SCIENTIFIC ABSTRACT BARABASHOV, N. P. - BARABASHOV, N. P.

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• Collection: Scientific Abstracts
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• Document Release Date: June 9, 2000
• Sequence Number: 12
• Publication Date: December 31, 1967
• Content Type: SCIENCEAB

Venuoq Unmaskl
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paper succeeded in observing a reflectiong which is probably
due to the presence
of large bodies of water as well as of ice crystals in the
clouds enveloping
Venus. Large amounts of carbon dioxide and small quantities of
oxygen as well as
a relatively high temperature suggest that conditions on Venus
resemble those
having prevailed on the Earth during the Carboniferous.
Possibly life on the
planet is now commencing, or some as yet unknown forms of life
are present on it
now. On page 17 A. G. Maseviah, Doctor of Physical and
Mathematical Soienoeaq De-
puty Chairman of the Astronomigql Council of the AS USSR,
discusses the questiong
which of the planets, Venus or'Alars is of greater significance
for humanity.
In his opinion it would be posi-ible for scientists to discover
such conditions
to prevail on Venus as would give this planet the top place
regarding its signi-
ficance for mankind. There are 6 figures.
ASSOCIATION: Planetnaya komissiya Astronomicheskogo soveta AN
USSR
noil of AS UkrSSR)
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AUTHORS: Barabashov,,L.4 .Koval', I.K.
TITLE- Some Results of Studies of Contrasts on Mars
PERIODICAL: Astronomicheskiy Zhurnal, 1960, Vol 37, Nr 2, PP
301-305
(USSR).
ABSTRACT: It is well-Imown that the continent-sea contrast K
for
Mars has a maximum value in red and a minimum in blue,
According to measurements carried out by the present authors
in 19 56 5; K = 0. 286 f or =. 647 mVL, and K = 0. 0'7 f or
?Lm;a = 420 mp.. However, occasionally, the contrast in blue
light reaches 80% of the contrast in red light. Usually,
this is explained by increased transparency of the blue
atmosphere on Mars. If one accepts the explanation that
the true contrast is the same for all wavelengths and the
apparent contrast depends on the state of the Martian at-
mosphere then one can try and estimate the optical. thick-
ness of the Martian atmosphere in blue light from the
Cardl/3 corresponding contrast, For this purpose it is assumed
VC

S/033/60/037/02/009/013
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Some Results of Studies of Contrasts on Mars
that K. = const and the red contrast is taken to be
approximately equal to the true contrast, since the optical
thickness of the atmosphere in red light may be taken to be
approximately zero. The present paper is concerned with a
critical examination of the possibility of an explanation
of the variation in Kblue by variations in the optical
thickness. Fig 1 gives the values of the contrast for
red, green and blue rays (curves 1, 2 and 3 respectively)
for June, July, August and September, 1956. These data
refer to the central regions of the planet, Fig 2 gives
0
the corresponding plot for the ratio
Kblue/Kred for the
same observational period. Another characteristic Considered
is B = Pi(l - Kred/Kblue) where ?I is the albedo of the
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Some Results of Studies of Contrasts on Mars
continent and B the brightness of the 'atmaphere above
the region investigated. Fig 3 gives t plotted as-a
function of time. Fig 4 shows the curves for the southern
polar cap in red and blue light. All these data indicate
that the variations can best be explained by different
energy distributions in the spectrum of each "sea" sep-
arately. The most probable explanation is that the diff-
erences are due to spectral properties of the surface of
the "seas", and that the optical thickness of the Martian
atmosphere in red, green and blue light is small, and
that it is mainly a scattering atmosphere. The fact that
the blue atmosDhere of Mars is optically thin is also in-
dicated by the curves for the southern polar cap shown in
Fig 4. which are virtually parallel to each other. There
are 4 figures.
a)
ASSOCIATION: Khar1kovskaya astronomichesk a observatoriya
Card3/3 (Khar1kov Astronomical Observatoryl
SUBMITTED: November 22, 1959.

. - - J~ 8184:~
t.7 AS-~5-0 ~�/033/60/037/03/011/027
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AUTHORS: Barabashov U& N.-P, and Gara a I -Vr-1
TITLE: Some Ideas About Dust and Mist Formations on,Mars
PERIODICAL: Astronomicheskiy zhurnal, 1960, Vol 37, Nr 3,
pp 501 - 507 (USSR)
ABSTRACT: An attempt is made to explain some of the
properties of
tho mist and fog which frequently appeared on Mars during
1956 and ]~-ersisted over considerable periods of time,
particularly during September and October. Data reported
by Barabashov and Koval' (Ref 1) are employed in the
analysis. The conclusions drawn from these results are
as follows:
1) the Martian surface is covered by very small dust
particles whose dimensions do not exceed 0.01 - 0.1 mm.
2) Martian dust clouds apparently consist. of even finer
particles.
3) The fog which occasionally appears in the Martian
atmosphere is transparent to infrared and red radiation
but is entirely opaque in the ultraviolet.
4) The dust particles are rarely found in the upper
Cardl/2 layers of the Martian atmosphere. Vr

81847
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Some Ideas About Dust and Mist Formatio s oa'Aars
5) The difference between the albedo of the "continents"
and the 11seas" has a maximum in the green.
6) The law of reflection from the Martian surface, or
from the low-lying clouds near it, is close to Lambert's
law.
7) The yellow fog appears to consist of particles having
the same (or smaller) dimensionsibm those covering the
Martian "continents".
There are 9 figures, 5 tables and 3 Soviet references.
ASSOCIATION: Kharlkovskly astronomicheskaya observatoriya
0~harlkov Astronomical Observatory)
SUBMITTED: January 16, 1960.
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ZEN
,ZARABASM. q akademikj- ARZUYANOVA, N.A., red.; RO I
,~2ay
B.A., tekhn. red.
(Venus) Venera. Moskva..'Izd-vo "Sovetskaia Rossiia,"
1963.. 38 .
(MIRA 14:105
1. Akademiya nauk USSR (for Barabashov).
(Venus (Plamet)) (Space fligbt to Venus)

BRONSR=p V.A.)--kARABAMOV V kadomik I otv. red.;
KOLOKOLINIKOV, X.A.9
j__J,4 a
tekbn. red.; GOLUBk, S.F.p tek1m, red.
(Atlas of drawings of Mars] Atlas rim2nkov Mersa.
Moskva, Izd--4
Akad. ndOt SSSRp 1961. n? p. - (KMA -14110
1. Akademi7a neuk USSR (for Barabas4q'v)
(Mars (Planet))

