1960

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• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP82-00141R000201230001-6
• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 42
• Document Creation Date: November 9, 2016
• Document Release Date: February 16, 1999
• Sequence Number: 1
• Publication Date: June 17, 1960
• Content Type: REPORT

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INFCP*T OI N ON SOVIET BLOC INTERNATIONAL GIEOPHXSICAL COOPERATION - 1960
Jung 17, 1960
U. S. Department of Commerce
Business and Defense Services Administration
Office of Technical Services
Washington 25, D. C.
Published Weekly
Subscription Price 012.00 for the 1960 Series
Use of funds for printing, this publication has been
approved by the Director of the Bureau of the Budget.. October 28, 1959
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J TERNATIONAL QBOPH72XCAL COOP &TIQ~ PRQIAA$ ??
SOVIIRL'-BLOC ACTIVITIES
Table cd 6wteate
I. ROM M AND ARTIVICIAL SARTH SATE MZM
II. UPPRR X1!W PRNRB
1
2
III. 14BTBORQLOf1T
33
IV. QIACIOLAQT
35
V.
OCMN0(1RAPHY
35
VI.
ARCTIC AND ANTARCTIC
36
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X. ROCKETS AIW ARTIFICIAL EARTH SATELLITES
"Priroda" Lead Article Reports on the Soviet Ballistic Rocket
On the evening of 20 January 1960 there was launched a powerful
multistage ballistic rocket from the territory of the Soviet Union; it
traveled a tremendous distance and landed accurately in a predetermined
part of the Pacific Ocean. This rocket was designed to put heavy earth
satellites into orbit and for making cosmic flights to the planets of
the solar system. The following represents the views at Prof. B. V.
Kukarkin on this subject:
The future tasks of space study present some new problems asso-
ciated with the fact that the reaching of the nearest planets, Mars and
Venus, far example, is a more conplex matter than that of reaching the
Moon. The shortest distance to these planets is more than 100 times
greater than the distance to the Moon. Consequently, an error of 200
km on a-flight to the Moan from the Earth would be equivalent to an
error of several tens of thousands of kilometers on a flight to the
nearest planet. Therefore for a successful launching of cosmic rock-
ets for the purpose of approaching Mars or Venus, it is necessary to
have more rigid requirements for the perfarmai ce of all elements in-
volved in the travel of the rocket. The specifications required for.
a Moon shot would be far inadequate far a rocket intended to hit mcwe
distant bodies (Mars or Venus) at a given moment and at a given point.
The experiments with the multistage ballistic rocket made on 20 and
31 January 1960 show that, there is every reason to expect that the
necessary accuracy can be achieved.
In actuality, the first launching showed that the rocket on
falling into the ocean deviated from the computed point by less than
2 km. Such accuracy makes it a sure thing that we will, be able to hit
Mars or genus with a rocket at a previously ccuputed disterce with a
tolerance of several thousand kilometers.
I would like to make note of other possibilities in the field
of astronocy that have been opened up by these remarkable experiments.
It is obvious that the accoupliebment of long-range flights in the fu-
ture will enable us to deliver to other planets apparatus, instruments
and other means for the transmission of information to the Earth. As
a result it will be possible to get such data about Venus or Mars as
would be impossible to dream of if the investigations were made frown
the Earth and through the Earth's atmosphere.
In respect to our own satellite, the Moon, u-e my expect new
najar discoveries by flights mad", around that body and by the direct
establishment of permanent stations on its'surface. It is probable
that these stations will be equipped with automatically operating in-
struments, and in the more distant future, Man will. undoubtedly be able
to directly explore the planets of the solar system.
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The ouccesafU launc.?ixigs of the posreri"al ballistic rocket are
an important stem ox7 'Ciie way to thN direct study of other planets.
("New Attainment of S-Wiet 8cienac,, unsigned article, Priroda, No. 2,
1960, pages '4,-4)
' e elys" Report's on Lect'xre Deli cored by Dr. I. S. Shklovskiy
The following in a summary of tIa.e contento of a recent lecture
delivered, by Dr. I. S. Shklovskiy entitled : "The Study of Cosmic
Space by Rockets and Satellites.' It should be emphasized that there
in no evidence that the authors of this article are directly quoting
the lecturer.
The lifetime of the third Soviet cosmic rocket was expected to
end in Me.rcb 1959, but later observations forced a revision in this
estimate. The original revision gave the rocket eight months more --
but thin estimate has now been revised again. It is now predicted
that the rocket will fall in the month of April of this year. Why was
the prediction so faulty? What was responsible for the error? (Trans-
tiator'a note: These questions are asked in the article, but are not
specifical? answered,,)
The article then proceeds to a review of the facts concerning
our upper atmosphere that are now generally known, although our con-
cepts of the atmosphere have been so greatly altered in the last few
years. The authors discuss the "breathing" of the atmosphere and the
theory of corpuscular radiation; this is followed by a discussion of
whether or not the Earth has a corona. Thereafter the subject shifts
to that of solar "winds," not winds at all, of course, but the move-
ment of corpuscles from the surface of the Sun.
This article, "mea?:,y" as it is, was published in a journal for
popular consumption; it wanders from topic to topic, touching only
briefly on the suoJect matter concerned. ("The Earth Satellites
Speak," by G. Goryachev and T. Mashke,rich, Nedelya, No. 10, 1960,
pages 8 and J.0 )
"Priroda" Reviews Book "The Nature of the Moon"
The author, well known for his works on the investigation of
the Moon, possesses the ability to tel1 about the most complex astro-
nuzrMcal problems in a lively and interesting way. All the material
related to the nature of the examined heavenly body is divided into
three chapters: The Moon as a Heavenly Body, The Topography of the
Moon, The Physics of the Moon's Surface. Each of the problems is
treated on the basis of the most recent research by both Soviet and
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foreign scientioto. Ii; the final. chapter N., N. Sytinskaya (the author
examines a problem a.' :for c w'idle c:U .e ux" ri adera -?? the
physical coudit.Lona tlurc will o.:- cu':xunt~red by the .'irrit people t3
tread on the Moor's m.rrar,!. TI'Xt o uma 1. book is supplemented by a
full list of the named of lwnar s eao azicl carat! rii .