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AUTHORS- Barabashov N P Koval', I. K., Chekirda, A~.. T.
TITLE: Photometric studies of Mars in 1958
PERIODICAL: Referativnyy zhurnal, Astronomiya i Oftdeziya, ri?.
6, 1962. 63,
abstract 6A469 ("Izv. Komis. po fiz. planet". 1961, no. 3, 3-15)
TEXT: The authors present data on distribution of brightness
along the
intensity equator and central meridian of Mars, obtained on'the
basis of photo
graphic observations of the planet with light filters. Moreover,
the data are
given on contrasts between light and dark regions, as well"as on
brightness
variations of the Martian northern and southern polar regiops.
'~ 11-4
Au st summary
[Abstracterts note: Complete translation)
L
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36619
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3, ), so AOO%&Ol
AUTHOR: Brarabashov, N. P.
TITLE: On changes in brightness of lunar formations as a
function of
azimuth and on sections of lunar indicatrices
PERIODICAL: Referativnyy zhurnal, Astronomiya i Geodeziya, no.
6, 1962, 64,
abstract 6A480'("Izv. Komis. po fiz. planet", 1961, no. 3, 31 -
40)
TEXT; The autlior investigates the dependence of brightness of
lunar objects
on the difference in azimuths of incident and reflected beams.
The effect of
azimuth difference is shown. Sections of indicatrices for i =
30 and 600 by planes
perpendicular to the incidence plane and passing through the
incident beam are
presented. Th.e conclusion is drawn that these investigations
confirm still more
the statement on the uniformity of the lunar surface
microrelief; moreover,
changes in brightness of lunar seas and continents as a
function of changes in
azimuth difference agrees rather well with data for crushed
tuff whose grain size
is equal to 2 - 6 mm. There are 5-references.
. Author Is summary
[Abstractex~ls note: Complete translation]
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S/035/62/000/006/039/064
C) A001/A101
AUTHORS: Barabashov, N. P., Yezerskiy, V. I.
T=: Spectrophotometric observations of lunar craters
PERIODICAL: Referativnyy zhurnal, Astronomiya 1: Geodeziya, no.
6, 1962, 64,
abstract 6A482 ("Izv. Komis. po fiz. planet", 1961, no. 3, 50 -
55)
TRXT: The authors present the results of spectr6photometric
observations
of the Alphons crater and other -craters at the KharIkov
Astronomical Observatory
in 1958 - 1959. No anomalies were detected in albedo of
individual sections of
the lunar craters, including the central peak of the Alphons
crater. There are
b references.
Authors' summary
[Abstracter's note: Complete translation]
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0
AUTHOR: Barabasho , N. P.
TITLE: The structure of theilloon's
Dhoto,-raphs of its far side
3~2 7 14
S 560/61/000/009/004/009
D045/D1l4
surface and investigations of the first
SOURCE: Akademiya nauk SSSR.'! Iskusstvennyye sputniki Zemli.
No. 0~1
Moscow, 1961, 56-61 1
TEXT: The article deals with the structure of both sides of the
Moon. As
reGards the 146on's visible side, the author quotes several
well-known theo-
ries on its si,ructure. On comparing terrestrial rock strata
with the Moonss
surface, only~!tuffaceous rocks and volcanic ashes resembled
lunar strata.
InvestiGations, by several Soviet scientists indicated that the
degree of
pitting on the lunar surface was so high that ordinary Earth
rocks, with the
exception of highly-porous tuffaceous rocks, bore no resemblance
to lunar
rock strata. A comparison of various artificial surfaces with
lunar observa-
tions showed that (1) the greatest similarity is obtained with
surfaces covei,
ed With parallel cracks and sharp irregularities, and (2) fine
dust evenly
coated over a uniform surface cannot produce the effects of
light reflection
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The structure of the Moon's surface D045/11114
observed on the Moon. Judging by investigations of the
photometrical uni-
formity of lunar details, it was concluded that, largely the
lunar surface
is photometrically homogeneous. However, it can be said that
the continents
are, on the average, redder and more porous than the seas.
Theoretical
studies and investigations on granulated tuff conducted at the
Kharlkovskaya
astronomicheskaya observatoriya (Icharlkov Astronomical
Observatory) showed
that the Moon's surface may consist of hiahly porous tuffaceous
rocks$ p'.0sc-
sibly highly-granulated with grains 1-6 mm in size. N. No
Sytinskaya kRef"
11: Izv. plan. kom., vyp. 1, KhGU, al, 1960) proposed that the
irregularities
conditioning the lunar microrelief are 1-10 mm in size. Turning
to the
structure of the Moon's far side, the author discusses the
preliminary re-
sults of studyin.- Dictures taken by the Avtomaticheskaya
mezhplanetnava
stantsiya (Automatic Interplanetary Station) (AMS) on October
7, 1959, On
this side of the Lloon, there is a predominance of mountainous
areas and few
seas like those observed on the other side. A fairly large
crater sea, the
"Sea of Moscow", was discovered. It is nearly 300 km in
diameter and is
located between latitudes +200 and +300 and longitudes � 140 0
and � 160
In the"Sca of Moscowfta bay, called the Buy of Astronauts, was
noticed. The
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The structure of the Moon's surface DOWD114
entire area of the Moon's far side, bordering on the western
edge, has an
albedo between the albedo of the mountainous areas and that of
the seas of
the visible side. In the southern hemisphere of the Moon, a very
large
crater called Tsiolkovskiy is very clearly marked. This crater,
more than
100 km in diameter and located at -200 to -300 latitude and +300
longitude,
has an exceptionally dark floor and an extremely bright central
peak -
briGht enouE;h to suggest that it itself emits light, and
possibly luminesces,
A bright band consisting of craters ard mountains stretches to
the south-east
of the Mare Humboldtianum. This band, broken in places by darker
spaces, is
like a mountain range, stretching for almost 2000 km, A very
bright band,
similar to a light ray, stretches in the same direction. The
results of the
treatment of photo material at the Khar1kov Observatory are as
follows: All
details, found in the first stage of treatment, appeared to be
completely
genuine; new craters were found and the borders of several seas
specified.
The final results of combined treatment by the Gosudarstvennyy
astronomiche-
skiy institut im. Shternberga, (state Astronomical Institute im.
Shternberg),
the Glavnaya astronomicheskaya observatoriya (Main Astronomical
Observatory)
in Pulkovo, and the astronomical observatory of the Kharlkovskiy
gosudarst-
ve-,-:nyy universitet (Khar1kov State University) are entered in
the "Atlas
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The structure of the Moon's surface D045%114
obratnoy storony Luny" (Atlas of the Moon's Far Side) (Ref. 17;
Izd-vo AN
SSSR, 1960)o More than 400 details were identified. The
following co=la-
sions are drawn: (1) the albedo of many areas of the Moon's far
side has
a considerably greater reflecting power; (2) the floor of many
craters on
this side is very dark and similar in darkness to the darker
areas of the
visible side; (3) preliminary studies show that the porosity of
the surface
of the Moon's far side is the same as, if not greater than, the
visible
and that the brightness on the surface of the full Moon seen
from the A1JS
i3 distributed almost in a straight line. The following
personalities are
mentioned: L. N. Radlova,A. V. Markov, N. S. Orlova, Vs Io
Garazha, Aj To
Chekirda, V. A. Pedorets, V. V. Sharonov, V. Ao Yezerskaya, V.
I. Yezerskiy,
and T. A. Ishutina. There are 19 references.- 14 Soviet-bloc and
5 non-
Soviet.-bloc. The three EnGlish-language references are.- L.T.
llinnaert~
Astroph. J-, 93, 403, 1941; J. H. Trexler, Proc. IRE, 46, 2a6~
19585 J, V"
Evans; Proc~ Phys. Soc-, B70, 1105, 1957-
SUBMITTED: September 15, 1960
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01
BARAWROV, M.P.p akademik
To the nearest planetse Mailke i zb;y-ttia Il no,60-10 Je
161*
- (KMA 14.-7)
III-AN USSR (Khartkov).
(Astronaution) Maneta)
~.a

40462
S/035/62/000/009/028/o6o
-)Sod A001/A10l
AUTHOR:
TITLE; on the microrelief of the lunar surface
PERIODICAL: Referativnyy zhurnal, Astronomiya i Geodeziyd, no.
9, 1c,162, 68,
abstract '9A48i ("Tsirkulyar Astron. observ..Khartkovsk. unt-t",
ig6i, no. 23, 3 - 14)
TEM. To represent the brightness distribution over the lunar
disk, a mock-l!
of the surface structure is employed which consists of
unevennesses of two orders.
Tbe microrellef of the first order, in which unevenness amounts
to several milli-
meters, is superimposed by thr-, microre lief of the second
order consisting of venj
small particles. On the basis of comparing indicati7ices of
light reflection by Vie V\
iunar surface, obtained from observations, with experimental
data and xilculatiuo:-
for various models, a conclusion has -been drawn that the best
agreement is achievc-c
with a surface of porous tuff, covered with prismatic terraces
whose height is
times as great as their width and separated.from each.other by
distances equal t .o
this height.
[Abstracters's note: Complet6 translation] 1. Lebedeva
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41817
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E032/E114
AUTHORS: Barabashov, N.P., and Garazha, V.I.
TITLE: on i-he microstructure of the lunar surface
SOURCE: Khar1kov. Universytet. Astronomichna observatoriya.
Tsirkulyar. no.24, 1961, 3-13.
TEXT. In a previous paper, the first of the present *authors
showed that 8ome of the photometric prope'rtiee of the lunar
surface
can be reproduced by assuming that the lunar surface can be
represented by (a) infinitely deep cracks with vertical
walls, or
(b) discontinuous prismatic formations whose.surfaces are
smooth
and reflect light in accordance with Lambert's law. However,
these
models do not account for somix other photoinetric
properties, for
example, the uniform distribution of luminance along the
intensity
equator and the centra-1 meridian at full moon, and certain
other
effects. A better representation of the light-reflecting
properties
~f the. lunar surface can be obtained by assuming that the
faces of
the irre-gularities consist of porous tuff with its own
specific
reflecting properties. It was then concluded that the micro-
structure of the lunar surface consists of two reference
surfaces
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.0
On the microstructure of the S/835/61/000/024/001/002
E032/Ell-
with irregularities of two different orders of magnitude,
namelyl
second-order irregularities characteristic of the material of
which
the rocks forming the lunar surface is made, and first-order
irregularities which are larger pores or bumps (of the order
of
n
i L
illimetres) which are associated with cracks, meteorite
impacts,
and so on. in the present work this investigation was
continued by
considering the reflecting properties of various geometrical
configurations such as regular arrays of prisms, pyramids and
so on.
Detailed numerical calculations showed that all the observed
reflecting properties of the lunar surface can be reproduced
witb
the aid of a niodel in which the surface consists of volcanic
tuff
which is covered by square cells of side equal to 1 m, wall
thick-
ness of 0.20 m, and depth between 1.5 and 2 m. Since the
appearance
of square cells can hardly be due to natural causes, the
analysis
was extended to cover six-aided cells. It was found that
neither
six-sided cells nor circular cells could be made to agree
with the
known reflecting properties of the lunar surface, and
therefore. the
presence of a cell-like structure on the moon is improbable.
The next model to consider was therefore a surface-consisting
of
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On th'e microstructure of the S/835/61/000/024/001/002
E032/E114
fragmented tuff with linear dimensions of the individual
fragments
of between fractions of a millimetre and a few millimetres.
Special specimens of fragmented tuff were prepared with various
framment sizes and their reflecting propert.ies were
determined in
the laboratory and then compared with lunar data. Such
comparisons
showed that fragmented tuff with grain sizes-between one ond a
few
millinietres has reflecting properties which are very close'to
that
of the lunar surface. Moreover, the fr~Lg'mented tuff had
similar
spectrophotometric and polarisation characteristics. Its
thermal
conductivity, density. electrical conductivity and other
characteristics were also similar to those of the lunar surface
material.
There are 11 figures and 9 tables.
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5/835/61/000/024/002/002
E032/E114
AUTHORS: Barabashov. N.P., Ivanchenko, V.M., and Chirkova,
R.M.
TITLE: Radio observations of the partial solar eclipse of
February 15, 1961, at the wavelength X 1.5 m
SOURCE: Khar1kov. Universytet. Astronomichna observatoriya.
Tsirkulyar. no.24, 1961, 36-38
TLXT: On February 15, 1961, the Kbar1kovskaya astronomiches-
kaya observatoriya (Kharlkov Astronomical Observatory)
carried out
radio observations of the solar eclipse in the 1.5 m range.
The
aim was to obtain the distribution of radio intensity over
the
solar disc and then use it to obtain information about the
nature
of solar radio emission. The measurements-were carried out
by a
compensation method using a 6 m diametdr parabolic mirror.
Toe
high frequency amplifier included the low-noise 6Hi4n (6N14P)
tube in a cascade circuit and the five-stage intermediate
frequency
dmplifier incorporated 6V,4 (6Zh4) tubes. The intermediate
frequency was 31 ~jc/s and the bandwidth was & f0-5 = 4 Me/a.
In the figure, curve II shows the intensity of solar radio
emission
as a function of time; curve I shows the ratio of the
uneclipsed
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Radio observations of the partial...
S/835/6l/ooo/oz4/oo2/002
b032/E114
area of tile solar disc to the area of the entire disc as a
function
of time. Because of unfavourable weather conditions no
spectro-
heliographic observations were possible and use was
therefore made
of data supplied by M.N. Gnevyshev of the Kislovodskaya
Gornaya
stantsiya (Kislovodsk Mountain Station). Inspection of tile
emission curve showed that a group of plages and sunspots
on the
disc was recorded during the eclipse in the form of a rapid
reduction in the intensity, which confirms an enhanced radio
emission from them. The partial eclipse at Khar1kov began at
10 hours 0.2 minutes, Moscow time. At 10 hours 17 minutes,
three
plages were covered. The region of these plages also
included
three groups of sunspots. After this the intensity remained
constant until 10 hours 47.3 minutes. The eclipse of a
central
plage which did not include sunspots apparently had no
effect on
the radio emission. At 11 hours 33.6 minutes, the western
active
regions re-appeared and there was a simultaneous increase
in the
radio intensity. If the interval between 10 hours 17
minutes and
10 hours 46 minutes is ignored, then the variation in the
radio
emission is very similar to curve I. There is 1 figure.
Card 2/%

Astronomical Council, Acadt
=y of
USSR
fl-9620- "Optics and geometry in
the matter of Saturn's rings"
-PRONDFI.M, Vladimir X., Crimean
Astrophysical
A. ,
Laboratory imeni G St-eyn ff~65- "On tbe
presence of oxygen'in the atmosphere of
Venus"
_GALMI)NOVICH, A. Ye., Physic3 Institute
izeni
P, N. Lebed;Tv. )Zs~ewy of Sciences tME, and
='MIT Arkadiy D Radio dztroncc*r Laboratory,
?. 11. Labedev, Academy
of Scientes USSR - "Observations of the
radicemission of Venus and Jupiter on the
vave of 8 mm. "
SALOWITOVICH, A. Ye., XMII-MI, ArkadLy D.,
and
XISLYPMV, A. 0. "Fadic-emission of Venus on
-�r -47
4 SALM40MVICH, A. Ye., XV4:12aN, Arkadly D.,
Ob! VA, Y-% P., and SIT.1NTMSXIY-I.. Y. -
vat,ons
vations of the redloamission of 'Venus
and jup, ter on the vave of 3.3 Cm - "
SPI01-I)NOVICH, A. Ye., and =1,4321, A. D. -
"Radiommission of Venus onthe veve or 9.6
cz."
SALOWNOVICH, A. Ye., and KUZIMIT, A. D.
"Results of the observations of radioc=ission
of Venus in 1961"
SHARONOV Vaevolod. V. Director, Astronomical
~Ob.? -~t.;U- ngr*'ad State University �961
position7- Probab-Le state of the surfacie
and
atmosphere of the planet Mars according to
photometric and coloriactric data"
IVS9BHMD%TSHIY, Bergey K., Read of the Chair
of
jkatronomY, Kiev Sfit-e University L'1961
POCL On
ti 7-
"Nature of Saturn's rings and signs of the
existpneq of a ring around Jupiter"
ILTMOKlyi, V. I., and BMWtS=, N. P.,
Director,
X~kov i~-troncaical Observator-f, Kharkov
State
University rig6o pooition7- "Optical
propocrties
of the atmosphere and surface of ~!ars
acco:,Jing
to photometric and cpectrophotometric
obscr-,rationa
carried out at the Kharkov University
Observato-r .
rt to be Pubwjt-~-,.j fcrt-ho 3.1th Thtl.
Antrc~pkmlca Sr-mgjmm, BOI&j&,j
- of Astrophyalca, Cointo-Sclonain, Belgium,
9-11 Jul jq~~2.