Thin book, LTG pngec, lnr: , r:4,." rl for fa i.- rttbh e3 25 kopecks.
It was published in 1-.959 in Moseo r. (Px:l.t'i,rca, S:, 1)6'0,, pt:ge 1.16)
Aurora Observed in Sinkiang Tall :t:ands:t?:or: of e. Dric_' Notch in
Pr iroda
Ou 15 June 19; 9 a g:ro:.p of sr.,;,entists Q;: the Acaden of Sciences
of the USSR and tae Acadhriy of Science3 of the Ch'ineae People's Repub-
lic returned from afield trip through Northern Dzungciria and the Altai
portion of Sinkiang. When stopping for the evening on the eastern part
of the Daungarian de-pre-asioo, oki the banks of the Urungu River, at the
Keleneay (Etta-.) svrvey mark at 40`0 N and 900 20' E, we beheld an un-
i;sually bright aurora.
The day was clear, completely cloudless and windless. We were
on a' hill and the sky was open in all directionri. At 2130 hours local
time ' (1830 ho=s, Moscow time), when that part of the ssgr at the point
of the setting Sun was still somewho;h illuminated, the sir unexpectedly
grew red an if from an immense conflag:?ation. In 2 to 3 minutes file
aurora intensified. It colored a considerable part of the sky in a
full, dark, deep and extremely rich crimson-claret color or ruby color.
Luminous bright rose-colored pil7.ars flared up and died away against
this background. All this illumination resembled hundreds of verti-
cally standing spindle-shaped searchlight beams, growing narrow at
both the top and bottom. At this time the lower part of the sky,
situated in a narrow band above the horizon, was without color. The
center of the aurora was situated a little below the pole star, while
the edges extended westward beond the constellation Ursa Major and
eastward beyond the constellation Pe=:-3eus. Three stare of the con-
stellation Auriga were visible ti'rough the aurora. The rose-colored
rays first arose in the nor';;hcaat, the:i shifted to the northwest.
This combination of a rich, dark., crimson-claret background and bright
rays continued for a period of 20 minutes -- until 2150 hours. Then
the bright rays disappeared, the dark red bacirground became homogeneous
and gradually became lest intense; at 2230 hours a reddish coloring
was still clearly visible in the sky.
Unfortunately, we could not determine where this aurora was
still observable. However, in the city of Hu-chen, situated farther
south, at latitude 4 40., the aurora was also clearly visible (informa-
tion from Lim Pea., soil scientist on this same expedition). It was
not observed in the city of Urumchi; this was probably due to the
dustiness of the air in this region.
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Since the problem o the origin of auroras has again attracted
the attention of astrophya cists because of the data collected by So-
viet earth satellites, we onsider it pertinent to note still another
fact. The summer of 1959 n Sinkiang was not distinguished by high
temperatures. However, t day following the aurora was unusual in
this respect: from 1100 h a to 1540 hours the hot wind blowing
from the west was accompan ed by extremely frequent and very strong
gusts of a burning wind au h as we had never observed in the course
of three years' work in S its southernmost its
situated at latitude 36?. ("Aur(;ra in China," by Professor B. A.
Fedorovich, Priroda, No. 2, 1960, page 105)
Radioelectronics in the Cosmos -- Full Translation of an Article by
V. I. Siforov, Corresponding Member_of the Academy of Sciences of the
USSR
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One of the striking accomplishments of the Soviet automatic in-
terplanetary station is the photographing of the invisible aide of the
Moon and the radio transmission of these images to the Earth. For the
first time in the history of mankind it bas proven possible to see that
part of the surface of the Earth's natural satellite which bad previ-
ously never been observable. In the scientific investigation of the
Moon and the cosmic space surrounding it an important role has been
played by the scientists and designers working in the field of radio-
electronics.
For the first time in the entire history of radioelectronics
the Soviet automatic interplanetary station accomplished the transmis -
sian of half-tone images for immense distances by means of a televi-
sion system. This has opened up alluring possibilities for photo-
graphing the surfaces of other heavenly bodies, of Mars and Venus in
particular.
Soviet specialists were faced with the problem of overcoming
difficulties of design and construction of radio apparatus for use in
space and on the Earth's surface. Included among these difficulties
were the following: the limited power of the radio transmitter placed
aboard the automatic interplanetary station, the immense distances of
space, and the extremely small intensity of the radioFraves arriving at
the Earth. When there are very weak signals the internal noises of
radio receiving apparatus at the Firth'a a=face and radio interference
of cosmic origin are detrimental factors. It was neceasary'to guaran-
tee that the weak, useful signals be distinguishable against this back-
ground of interference. We can judge hoer weak the useful signals were
by merely stating the fact that their power was 100 million times less
than the power of the radio signals reaching the antenna of an ordinary
television set. Just a few watts -- that was the power of the radio
transmitter carried into space; it was this transmitter that sent to
Earth all the scientific information for a distance of 470,000 km from
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the iXrth. Each watt of the power radiated by the radio transmitter,
as a result of its passage through an immense sphere with its center
at the momentary position of the interplanetary station, produces on
each square meter of the Earth's surface a power that is approximately
three times leas than one billionth of one billionth of a watt.