S/035/62/000/010/050/128
A001/AlOl
AUTHOR: Barabashov, N. P.
,TITLE: The nature of the Moon
PERIODICAL: Referativnyy zhurnal,-Astronomiya i Ge~deziya, no.
10, 1962, 62,
abstract 1OA434 ("Tr. 3-90 s"yezda astron.-geod. o-va, 1960",
M.,
AN SSSR, 1962, 59 - 66):
TEXT: This is a survey article which considers hypotheses of
the lunar
surface structure, results of modern studies of physical
conditions on the
Moon,amicrorelief of the surface, homogeneity of the surface on
structure and
color, data of radiometric and radioastronomical observations,
the back side
of the Moon according to photographs taken from the third
Soviet space rocket.
The author considersfurther investigations of the Moon by the
methods of as-
tronautics,
V. Sh.
[Abstracier's note: Complete translation]
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S/030/62/000/010/002/007
D204/D307
AUTHOR: Barabapligy, N. P., Academician
TITLE- The physical conditions on Mars
PERIODICAL: Akademiya nauk SSSR. Vestniko*no. 10, 1962, 18-25
'~sent knowledge oi Mars is briehy reviewed.'The re-
TEXT; The pr
,....ported observations of the-colors' contours, pole caps, canals
macro- and microtopography, atmosphere and clouds ard summed up.
From those and the author's own studies, it is believed that the
surface of Mars is covered with-a material similar to finely di-
vided terrestrial volcanic.tuff, limonite, ochre-and reddish sand-
stones; this material may be the same over' most of the planet, in
various stages of oxidation. The-luminance differences between the
Martian seas and continents, ahd the variations of this difference
y~ith the wavelength at which the comparison is,made are described
and discussed. Various views regarding the nat4re of the seas are
given,-concluding that these areas are less level than the conti-
--nents and that some vegetqtion may be present. Composition and
Card 1/2

8/030/62/000/010/002/007
The physical'bonditions oh Mars D204/D307
pressure of the atmosphere is treated in some detail, and data
re-
garding the surface temperatures are quoted. The author's work
has
shown the observed polar'6aps to be slightly reddish and discon-
tinuous. They are believed to be composed of frozen water and
thin
clouds. From.-cloud movements, the author calculated the wind
velo-
cities (a.few~km above the Martian surface) as 15'- 40 km/hr. The
nature of canh1s and associated seasonal changes are discussedp
the latter being ascribed to vegetation, the existence of which
is
considered proved by their studies of V. P1. Sinton, Regular
long-
term observations of the planet by a variety of methods are re-
commended and particularly the studies of the luminance ratios
be-
tween light and dark features on Mars (in the region of 0.2 -
5/u),
the radioemiBsion from Mars (at various wavelengths), and the op-
tical properties of minerals and rocks. There are 2 tableB..
ASSOCIATION: AN USSR (AS UkrSSR)
Card 2/2

ACCESSION Mt i
AR3010373 S102691631000100.81005910059
~4
SOLMCE: RZh. Astrono~iya. Abs. 8.51.424
Ba'rabashov,'. N. , P.
TITLE t On diffusion and truq absorption of light in the atmosphere
of Mars
CITED SWRCE: Tsiikulyar Astron. observ. Khablkovsk. un'-t. no. 25,
1962, 3-14
TOPIC TAGS:. Mars, atmospheric light absorption
,'':TRANSLATION: It is" shown that the assumption's of the uniform
distribution of
brightness over the Martian diso (during the solstice, when i in the
case of absence of'an atmosphere, as well as of a high surface
albedo and substan-,
tial true atmospheric-absorption are of low probability. It is shown
that in the
case of brightness distribution ovir the hard surface of Mars
described by the
.Lambert law, the true absorptiop must increase as the wavelength
shortero and
that the model with low-atmospheric thickness and reflection of
light from the
hard surface by Lambert'slaw is most probable. Bibliography with ten
titles.
..'.Card 1/2

S/033/62/039/002/010/014
E032/E314
AUTHORS: Barabashov. N.P. and Garazha, V.I.
TITLE: On the microstructure of the lunar surface
PERIODICAL: Astronomicheskiy zhurnal, v.39, no. 2, 1962,
305 - 314
TEXT: N.P. Barabashov and A.T. Chekirda (Ref. 1 - Izv.
Komis'sii po fizike planet, no. 1, 1960) have reviewed the
photometric characteristics of the lunar surface and have
concluded that the latter is very similar to tuffaceous rocks
in pulverized form. It is therefore of particular interest
to determine the geometrical structure of the surface layers
of the Moon. It is shown that by assum-ing that the surface
consists of volcanic tuff with a square-cell honeycomb
structure,
all the 1mown properties of the surface can be satisfactorily
interpreted (wall thicImess 0.20 m, depth 1.5 - 2 m, where m
is the side of the squares). However, since the appearance
of a square-cell honeycomb on the lunar surface is rather
unlikely, six-sided cells have also been investigated. It is
foui~dAjhat the latter cells' lead. to a d1sagmment with the
Card

S/033/62/039/002/olo/oi4
On the microstructure of .... E032/E314
knoum characteristics of light-reflection from the lunar
surface.
It is concluded from this that first-order irregularities on
the
lunar surface can hardly be of the honeycomb type. A more
realistic assumption is that the surface consists of a porovis
or pulverized tuff with characteristic linear dimensions
between a fraction of a millimetre and a few millimetres. To
,-rify this hypothesis the authors have carried out some
1 boratory ec-cperiments on pulverized tuff with g7-aln
dimensions
between 0.01 and 5 nAni, A detailed comparison of the results,
with the Imown photometric properties of the Moon suggests that
the best agreement is obtained by assuming that the lunar
surface consists of pulverized tuff with linear grain
dimeiisions
between 1 mm and a few mm. This is said to be consistent
-,,ritli
radar observations. There are 11 figures and 9 tables.
ASSOCIATION: Khar1kovskaya astronomicheskaya observatoriya
(Kharlkov Astronomical Observatory)
SUB]MITTED: June 2, 1961

3,7,5'00
AUTHORS:
Barabashov, N. P., Yezerskiy, V. 1.
S/035/62./ooo/o 12/016/064
AOOI/AIOl
Photometric studies of the microrellef of the lunar surface
PERIODICAL- Referativnyy zhurnal, Astronomiya i Geodeziya, no. 12,
1962, 65,
abstract 12A477 ("Uch. zap. Kharlkovsk. un-t", 1962, v. 122, "Tr.
Astron. observ.", v. 14, 5 - 78)
,TMT: This is a survey of the basic works described in historical
se-
quence, on microrelief of the lunar surface by the photometric
method. The ar-
ticle contains also data on this problem obtained by studying
polarization and
thermal properties of the lunar surface and its investigation by
the radar meth-
od. There are 79 references.
Authors' summary
[Abstracter's note: Complete translation]
Card 1/1

ACCESSION NR: AT4039417 S/2835/62/000/025/0015/0021
AUTHOR: Barabashov, N. P.; Yezerskiy, V I.; Prishlyak, N. P.
e microrelief of different sectors of the lunar surface
TITLE:, Differences in th
SOURCE: Kharkov. Universitet. Astronomicheskaya observatoriya.
Tsirkulyar, no.
25, 1962, 15-21
TOPIC TAGS: astronomy, photometry, lunar surface, lunar
microrelief, moon
ABSTRACT: To a considerable degree, the lunar surface possesses
photometric uniformi
and therefore the microrelief responsible for the character of the
reflection is also
tmiform. Only in individual cases is there an appreciable
difference, indicating a, differ-
ence in microrelief or the presence of slopes. In making a
detailed study of the photo-
metric characteristics of individual sectors of the lunar surface
it is desirable to compa3
-them with averaged data for the lunar surface. Such averaging is
possible bedause, for,
a particular value of the phase.angle, brightness is a function
only of selenographic longi
tude. The authors used graphic methods for finding the dependence
of B on -), for differe
values of ,,L . The brightness of a detail was expressed by its
brightness at full. moon.
The resulting curves of the dependence of brightness on X for
different values of the
1/.3

ACCESSION NR: AT4039417
phase angle, when put in graphic form, represent the law of light
reflection from the lunar
surface as a whole. On the basis of the dependence of B on'). it Is
possible to compute
the relative brightness of the moon for a particular phase angle.
The derived curves were
'used to determine the deviations of brightness of various details
from the curves represent
Ing the averaged lunar- surface, the deviations being expressed by
the relative value.611/33,
!i where Is the deviation, with sign taken into account, and B is
the brightness. value froll
the curve for the corresponding value of The character of the
dependence of 4:~, B/B
of individual details on phase angle was then investigated. A
considerable number of de-
tails were found for which the value A B/B and the dispersion -+*
are small andAich r
e
present a photometrically averaged moon. The condition was
A_B � e < 0. 15
B
satisfied by 67 of 164 details (about 40%). Of these, 29 were
sectors in seas, constituting
54% of the,total number of details in the seas. The similar
relation for continents and
craters was 26% (25 out of 94 details). The above condition was
also satisfied by about 50%
of the bright rays and bands. . There w6re a number of details for
which the value a B/B
was positive, equal to 0. 2-0.3 with a relatively small dispersion;
these details are listed
in a table; all are craters or continental regions. ,Another table
lists details for which
brightness was systematically less and the value. 6B_7B___had a
negative sign with a rela-
tively small dispersion: those details include both continental and
sea areas. The authors
2/3
Caed

ACCESSIONNII: AT4039417
anterpret these photometric differenct6s-. "In c6nelusion the
authors,.thank M. K.* Kapinus
t
:and L. 1. Yefimova who performed some of the computations for
this study". Orig. aft.
:has: 6 formulas, 2 figures* and 4 tables.
It
!ASSOCIATION: Astronomichoskaya observatorlya Eharlkovskop
universite-ta
:(Astronomical Observatory of Kh4rqcov University).
SUBMITTED. 00 DATE Aft 2~J=64 ENCL: 00
SUB FODE: AA .NO'REF.SOV: 007 OTHER: 002
3/3
cwa

... ACCESSION Nit: AT4039416 S/2835/62/000/02510003/001C
AUTHOR: BR!a~rabash~N-~Pq
TITLE: Scattering and true absorption of light In the Martian
atmosphere !;6
SOURCE: Kharkov. Universitat, Astronbmichaskays observatorlya.
Tsirkulyar. no*
25, 1962, 3-14
-Martlan atmosphere, light absorption, light sc
TOPIC TAGS: astronomy, Mars, atter-_
i
Ing I%
ABSTRACT: The author demonstrates the Improbability of the
assumption of a unp-
form distribution of brightness on the Martian disk, in the case of
either the
absence of an atmosphere, a high surface albedo or significant true
absorption 'in
the atmosphere. it also Is demonstrated that, In the case of-a
brightness distri-
bution on the solid surface of Mars described by the Lambert law,
the true b-
sorption would Increase with transition to'the short wavelengths,
so that a model
with a low atmospheric optical density and light reflection from
the solid :urface',
In accordance with Lambert's law is most probable.. There Is a
basis for believing,
that the Martian atmosphere, at least In thevisible region of the
spectrum, pos-
sesses mostly scattering properties. The decrease'In contrast often
observed in
e short-wave part of the Apectrum can be attributed to the
appearance of.extreme-1
Ca I
-.12

ACCESSION NR: AT4039416
,0' ly tiny ice particles .(1-2 microns In diameter) in the
atmosphere, Increasing both..
scattering and possibly absorption. in the long-wave part of the
spectrum the
contrast also decreases due to dust storms. There is no basis for
invoking IM- i.
probable hypotheses assuming a high optical density of-the Martian
atmosphere.
it Is reasonable to assume that the Martian surface reflects in
accordance with a
law close to the cosine law and the observed spectral peculiarities
of'the vi*sible'
surface of liars In the Indicated region of the spectrum should be
attributed to
the solid surface of the planet. The author extensively cites his
previous studies
of this problem. His criticism of Opik's work (journal of
Geophysical Research,'
v. 65, No. io, ig6o, P- 30057) Is detailed and harsh. "in
conclusion, the author
thanks V. Yarko, laboratory specialist In the Kafedra astronomil
khGU (Department.
of Astronomy, Khar1kov State University), for certain computations
made for this.
study." Orig. art. has:' 12 formulas and 15 tables.
ASSOCIATION: Astranomicheskaya observatorlya, Khar1kovskly
Universitet
(Astronomical O.bs6rvatory# Kharlkov*
State University
-SUBMITTED: 00 -
CQ: 23Jun64 ENCU 00'.'
DAT E A
p
SUB CODE-.- NO REF SOV: 006.-,' OTHEM' 004
M
gi Lcrd 2/2

BARABASHOV, N.P.
Some considerations on the atmosphere and surface
structure of
Mars. Uch.zap.KHGU 122:103-106 162. (KM 15:11)
(Mars (Planet))

L19328-63 E,4-,(l)/r-CC(w)/BDS/ES(v) Ar-~TC/ESD-3 Pe-h/Po-4
"'Ca- -R: R3002047
SS10", Al S1026916310001003loo6oloo6o
SOURCE: M. Astronomiya. Otdellnyy vypusk.. Abs. 5.51.495
A
U7
r. OR: P.; Yezorska5s, V. A.; Yezer V. 1.
TIME: The photometric method of studyinfr the relief of the lunar
surrace
tita
CITED SOURCE: Uchanyyo zapiski )Iarllcovsko universi v. 122, 1962,
Trudy
Astronomicheskoy v. 14, 107-110
TOPIC Tj',,C-S- astronomical photon, etry, lunar microrelief
TRAIISUTIO'l- The *-uthors refine the photometric met-hod for
detendinin.-- the Steep-
ness o4 blopez and elevat tions in. the lunar seas (first proposed
by van IDiggelen,
Bull. Astron. !n#. Nothorl., 1951, 11, No. 423) - They evlain that
this nethod
sup~.lies direct data on slopes provided the photographic strips
are taken zuf-
k,
ficiently close to ,'he equator of intensity and in directions
parallel to ; . In
suc1h measurements it is generally useful to employ large-scale
lunar p%otographs
0
idth a rc!;olution of < 111. -Tao au-Lhors nade mcaSurc-ionts of
moon p~ioto~;,xaphy
obtained at a phase an,;rlo of 770.5, with an irage,diameter of 59
rm. Rhoto.-atric
stripz alonr, the Arzachal and Archimedes craters, obtained on the
Card 1/2