Tt& great difficulties in receiving ouch extremely weak radio
signals were overcome by using highly sensitive radio receiving appa-
ratue Lvd high-quality antennas and also by using speeds of transmis-
sion f.)r the images that were tens of thousands of times slower than
the speed of transmission in ordinary television centers at the Earth's
In crxeaparison with the first two cosmic rockets, our third rocket
bad +a camber of important innovations. The apparatus aboard was de-
I signed for a greater largev'ity. What were the measures used to accom-
plish this? First, solar batteries were included among the various
different power a .uz'cea; these made it possible to transform the Sun's
energy directly into electrical energy. Second, an operating regime
,..ore economical in its consumption of electric power. was incorporated
for use. in the functioning of the various instruments and the transmis-
sion of info ? tics. The transmission of information was accomplished
in accordance with a fixed program, from 2 to 4 hours each day. Third,
the control o; the apparatus aboard the station was accomplished from
the Barth. This made it possible to switch on the instruments aboard
the station only when it vas necessary to do so. All this provided a
considerable economy in the consumption of electrical power from the
sources of supply.
Very high accuracy crag already achLeved at the time co the
launching of the second Sorr,;,et cosmic rocket. It should be noted that
if the initial velocity of the container of this rocket deviated by'
only a rew hundredths of a percent, it would not have reached the
Moon's surface. The sccii-acy of the initial data of motion of the
third cosmic rocket would have to be still greater, since it was nec-
essary to predict its travels for a considerably greater period of time
and compute the position which it would occupy in space after covering
a route on the order of a million kilometers -- from the Earth to the
Moon and back to the region of the Earth.
The required accuracy was brilliantly insured by the efforts of
Soviet specialists. Already in the initi+:l period of travel of the
automatic interplanetary station it has become clear that the*estab-
lished objective will be attained. A comparison of the actual and com-
puted trajectories has shown that zney colncxae win a nlga degree cu
accuracy.
The role of radioelectronice in the study of cosmic space by
artificial satellite has already been revolving around the Earth for
a year and a ball. The chemical and solar power sources are providing
the proloaged,and stable operation of the radio transmitter "Mayak"'
('Beacon"), radiating radiowaves on a frequency of 20.005 me.
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At the present time, when the power of the chemical batteries
has been exhausted, the powering-of the transmitter in being accom-
plished by solar batteries and the transmitter io emitting signals
during the period when the satellite is situated outside the Earth's
shadow.
Observation of the passage of the radio signals sent by the
transmitter has provided supplementary information about the iono-
sphere and the propagation of radiowaves. It can even be stated that
without radioelectronics it would be impossible to set up these re-
markable experiments.
What is the principle role of radioelectrontce? By meant' of
electronic computers there have been made preliminary computations of
a great number of alternatives of different trajectories for the travel
of cosmic rockets, the computation of permissible inaccuracies in the
values for initial velocities, the directions of travel, the moments
of separation of the container, etc. The artificial heavenly bodies --
satellites and rockets -- transmitted by radio abundant scientific data
.about the most varied properties of cosmic space. Finally, by means of
the radio electronic apparatus there has been accomplished a checking
of the corrections of the selected flight trajectories of the batel-
litee and rockets in their process of travel in the initial stages of
their course. On the third Soviet cosmic rocket the control of on-
board apparatus was accomplished from the Earth by radio and many other
things have been achieved by means of radioelectronics.
During the last two years our scientists have achieved immense
successes in increasing the range of radio transmission. Whereas radio
transmission from the artificial earth satellites to the Earth was ac-
camplished over a distance of several hundred kilometers, with the
first, second, and third cosmic rockets the range of action of these
transmitters became a matter of several hundred thousand kilometers.
There was also a considerable increase in the rapidity of transmission
of scientific Information from aboard the automatic interplanetary
station in comparison with that which was achieved on the first and
second Soviet cosmic rockets. For the first time in the history of
radio engineering and electronics there was achieved the automatic
control of ow board apparatus of the third cosmic rocket at a distance
of about 500,000 kilometers. It was achieved by means of a radio com-
munication line "Earth-8tation." This made it possible to more ra-
tionally utilize the power resources of the interplanetary station.
The radio transmitter and a number of other elements of the station
were switched on only in those periods of time which corresponded to
the most favorable conditions for the transmission of information
along the line of the cosmic radio connection and when this was nec-
essary from the point of view of determining the characteristics of
movement of the station. By means of an automatic system of orienta-
tion an end was brought about to the rotation of the entire.etation
around its own center of gravity, criaing at the moment of separat:3.on
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from the last stage of the rocket, and the station occupied a fixed
position in relation to the Mooia. This was favorable for the photo-
graphing of its rv_vez-o.:? aide. This complex technical problem wan
solved by means of an array of apparatus which included solar and
lunar pickups to transform the energy of the direct rays of the Sun
and those reflected from the Moon's surface into electrical signals.
In turn, the received electrical signals reacted on the complex sys-
tem controlled by the mciem,nt of the station around Its center of
gravity.
In the course of the enti.oe period of photographic work, the
automatic system of orientation :insured the continual pointing of
the station at the Moan. This system was designed in such a way as
to practically eliminate static caused by reflected light from the
Earth. To accomplish this the station was first oriented on the di-
rect rays of the Sun, and then on the light reflected from the Moon
falling on the station approximately from a direction opposite to
that of the Sun. In this case the Earth was situated to one side
and its light d:1.d not d,tsrupt the operation of the system of orienta-
tion. On completion of the process of photographing the Moon the
orientation system was automatically switched off and the entire
station was given a regulated rotation with a fixed velocity, in-
suring a favorable thermal regime and normal functioning of the sci-
entific apparatus.
More than a few other complex problems have been successfully
solved by Soviet radio specialists in this grandiose cosmic experi-
ment. Included among them was a provision for the reliable opert'f.on
of the radio apparatus under the complex conditions of flight In
space, the housing of a2.1 the instruments in a limited space, a pro-
vision for their electrical supply, the design of a reliable system
of control of the instrwnents from the Earth at distances up to
500,000 kilometers, and a series of others.
In our time science and technology are developing at a rapid
pace. Before us are many difficult tasks and problems in the con-
tinuing study of cosmic space. However fantastic these problems ap-
pear, it is nevertheless possible to assert with great confidence
that they will be successfully solved. And this will not be in the
very distan future.