.L 1~326-63
ACCESSION IM: AR,1002047
"are s6m in the Must tions. in
-;7!~P;Mpllotoncter Cra the Arzachel crater
120.3), inclinations of the western and eastern slooes are
60.8 and 130.5.
in the' can so of Ar-I.:Lmed6s"( -+'34'0. 6), they are 40.
2and720.'L. A Comparison of
.0hotometric mcasurem the results obtained by the shadow
=ethod -will give
* clue to -Uic feasibi.34-ty of studying micror-elief in
various parts of a crator --
C.
* matter of considerable interest. 1. Lebedeva
D.%=,- ACQ: "10,.,'ay63 SUB CODE: AI EINCL: 00
Ccrd 2/2

BARABASHOV, Nikolayje ;. PgZHIDAYEVA, M., red.;
YEIAGIN,A.,
':~~RnkO --
Mars. Moskva, Izd-vo "Sovetakaia Rosaiia, " 1963.
63 P.
(MIRA 17:3)

B&MBiSHDV. N 2 TEZERSKIr,, V.I.
Some results ofthe Investigations of the Microrelief of
the
Lunar Surface by Means of Photorntric Method
Report to be submitted for the 4th International Space
Science Symposium
(COSPAR) Warsaw, 2-12 June 63

BAPi BASHOV, u.1%
Dust formations in the atmosphere of Mars and the
color of
Martian seas. TSir. Astron. obser. Khar. un.
no.26-3-13 163.
K, RP 17 s 5)

ACCESSION NR: AT4044397 S/2835/63/000/026/0014/0019
AUTHOR: Barabashov, M. P. (Academician AN UkrSSR); Akimovj, L.
A.
TITLE: The structure of the lunar surface
SOURCE: Xharkov, Universitet. Astronomicheskaya
obser'vatorlya. Tairkulyar, no. 26,
1963, 14-19
TOPIC TAGS: astronomy, moon, lunar surface, lunar albedo-
ABSTRACT: In previous papers (Astr. *zh., Vol. NXXIX, No. 2,
1962;lzvesUyakomissiipq
fizike planet, No. 3, Izd-vo XhGu, 1961) the author has
demonstrated the incorrectness
of the supposition that the lunar surf ace Is covered by a
layer of fine dust, since such a
layer does not correspond to the reflectivity of the lunar
surface. The best agreement on
the basis of this criterion Is with a surface of highly
shattered rocks In the form of
pointed structures with a low albedo and also with
extraordinarily porous surfaces in
which the width of the pore walls to many Umes lose than the
distance between walls, In
these earlier papers, the first attempt was made to compare
curves of the dependerice of
brightness on the difference between the azimuths (A) of
incident and reflected rays for
different but equivalent angles of incidence (I) and
reflection (e) of light from the lunar
Card 1/3

ACCESSION NR: AT4044397
surface, and also the surfaces of models with rough -surfaces of
shattered volcanic rocks,
i etc. A new automatic Instrument'(not described) has now been
devised which makes It
possible to obtain, directly and conveniently, the dependence of
brightness not only on I
ande,, but also on A. A series of models was used in an effort to
determine which
materials would correspond best to the lunar surface not only for
curves B = f(I,C, ), but
also for curve6 B = F(i,e , A) for a difference In azimuths from 00
to 180'. The
following materials were used: fractured tuff with grain size 2-5
mm; a sponge, colored
by dark clay; pulverized tuff with grain size less than 0.7 mm;
pulverized tuff, with
individual pointed fragments of taff (4-5 mm in height) on top;
volcanic ash; pointed
fragments 3-5 mm in height, 4-6 mm apart; fractured tuff with grain
size about 5 mm.
In all samples the grains and walls were opaque. The values
obtained are presented in
'tables; the data confirm the author's previous conclusions: 1. the
lunar surface
cannot be covered by dust; 2. the law of relectio'n from the lunar
surface differs
appreciably from the law of rdlection for volcanic ash; 3. the
lunar surface does not
i resemble volcanic slag because at large i =P_ It begins to have
appreciable mirror
properUes, especially when there Is a difference of azimuths of
18(r. Final confirmation
i Card 2/3

'ACCESSION NR: AT4044397
Is obtained that the surface Is covered either by an
extraordinarily porous spongy layer
with vory thin but opaque walls separating the individual pores,
or by pointed, closely
spaced opaque fragments consisting of shattered tuff-like
volcanic rocks not having mirror
properties. Orig. art. has-. 3 figures and 3 tables.
ASSOCIATION: Astronomicheskaya observatoriya Kharli kovskogo
Universiteta (Astronom-
Ical Observatory) Kiarlkov University)
SUBMITTED: 00
ENCL: 00
SUB CODE: AA NO REP SOV.- 002 07HER. 000
Card 3/3

YAKOVKBi, A.A., otv. red.; FEDOROV, Ye.P.,
red.; AMMITIYEVA,
I - _#-,,Xed.; BOGORODSKIY, A.F.,
Z.N. I red.; bARABAAP_V,,,4,tt.
red.; GOBVINT,-A.A., red.; KOVAL', I.K., red.;
KOLCE;MSKIY, I.G., red.; TSESEVICH, V.P., red.;
KOVAISNKO, L.D.~ red.
[Figure and motion of the moon] Figura i
dvizhenie Luny.
Kiev,~ Naukova dumIka, 1965. 135 P. (MIRA 18:7)
1. Ak-ademiya nauk UH&q, Kiev.

t 11529-66 w(l) -GW
ACC NRs ARZOO1133 SOURGE CODEt UR/020/65/OOO/00,/W55t0055J
r
SOURCE-z Ref. zh. Astronomiya, Abs. 9-51A68
AUTHORs Barabashov N P
formation on Venue
TITLE: An unusual
RUERENCED SDURCEt Astron. tsirkulyar, not 3061 okto 16s 1964o 1-2
TOPIC TAGS: Venus planet, photograph, spectrographic analysis
TRANSLATIONa The workers of the Astronomical Observatory of Kharkov
State University
have detected on photographs of Venue, mde wAh ultraviolet raysl a
large dark
spot which occupies : r%-, 3:/3 of the disk of Venus and which is
adjacent to the
terminator. The spot was observed on 3# 5,. 6., and 7 September
1964, It was alao
traced on spectrogram3p beginning with J\ 4000. A small dark spot
was photographed
with ultraviolet rays on 9 March 1964. V. B.
SUE CODRe 03

ACC NRi AR6020M
SOURGS OOLEs"
AUTWRs Barabashoyl, No Pe; leser9kils V. Is
TITUi DIfferences in saworelLef of the individual parts of the Unar
evrface. Part-
2.0 11
SOU
, ROE& Rafe zhe Astivnomipp Abse 3.51-590
REF WURCE: Vestne, %arIkovok# un-ta, no* 4y ner* astronev vYpt 1p
1965# 22-42
TOPIC TAGS: lunar refleotivity., selenography,, pbotometria
analysis, lunar temp
ABSTRA,GTt Part I was given in RZhAstr., 1964j, 1,51o539, The law of
light reflection
for the medium-high microrelief and the smooth spherical Ybon-was
derived on the basis
of data given in V. A. Fedorov's catalogue as B(c(jX)t where B is
the medium brightneq
denoted further as Bm,ocis the.phase angle., X is the selenographic
longitude. -come
small objects (details) had systematic deviations in brightness from
the mediume Thea
deviations were wqwessed as .4 BAam# The small objcicta possessing
large porosity had
A.B/Bm0 had a lower
porosity* May were chiefly the craters and continental areas. The
presence of slopes
was expressed by changes in the sip ofAB/B. with the changing sign
of the phase
angle a * This was observed in terraces and e6t the bottom of
craterne Caloulations

L 3282-66 P$/QK--
ACCESSION NR: AT50-t4605 UR/00oo/65/000/000 2/06o
1AUTHOR: Barabashov,_N. P.
TITLE: Optical properties of the atmosphere of Mars based on
photometric, bVservati~
data
SOURCE: AN UkrSSR. Voprosy astrofiziki*, iseledovaniye atmosfer
VenerYi Marsa
(Problems in astrophysics; investigation of the atmospberes of
Venuj and Mars).
Kiev, Izd-vo Naukova dumka, 1965, 52-6o
TOPIC TAGS: Mars, Martian atmosphere, planetary astronomy,
planetary atmosphere,,
photoinetric observation
ABSTRACT:. An analysis of the results of photometric observations
of Mars on the.''
basis of the theory of light scattering in the planetary atmosphere
shows that ther
is a greater probability of low values of optical thickness in the
Martian atmos-
phere whose scattering properties are mainly in the vi'sible part
of the spectrum.
True absorption increases in the shortwave -part of the spectrum,
but the optical
thickness of the atmosphere is relatively small in this case, too.
Many areas of
the maris have a greenish shade. It is recommended that Martian
studies be conducl
on a larger scale and with greater diversity. Not even sketches
based on visual
__C0rd_,l/2__

L 3282-66
ACCESSION NR: AT50246o5
observations should be excluded,since they can provide useful
information, especial
when used in combination with phdtographi4~,.spectral,
polarimetric, and other obsel
vations. Spaceship investigations should yield even more valuable
information vhic
is difficult, or even impossible, to obtain from the earth!s
surface. Orig. art.
has: 2 tables. (ii.
ASSOCIATION: A4tronomicheekaya observatoriya Kbarlkovskogo
gosudaretvennogo
universiteta (Astronomical Observatory, Khar1kov State
Universi-,ty)
6
IBUBMITTED: 05Jun 5 ENCL: 00 SUB CODE: AA
DO REF SOV: 010 OTHER. 005 ATD PRESS!
L

L 15763-66 EwT(l) Gw.-',I
ACC NR# AP6006777 SOURCE CODE: UR/0033/66!043/001/0144'/0148--I
AUTHOR: Barabashov. N. qqKqLh
11M" P%L Dudinov. V. N.
ORG: Kharkov Astronomical Observatory (Khar'kovskaya
astronomicheakaya observa-
toriya)
TITLE: Some thoughts on the poselbility of correcting planetary
photometric crosi
sections
SOURCE: Astronomicheskiy zhurnal, v. 43, no. 1, 1966, 144-148
TOPIC TAGS: planetary astr onomy, photographic photometry, Mars,
Nor eian 41:zkv
ABSTRACT: The method proposed by I. K. Koval' (Astron. tsirkulyar,
no. -319, 1,
1965) for correcting the distortions in the brightness distribution
of a planetary,
disk in photographic ph \4nvestigations is reviewed and evaluated.
in an
Rtometric
attempt to correct the distortion in the brightness distribution of
the Martianq-~,
disk, Koval' first made comparisons against the brightness
distribution of a star
and then used the following integral equation for a one-dimensional
case:
Card 1/2 UDC: 523.46

L 15763-66
ACC NR: AP6006777
where F(t) and f(x) are the observed and true brightness
distribution of the plan-!
i
etary disk, and g(x) is the measured distribution in the star
image. -The solutioni
of this equation is considered to be the only appropriate stable
one. Decreasing
the error in measurements in F(x) decreases the error in
determining the unknown
function. f(x). It ie found, however, that the method has limited
application, es-
pecially in the correction of the brightness of points very close
to the limb.
Orig. art. has: 4 formulas. (DMI
SUB CODE* 03/ SUBM DATE, llOct65/ ORIG REF: 004/ OTH REF: 007/ ATD
PRESS:
11260

AP6033169 L
1R/0033/66/04-/()05/I0"9AG46i
'AUTHOR: Barabash,;,-, N. P.; Belobrava, 0. I.t Yezerskiy, V, I.;
Yezerskaya, V. A.
IORG: Xharkov Astronomical Cbservato (Kharlkovskaya
astronomicheskaya observatoriya)
Photometry of the marginal zone of the Moon
Astronomicheskiy zhurnal, ve 43, no* 5, 1966, 1039-iOk6
TOPIC TAGS: moon, photometry, lunar albedo, lunar landing, lunar
surface, lunar optic
property I
ABSTRACT: Photometric characteristics of the eastern and western
marginal zones-of thel
lunar surface were studied by comparison with data for the
photometric-mean lunar
surface. Analysis of published data as well as of original
photomet-.-'-c measurements of
regions in the eastern and western marginal zones showed the
relative brightness of the
eastern zone to be generally greater, and that of the western
zoiie to be less than the
photometric mean for the lunar surface. This indicates differences
in +.he microrelief
structures of the marginal zones--denser material in the outer
layer of the eastern
marginal zone (including the landing site of tho Inna-9 stat-ion,,
'~ = +70.08,
A= -640.2-2) than In the western marginal zone. Heat anomalies bf
the lunar surface
(e.g., less rapid heating of the eastern than of the western zone
after the full ase;
craters, warmer than surrounding regions, observed at the time of
a 'Lunar eclipser.
_q.,jrd 1 /2 1

ACC NR: AF6033169
corrolated with its photometric characteristicsare cited to
support the possibility
of the presence of rock formations in addition to porous
material, Mle lesser
intensity of the moteor strewn near tho eastern zone of the Moon
caused by the Earth's
gravitationalfield is mentioned as a possible explanation for the
observed.photometric
and structural characteristics, Orig, art, has: 6 figures, 4
tablesand 2 equations.'
I
SUB CODE: 03/ SUEM DATE: 26Apr66/ CRIG REFs 016/ OTH REF; 008
ATD PRESS: 5101
Card 2/Z afs

ACC NR' ARG034903
SOURCE CODE: IJR/0269/66/000/008/0061/0062
AUTHOR. Barabashov,
TITLE: S ectrophotometry of a large dark spot on Venus
p
SOURCE: Ref. zh. Astronomiya, Abs. 8.51.488
REF SOURCE: Astron. tsirkulyar, no. 353, yanv. 23, 1966, 1-2
TOPIC TAGS: spectrophotometry, astronomic observatory, Venus
planet,
venusian spot, venusian cloud layer
ABSTRACT: A series of spectrograms of a large dark spot on Venus
was obtain6d-
between August 30 and September 20, 1964 at the Astronomic
Observatory of the
Eharlkov State University by means of the AZT-7 telescope using
an ASP-9
spectrograph. Their processing, which was carried out by the
author and I. L.
Belk-ina, showed that the spot was reddish in color, but changed
with time. During
the period of highest spot development (Aug. 31-Sept. 3), the
violet end of *the
spectrum showed its maximal degree of weakness, Hence, the
conclusion that. the
occurrence of such spots may alter energy distribution in the
specLrum of Venus
Card' I 11DC: 52'3. 43