However great are the suc.esses of the future mastery of cosmic
space, humanity will never forget the Soviet researcLers whose self-
sacrificing work resulted in scientific feats of immense signifi-
cance -- the launching of the first artificial earth satellite, the
creation of the first artificial planet of the solar system, bril-
liant investigation of cosmic space near the Moon, the sending of
the first automatic interplanetary station into space, the photo-
graphing of the unseen. reverse side of the Moon and the successful
launching of a power-F'ul ballistic rocket which deviated fk om its tar-
get by less than 2 kilometers after having traveled 12,500 kilometers.
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There is n doubt that Soviet scientists in the future will
also make a wort contribution to the development of the science of
cosmic apace. De pite the exceptionally great difficulties involved
in interplanetary flights there is every reason to believe that it
will be solved au cessfully. The high level of Soviet science and
technology, the r pid tempo of its development and the fundamental
superioritiee of he socialist structure, are insuring all the neces-
sary conditions f r the successful and rapid conduct of scientific
research on an nae scale; the great zeal on the part of Soviet
scientists to coo erate with the scientists of all countries for the
attainment of sci ntific progress for improving the life of the masses,
together with the previously mentioned factors, is very markedly e;c-
celerating the so tion of the most difficult -problems -the 'ores
("Radioelectronics in the Cosmos," by V. I. Siforov,
Priroda, No. 2, 1960, pages 5 -7) - r''.. !f : i.
Determination of Radial Velocities of 'Stars by Use of a 70-cm Meniscus
Telescope and Large Objective Priam
The, investigation of radial velocities in an important factor
in the study of the dynamics of celestial bodies. In the past a knowl-
edge of radial velocities has played an important role in the discovery
and study of such phercmiena as the asymmetry of stellar motions, the
rotation of the Galaxy and the "red shift" effect in extragalactic
nebulas, etc.
At the present time the study of. the character of stellar mo-
tions in such systems-as the stellar asaociationri w:e assuming great
importance. Accordingly., interest is increasing in the radial veloci-
ties of these objects.
The determination of radial velocities in the associations
should preferably be accomplished by use of an objective prism for
the following reasons :
1. The stars forming associations are grouped in relatively
small sectors of the sky; for this reason it in possible to simul-
taneously photograph then with an Objecti?7e prism and this gives a
great ecoaogr in time of observation.
2. Making up 0-associations are stars of early spectral
classes (for the most part); fcr such stars it is more convenient
to use smell dispersion during the deterzrinatior of radial velc'ct -
ties inasmuch as small dispersion enables us to emplc briefer expo-
sures, while the accuracy of measurement of the spectrograms depends
but little on the dispersion value due to the extraordinarily great
width of the spectral lines.
3. By using an objective prism it is possible to photograph
weaker stars than is possible with a slit spectrograph with the came
aperture of the feeding instrument.
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On the other hard, the determination of radka., velocities by
means of t} objective prism to associated with a series of difficul-
ties, among which the moot conp1ex is the problem of the reference
line and the elimination of a whole series of systematic erro:e.
The determination of radial velocities requires measurements
of the ap".-tral lines relative to those positions which they would
occupy in the t,;pectrtun of a fixed star. Whereas when using a alit
spectrograph the establishment at such reference lines iv possible
by nr-ans of an ertieicial light oaurce, in a case when an objective
prism is used the establishment of such a reference line is
impossi- ble. It is also extremely difficult to establish additional lines
in the spectrum of the star by use of an a]~)rqpriate filter.
Also associated with great difficultkois is the elimination of
numerous systematic errors.
Because of the difficulhies mentioned, numerous experiments
have been made for the determination of radial velocities of stare
by using an objective prism; in a majo:4ity of cases they have not
attained the desirod accuracy. Only i individual cases has it
proven po iible to reduce errors in measurement to a value less
than 1 10 9-.. .
sec
After the installation of the 70-cm meniscus telescope at the
Abastumnskya Astrophysical Observatory, work has been carried on
for the purpose of determining the radial velocities of stars by the
use of an objective prism.
In photographing stellar spectra we have used the reversion
method. The photographing of each region was accomplished twice on
the same plate. Between these two exposures we turn the prism 1800
on its optic axis. As a result., each star gives an image in the
farm of two spectra situated side by side. The ultraviolet en .s of
these spect..*a are throed in opposite directions; the Doppler shift-
ing o? spectral lines also takes place in opposite directions.
Therefore In the two spectra received from the one star the rela-
tive shifting of the line is twice as great as in either of them
indiit'AiLs'!ly. There is a correspondiiiq increase in the accuracy of
measurements. In this way there is eliminated the need for the es-
tablie+he nt ~7r a fixed reference line.
At the saw. time the reversion to all intents and purposes is
free frr m systematic errs-?s caused by the presence of atmospheric
dispersion ani the chromatic aberration of magnification.
Other acairces of systematic errors are distortion cc the prism,
distca?t,ion of the objective, and change in atmospheric conditions in
the imterval of time between two exposures; during this time there can
also be a !::barge in the position orf the plate in the instrument,
a case' eta .
The joint action of these factors is the reason why the shift-
ing of the spectral lines beccwes a function of the position of the
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star relative to the center of the plate in the instrument. This re-
lationship has the following form:
oy - ax + by + cx2 + dxy + ey2 + ... (1)
where Ay designated the shifting (displacement) of the spectral lines
caused by the above-indicated reasons, while x and y are the rectangu-
lar coordinates of the star.
For computations of the indicated errors we made a detailed in-
vestigation of the optical characteristics of the telescope and the
objective prism We On the basis of these investigations we computed
the values of the coefficients of the terms ii, expression (i), from
the second to the fourth power.
In respect to the coefficients of the terms of the first order,
their value depends on many factors that are difficult to take into
account, and the theoretical computation of these coefficients is ac-
companied with great difficulties. Therefore the determination of
the coefficients a and b, entering into expression (l;, is better
done empirically.
This is especially convenient in a case when we know ahead of
time the values of the radial velocities of many measured stars.
this case it is possible to get the abeo'iate values of the radial
velocities of the remaining stars. In a oase to the contrary it is
necessary to assume that the velocities of the stars measured on one
plate are equal, on an average, to zero. On the basis of this assump-
tion we get the relative radial velocities at the stars (the velocity
of the individual stars relative to the center of the whole group).
To all intents and purposes the computations are accomplished
in the following manner. After the measurement of the plate the ini-
tial point of the coordinates is selected to such a way that -- taking
terms of higher power into account -- the valu:e of the readings change
little from star to star on the whole plate. This means that the val-
ues of the coefficients a and b. entering into expression (1), differ
little from zero.
The accomplishment of such a step is always possible due to
the following reason. As direct computation indicates, the coeffi-
cients c and e., standing before the squared terms, considerably ex-
ceed in value the coefficients of terms of higher paver; therefore
the expression (1) to all inteocs and purposes constitutes a squared
form. This fact enables us to zero the coefficients of the terms of
the first power by means of a change in the beginning of the coordi-
nate system.
After the introd.actiox of a correction for the terms of higher
powers, we compute for each star the differences between the indi-
vidual and mean values of the readings (for the individual lines).
The derived differences, after multiplication by the scale, gives
values for radial velocities which require additional correction for
terms of the first order.
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If the value of radial velocity derived in this manner f or the
i-th star is designated by vi, and the real value for radial velocity
is designated by vio, then for each star it is possible to write a
condition equation:
CPYRGHT
A + llx i + Cyi - Avi , (2)
where xi and yi are the rectangular coordinateu of the i-th star and
Avi -- a correction which must be introduced into the value vi:
Avi - vio - vi. (3)
It sufficient stars with the known radial velocities vio are
measured on the plate, then the solution of a system of condition
equations (2) gives values for the coefficients As B, and CO and, con-
sequently, there will be determined the absolute values of the radial
velocities.
If there are no objects with known radial velocities among the
measured stare, then we assume that:
(*)
In this case the coefficient A remains undetermined and we get
the relative values of the radial velocities. The condition (4) is
equivalent to the assumption that the studied group of stars does nab
rotate around an axis perpendicular to the line of vision. It is
clear that the validity of such an assumption should be checked by
cane method or another in each individual case.
A case is also possible when the number of reference stars with
certain radial velocities is inadequate for the determination of all
three coefficients. In this case the coefficients B and C are deter-
mined by the above-indicated method, while the reference stars are
used for determination of the value A.
At the present time a determination is being made of the ra-
dial velocity of stars of types B-F in an association lying near C
Perseus,
Given below are the results of measurements for a region with
the center: .
011950-3b54m,81950-+31050' -
Table
BB Sp V BD Mpg Sp V
310646 10.1 Al + 56, 310674 9.9 A2 + 25b
31 647 9.7 B9 + 24a 30 595 9.1 B9 + 3001
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 Cp4g ped For Release 1999/09/08: CIA-RDP82-00141 R000201230001-6
BD
Bp
V
BD
m. 3.
Bp
310649
6.5
B4
+ 22c
30597
10.3
75
- 650
32 665
9.6
A8
+ 53a
32 697
8.4
A0
+ 15a
32 666
9.8
A0
- 19b
31 675
10.3
F5
- 22b
31 650
6.6
79
- 32c
29 654
9.8
A6
- 5b
31 652
8.4
A6
- 9a
29 655
9.8
Al
- 84c
30 576
9.5
89
- 35c
32 698
10.2
P3
- 15b
31 653
10.3
B9
+ 15b
29 656
9.9
A2
+ 20b
31 655
7.4
B9
+ 29c
31 678
10.3
Fo
- 33b
31 658
8.6
B9
+ 39a
30 598
10.3
PO
- 46b
31 657
9.4
39
- 2b
31 680
9.3
B8
- 166
29 634
10.3
A;
+ 9b
30 601
10.0
A4
- 19b
30 579
9.8
A0
+ 33b
32 702
10.4
P3
- 6c
31 659
9.6
A3
+ 2s
33 754
10.4
A9
+ 24c
32 669
9.4
A3
09
30 605
10.6
A3
- 15b
30 581
10.9
A7
+ lc
33 756
10.0
75
+ 36c
30 582
6.4
A3
- 58c
32 703
8.5
B9
+ llb
30 583
10.1
A7
+ 21b
33 758
10.0
Al
- 8b
32 674
9.2
AO
- 1U&
31 686
8.9
AL
+ 1-17a
32 675
10.6
B8
+ 7b
32 706
9.9
76
+ '.8b
32 676
9.8
B9
- 34b
33 760
10.3
A5
+ 15c
33 731
9.0
72
- 5b
31 687
9.3
B8
+ 49b
32 8T8
10.6
A3
- 2c
31688
10.2
A6
- 46b
29 640
10.1
B8
- 35c
31 689
9.7
B9
- 1b*
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 A wm or Release 1999/09/08 ' CIA-RDP82-00141 R000201230001-6
ga Sp V BD 8p V
32?679 8.4 AO + an 310690 iC.l P3 + 32b
32 661 10.9 A3 - 53c 30 60rt 9.6 FO + 10a
33 736 10.0 P3 - 4.3c 29 663 10.3 Al + 32b
30 589 10.0 Al + 25b 31 692 8.6 AO + 7b
32 683 9.1 A + Ea 31 694 9.8 AO + 15b
31 667 1040 A2 - 17c 33.76b 10.1 Al - 30b
~1 669 8.9 AO Oa 30 611 10.1 A5 +206
33 741 9.8 AO - 2c 32 711 9.9 A3 - 34,c
31 670 8.5 AO 0a 30 614 9.4 A2 - 26a
33 743 9.8 A4 + llb 32 717 9.8 AO - 32b
32 690 10.7 A8 + 321c 32 718 10.1 A3 - 21b
32 691 8.6 B8 - 26a 31 705 9.1 B8 + 23a
32 695 9.0 A3 - la
The table gives: the number BD., the photographic star magnitude.,
the spectral class and the relative radial velocity of the star. The
spectral classification was made by taking into account the data'in
source (2). The values of the star magnitudes were taken from
catalog (source 3) or eatinated visually, based on the density tithe
spectra on .he negative.
The indices ay b,, and c d,tsignate the quality of determInation
of velocity; the index a designates stars for which the mean error in
determination is 17 k"i s the index b designates measurements with a
sec
mean error of ? 9 km , while the index c designates the radial veloc-
sec
ities for which the errors constitute 113 Sc .
With the aid of steers B) + 310649? BD + 3loeO and BD + 30?582,
for which the radial velocities are kaowm (4), we determined the cor-
rection for the conversion of the relative radial velocities (the data
in the tale) into absolute values* MU correction was equal to
+14 +_8
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Literature Cited
(1) Kiladze, R. I., Experiment for the Determination of the Radial
Velocities of Stars by Use of an Objective Prism Placed Before
a 70-cm Meniscus Telescope, 13u11? of tpL Abgt,tman. Aetrofiz.
.r No. 24 , 195 (2) Cannon, A. J., and Pickering, E. C., The Henry Draper Catalog
Annals of the Aetron. Obs. of ALVMEA d e Vol. 91, 1918.
(3) Hillo-S . J., and cailt, J.~ Photographic Utgnitudea of 55,700
Stare in the Zones + 100 to + 200 and?+ 30 to + 500, Contr
(4) W on, R. E., General Catalog of 8tel a.r Radial Velocities,
Pavers- of Mount Wilson OboeNvat Vol 8, 1953.
("Determination of the dial Velocities of Stars by Use of a 70-cm
Meniscus Telescope and Large Objective Prism," by R. I. Kiladze,
8oobehcheniya Akademii Nauk Gruzinakoy SSR, Vol. 23, No. 5, 1959,
pages 535-539) (/
StUdY_ CC IInt lanetary Ion zed Gas. )tigh-Ener Electrons ands
p_ueeular ftdiation of t2_un by the Second Soviet Cosmic Rocket
.Experiments with a three-electrode trap fag' charged particles
were made on the lot, 2d and 3rd Soviet cosmic rockets. The most sta-
tiotically valuable data from the experiments in question (about 12,000
int'.ividual measurements of collector currents) were received during the
flight of the second cosmic rocket. Therefore in the article that fol-
lows we essentially set forth the data for the second rocket. The vol-
ume of information derived about the operation of the three-electrode
traps on the 1st cosmic rocket was subetantial]y less; the data from
the automatic interplanetary station (3rd cosmic rocket) is presently
only partially processed. Nevertheless, considering the importance of
the observed recurrence of the results, we will give below individual
citations to the data derived during the flights of the 1st and 3rd
cosmic rockets.
On the Soviet cosmic rocket launched to the Mocx on 12 Septem-
ber 1959 an experiment was set up for the study of interplanetary
ionized gas, electrons with the energies W greater than -200 ev, and
the corpuscular radiation of the Sun. With the assistance of a radio-
telemetric system at the time of tba flight we recorded electrical
currents created by the charged particles falling into traps set in a
container separate from the. rocket with the scientific apparatus. On
the surface of the container there were four three-electrode traps,
situated at the corners of a tetrahedron inscribed in a sphere. Each
trap consisted of a hemispherical outer nickel grid (with a radius o
30 nom), within which there was a f3at'nickel collector. Between the
collector and the outer grid there was a flat wolfram inner grid.
The potentials of the electrodes of the traps relative to the body
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of the container were s the ~c co3.3aotcrw . - (60 s 90) v, inner grids
1 ? - 200 of the outer grid b~ the following potent. ais y.2 re-
s actively: - 10j - 5; 0 and + 15 v (see figure 1).
The basic purpose of the inner grids was the suppression of the
phat;oefteat from the collectors, arising under the influence of ultra-
violet radiation Pram the than, and also the suppression of seeoodary
electron emission due to the baabardment at the collectors with else-
trots and protons. The outer grids of the traps were given different
potentials in order to make it possible to estimate the energies of
the positive particles entering the traps and, in particular, in order
to distinguish the currents which can be created by the protons of in-
terplanetary stationary plasma (with energies on the order of 1 ev)
from currents created by the protons of eaa'pucular currents hating
energies 3 orders greater. The electrons at the stationary plasma
(with energies to 1 ev) and of solar aarpw cu3ar currents (with ener-
gies up to 25 ev) do not play a role in the establishment of collector
currents In the traps, since they cannot overcase the retarding field
created by the difference in potentials between the inner and enter
grids (equal to N - 200 Y). The electrons moping in the Earth's mag-
netic trap (In the so-called outer radiation belt), hating sufficient
energy to overcame the retarding field between the' grinds of the trap,
can create a negative collector current.
It shailA be barge in mind that the negative collector current
is also created by part of the phatoelectrons emitted by the inner
grid during its 311umination by the Bun and which enter the collector
under the influence at the electrical field between the grid and the
collector. If the trap is not illuminate3 by the Sun (and the traps
were situated cc the container in ouch a way that at least one of
them was alvay. in the sbadow), the negative current can be created
only by high-energy electrons held by the geoaagnetic field.
In the selection of the characteristics ton the apparatus the
following models warp. taken se the mast probable models of inter-
planets-ry gases (in accordance with data existing in the literature.,
sources 1-3). A. There In a stationary gaseous medium consisting
eeeenrtially of iarixed bLvdrogea with a concentration of ni ^
5 ? 102 s 103 cm-3, with an electraa temgperature on the order of
104 011, close to ix ten earature. B. Mrere are only sporadic cor-
pus ru3sor currents, r.Q isting c 1r4rtans end electrons with veloci-
ties cf (1 f 3) ? 146 cm ? sec-1 and with coccentrations of ni son
1 s 10 cm-3. We a1oo bad in misxt the possibility of a case C --
the simultaneous existence of A and B. It was expected that in case
A there would be expected a de=ease in the value of the collector
cts Ik with an ?1z aaae of p and an absence of positive cur-
rents I,, vhen PP a + '! 5 v. In t . cue B the pceitiv~e values of 1k
should be 1A eutcai independent of the value, of p . In the case C
positive 9sluee of Ik shuxz1d be observed in all t traps, but . de-'
crease with an,increase in pge.
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The arplifiers of the collector currents, and the telemetric
system make it possibly to record positive collector currents from
10-10 to 50 ? 10-10 a, and the negative Collector currents from 10-10
to 15 ? 10-10 a. The inatantaneoua values of each collector current
were recorded twice each minute.
While moving along its trajectory, the container with the sci-
entific apparatu2 a,imultaneoualy nude complex.rapid rotational move-
ments. Due to this factor the orientation of each trap relative to
the velocity vector and directir:. to the Sun changed continually;
this caused correopondin variations in the. collector current (see
Figure 2). The riaximtua (like the minimum) values corresponded to
certain orientation of the container that were close to one another.
Therefore changes In the value of Iic along the trajectory, depending
pr nmril j on the surrounding medium,, can be described by means of
curves enclosing the maximum and minimum values of X. In this case
the influence of rotation of the container on the results of the ex-
periment can to a certain degree be excluded.
In a similar way, Figure 3 shows the experimental results in
that part of the trajectory up to 75 ,000 kilometers from the Earth's
surface and Figure i. shows the results beginning at a distance of
25,000~kilometers and lasting to the falling of the container on
the )loon.
The absence of similarities in the variation Of the curves in
Figure 3 is evidently due to peculiarities in changes in the orients-
Von of the different traps relative to the velocity vector of the
spherical container and is associated with their different positions
on the surface of the complexly rotating container.
At CP-15 hours Moscow time on 13 September 1959 when the ccr_-
tainer was situated at a distance of R x 190,000 kilometers from the
Earth, radio communication between it and the territory of the USSR
was disrupted beca:uie at that time it Iias over the Western Hemisphere.
After the restoration of communications the character of the recorded
collector currents had changed and before the end of the experiment
was as indicated in the last part of Figure 4.
An examination of the cited experimental data shows:
1. At distances R from the surface of the Earth to 4 earth
rrAdii there is plasma with a temperature of no more than 10,000 de-
grees. This follows from what we can see clearly in Figure 2 -- the
substantial influence of relatively small (5v) differences in the Po-
tentials of the outer grids of the traps on the values of the col-
lector currents and from the absence (at distances of R ) 3,000 kilo-
meters) of a current in the trap with the positive potential in the
outer grid. The existence of plasma at the indicated distances from
the Earth is confirmed by the results obtained by the lot cosmic
rocket in January 1959 and by the 3rd cosmic rocket in October 1959.
(In the latter case to 7,000 kilometers, since at that distance the
first period of communication with the interplanetary station ceased.)
16
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Problems associated with eatimatau oi' the concentrution of t;ar= plasma
which we discovered here and t:'iso tlaa Nofvciblo concentration of inter-
planetary planma (with large values of B)., go beyond the limits of
this present paper and will be examined separate 1 .
2. In t.'..? < .'. < '%F;,OCU :C1~.r the instruments
and method of measurements see (8)).
In the course of these soundings the cbant a in wirte::oity of
the electrostatic field E With height B :tae measured. The potential
of the corresponding point was computed by mmeam a of integration of
the experimental curve E ? f (8). It must be taken into account that
a basic part of tLe reesistewce of the atmosphere is concentrated in
its lower layers (4), Thus, in the o?.6 km layer there is concentrated
about 66% of the total resistance ue the atmosphere; it may therefore
be assumed that the potential at a height of 6 km ohoulll not essen-
tially differ from the potential of the ionosphere -- by no more than
30-35%. Therefore changes in potential at a height or 6 ton should be
eanentia13y similar to changes in the potential of the ionosphere.
Disruptions of thin similarity can occur because of dev. ations at at-
mospheric conductivity from their ".t( I" values. Since these devia-
tions for the moat part occur in the 0-3 s 4 lan loser end usual3y lead
to a decrease in conductivity, the ccr*uted values of the potential of
the ionosphere may prove to he somewhat higher (1+).
The proceoning of data for these measurements gave the follow-
ing results :
26
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CPYRGHT
P?PInRi
Or
41 '
P- %WS
.~t!'ap 4om 10'" 10"' 1I "!G'" Z17"' 10 "Y?"UO"'1Y1'" 4!l"' ~7"p7"'Z!?"' 40"' P! A7'"117'" 40"'
Fig 3. Timc-bust chanaou of the signal oxcludinS the effect
of distance.
a --12 September to 13 September 1959; b -- 13 to
14 September 1959
("Radioaotronomical Obeervationo of the Second Soviet Cosmic Rocket,"
by V. V. Vitkovich) D. Kuz'min, R. L. Sorochenko, and V. A.
Udal'toov, Doltlady Akademii Nauk SSSR, Vol. 132, No. 1, 1960, paSeo
65-88)
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1) The monotonous pattern of change of field intensity with
height in often disrupted, even on clear dayn. Together with an ax-
ponential decreace frith height II of the field 1 , j.,, e-ad (a changes
from 10-3 to 1,5 ? 10-3, if' H iu Waatued in :.xiterfig, a number of
cones are encountered when at name height (moot corcnon3y 1y000-
4,000 m) the intensity of the 'ic3d. dr'o;~)c; to z. o cu.' bemk's steadily
negative. Cacao are observed when tlv., e is n3tuou : no clir""ge in the
electrical field with height -- it maintaiua valueu ol.' C.25 to 0.35
V/cm to great heights. There is a pattern o,C vwr{t:,tton ~.n the field
in which the intensity has a maximum Gt a heiClit of several hundred
meters to several Icilometern, usually situated under the boundary of
a temperature inversion (9). Above the intensity maximum the sign
changes and it becomes negative.
2) The monotonous increase in potential with height is often
disrupted even in clear weather.
3) The most probable value of the potential at a beig1 t of
6,000 m was less than expected. As can be seen from Table 1, it lien
within the limits of 320 to 160 kv; the moot probable value of the
potential in the ionosphere is therefore about 200-250 kv.
4) The diurnal changes in potential at a height of 6,000 m
moot commonly are not similar to "unitary variation" but are differ-
ent for all three points of observation at one and the same time
(Figure 2A.). Relative variations in the potential in the course of.
a day at heights of 300 to 6,000 m have a tendency to decrease with
height- Minimum IUriations in the potential are often observed at a
height of 3,000 to 4,000 m. Higher aloft the relative variations of
the potential often increase again. A shifting of the maximum with
height (Figure 2B) is often observed in the diurnal pattern of the
potential at different heights. The "Unitary variation" of field
intensity appears rather clearly (Figure 4) at heights of 200 to
300 m (at Leningrad and Kiev). It begins to fade out above and be-
low, and the maxi 1J2 of the curve begins to shift.
Our experimen':s therefore did not confirm the model of a
"spherical capacitor,''
We can interpret the derived reoul',;s if we change from the
model of a "spherical capacitor" to the model of a charged sphere
surrounded by a space charge. Since there is a "unitary wave"
(5-7) at the Earth's surface in the po3ar, mountain and oceanic
regiena, and since there is a good correlation between the "unitary
wave field" and the d1luml pattern of tbunderatarms activity over
the entire globe W., it may be assumed that the currents flowing
on the Earth in regions with a thunderstorm mart a charge to the
Earth a, - d the diurnal jettern of field intensity new' the Eartht s
surface is, in essence, the pattern, of density of the Barth's sur-
face charge in areas where it is not disrupted by local space charges.
The Earth is surrounded by a apace charge whose field Is super-
imposed oar the field of its surface charge and its variations "smear"
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the variations of the "~tnitary varirtttor"; therefore the variations
of the potential at various heights in caunerl by the distribution
and value of the apace charge in tho atmosphere. 1 ho apace charge
in the 3 to 4 loo layer is often already such that its field capacity
completely compensates the field of the Earth's surface charge.
If we subtract the intensity created by the Earth's own charge
(E unitary) from the measured intensity of the fields then in the
first approximation we can delimit the field caused by the apace
charge of the atmosphere. Figure 3 shows an exam',tle oe ouch an
analysis. As we can see,, the variations of the measured potential
even under undisturbed conditioa:a essentially duplicates the varia-
tions of the potential caused by the apace charge of the atmosphere.
The entire globe can be divided into three regions:
I -- a region of generatiai of the space charge. We must in-
clude here all the regions covered by clouds; the, profile of the elec.-
trical field in these cases is usua3.y sharply disturbed.
II -- regions where the monotony of the change in intensity of
the electrical field with height is disturbed by t1w space charged
introduced from Region I. Included in these aacieri are profiles di-
verging from the exponent. This type of profile depends on the value
and distribution of they charge in the atmopphe:.:i , coliuvn.
III -- regions when? the spa^.e :c. the entixe atmospheric
column is small and does rot e.xerciap s. a;i~-~ ;~wi;.'~:1. i.nfl. wrtce on the
field of the Earth's surz)ace charge. There rshot1'ai be a "unitary vari-
ation" is these regions, both at the Farth'a surface and aloft.
The fact that "unitary variation" is observed in "disturbed"
regions (type region II) orly at certain hel ht,i; 200-390 m) (Fig-
ure 4) is due to the fact that the field of space charges situated
above and below this level (co fIeniugrad) coupeiate one another,
permitting the field of the Earth'a own ckinxge to appear in pure farm.
Experiments in the sounding of the electrical field of the at-
mosphere have therefore not confirmed the theory of a "spherical ca-
pacitor." Judging by the results of these measurements, it is obvious
that it in better to c1Bnge over from the model of a "spherical ca-
pacitor" to tke model of a charged sphe_e., 9t=r a"de3. by a space
charge. In order to mcme seriously suppoc1 -this model., we have need
for continuing study of the beha rLor of the space charge in the at-
moophere., the conditions under which it is ganerat~al and diffused.,
and its distribution in the atmosphere.
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 CPXERM,Te i Far Release 1999109108 - CIA-RI11287-00141 R000901930001 -6
ltitble 1
8sapnu OF TAZ $ Cr P03'DTTAL AT A U3DR a? 6,000 BnW *11958
CE T iu03M OT ==)o 8 ElmM OF 6,000*,. IV V
. ICNOOP XPPTBTL + 400 KV
~u
(~iue ab i ~}
z
1
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o 0 4a?
L?
n-
7auhlmt
'cka :p~p~,aib~?}
2
6
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32OaO
5
5
1
0
8 26
#7 32
4 10
200? 0
38
21
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2400
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36
23
.22
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2he2tjorat (
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35
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3
280j SO
320=
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36 o
- 400o
4ntngma
110
8
5
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.fir
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Slluhlaalt (Nxrch i Se ear)
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4g'48b
20
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TUhk eat (*xtah & Bsptulbw)
].
11
?29-
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 CPYRGHT
pproved For Release 1999/09 nt?VAt.RRfN2-00141 R000201230001-6
/~/~ M1
4 0 11 111'1\~I~il.Ntt
} MMMMM1M
I ~ yM
MM
~it5 Yariation of ,the electrical potcnti4.1 witn altit.ude
I ,-,I,~nin rad, 1958 (0 cuicente); II--Kiev, 1958 (50
aueont );,, .'IZT.-?.Tauhkcbt, 1953, (50 ,aupltu).; ..GDntinuouu
Curve-