ACC NR- AR6034903
which could explain the discrepency between the results of i.
G,'U,~hnet.7a and
N. A. Kozyrev. No new spectral lines were detected on the
spectrun-, of the spot.
It is assumed that the spot is a huge discontinuity in the
upper sect-ion of the
venusian cloud layer through which can be seen the redder
layers lying below it, or
that it is a cloud of large particles ejected from the surface
of Venus or formed in
the cloud layer itself. The fact of the occurrence of such
large clouds (20 million
km2) bears witness to the intense processes covering
considerable regions of the
planet. V. Bronshten.
SUB CODE; 03/
Card 2/2

ACC NR:
ARG035553 SOURCE CODE: UR/0269/66/000/010/0065/0066
AUTTIOR: Barabashov, N. P. Yezershaya, V. A.; Yezerskiy, V. I.
TITLE: Photographic photometry of.some parts of the Sea of
Clouds and Sea of
Cognition
SOURCE: Ref. zh. Astronomiya, Abs. 10. 51.481
REF SOURCE: Vestn. Khar1kovsk. un-ta, 1965, no. 8, ser. astron.,
vyp. 2,
12-25
TOPIC TAGS: moon, lunar topography, lunar surface, lunar crater,
lunar
photometry, lunar photograph#.e-)photometry/Sea of Clouds, Sea
of Cognition
ABSTRACT: The following characteristics are obtained for 31
sectors in the region
of the Sea of Clouds and the Sea of Cognition: brightness
Bobs--Bmp where Bm is
the brightness of the photometrically averaged lunar surface at
corresponding
values of the phase angle and selenocentric longitude, reduced
(like Bobs) to a unit
value at a = 1% 5; average values of relative declination E-81B.
and cor-
responding values of the mean quadratic deviation a ; values of
the relative
brightness gradient near zero phase A* , etc. An analysis of the
data obtained
TTT)I'- .52.q- R4

ACC NRt AR6035553
shows that the relationship between X-BIB. and A, is in good
agreement
with the theoretical relationship between these parameters,
computed from B.
Hapke's formula. The measured areas are basically situated in the
region of
negative TB-ID. values and positive Ao values, which corresponds
to a
somewhat greater degree of irregularity (pitting), and, in
accordance with Hapke's
theory, corresponds to a somewhat smaller value of the compaction
factor as
compared with the photometrically obtained average of the lunar
surface. It is of
interest to note that some of the measured sectors of the Sea of
Cognition are-
available on photographs obtained from close range by Ranger VIL
As these
photos show, these sectors differ from each other in their
distribution of small
craters. On the other hand, they do not indicate large deviations
according to the
law of light reflection. This makes it possible to assume that
the observed
deviations in the law of reflection of light cannot depend
substantially on the
presence of such craters and the structural characteristics
related to them.
A bibliography of 8 titles is included. V. - Avramchuk.
-[Translation of abstradq i
[SP]
SUB CODE: 031

UR&BkSVZ.Vl N'. P.
"Distribution of Brightness in the Earth's Shadow During the
Total Eclipse of
the Moon on 7-8 Nov 1938," Astron. Zhur., 16, No-5) 1939

BAWASHEV, N. P. and TIMOSHENKO, 1.
"Photographic Photometry of Mars in Red and Blue Rays," Astron.
Zhur.., 17.,
No-5, 1940

RARABASHEV, N. P.
Barabashev, N. P. "The moorvand planets," in
symposium: Astro-
nomiya v SSM za tridtsat' let)
Moscow-Leningrad, 1948, p. 71-82
SO: IJ-2888, Letopis Zhurnallnykh Statey No.
1, 1949

JMBASS
B k 11~7v, N. P.
41988. BARABASHCV, N. P., CH-EhIRDA, A. T., FEDORETS. V.
A, Ob osves,11chem-ost-i
zemnoy poverk-hosti prim,", i m-sennVm solnechnym. Ushen.
Zaniski
khar'k. Gos. un-ta im. Gor'kog -t
go, T. CM.II. Publikatsii As ron
Observatorii, t. VIII, 1948, S. 21-27
SO: Letonis' ZhurnallrrjkJi Statey, Vol. 47, 1948

. URABASIIIEV~ N. F.
41987. 13ARAWHEV, fl. P---~HEKIROA) A.
T.--Fotograficheskaya fotoine'triya lunnoy
poverkhnosti, uchen. Zapiski kharlk goa. un-ta im.
Gurlkogo, T. L(VIII
Prblikatsii Astran. Observatorii, T. VIII, 1948, S. 29-50
SO: Letopis' ZhurnalInykh Statey, Vol. 47, 1948

BAILUAS'LIEV, N. P.
)11906. 11JUABAStIEV, N. P.-Yotometriya svr-4UyKh 1:
Le,jiykli Lon. Yupitera.
Uchen. Zapiski kharik. Gos uh-ta im. Gorlkogo, T.
)CMI-Ii. Publikatsil.;
Astron. Observaborii) T. VII.Ij 1948 S. 51-64-
--B-ib-lioi7r: 9 N=v.
SO: Letoois' '"hurnallnykh Statey, Vol. 47, 1948

HORDZLADZB, Sh.H.; BARARASHOV.'V.P.. diysnyy chlen.
'WWWAW- ITMOMMM
Chemical composition and transparency of novae envelopes. Dop.AH
URSR no-3:18:
18) '51. (HLRA 6:9)
1. Akademiya nank Ukrayinalkoyi RM (for Barabashov). 2. Holovna
astronomichm
observatoriya Akademiyi u9YA Ukrayinalkoyi. PZR (for Hordeladze).
(Stars, New)

BARABASIU, 11 P,
Dac
wrmo* plawts.. "ice of
Astrophysics
"All-Union Conference on Planetary Physics,"
V. V. Sharonov, 4 pp
"Priroda" No 12
Conference.. held at Mwlkov 21 23 Yhy 49.0
was premijIed over by N. P. Barabambev, Dir,
EbarIkov Astr Obs. Reports were heard on sev-
eral aspects of,planetary physics. Conference
vas held in aftordance with resolutions passed
at Dec 48 conference, reported'in "Astronomi-
cheskiy Zhurnal" Nol,'Igkg, andVestnik.Lenin-
-gradskogo Universitete No 1, 1949.
155T3

BARABASHOV P., diyonyy chlen.
Some results of photometric analyois of photographs of Mars
taken in 1933
and 1939 through light filters. Dop.AN URSR no-5:329-)36 '51.
(MT,'RA 6:9)
1. Akademiys, nauk Ukrayinalkoyi RSR. 2. Kharkivolkyy
derzhavuyy universytet.
(Mars (Planet))

BARA]EAS71EV, II.P.
Bor'ba s idealizmom v oblasti
kospiogonicheskikh i kosriologicheskikh gipotez
(StruF.gle againt idealism in the field of
cospiogonic
and cosrological hypotheses). Xharlkov, Izd-vo
Kharlicovskogo universiteta izneni A-MI.
Gorlkogo, 1952. 120 -.
SO: Monthly List of Russian Accessions, Vol. 6,
No. 1, April 1953

N4 Pt
BAPLABAMR, N.P.
LStudy of physical conditions on the Moon and the
planets] Iselede-
vante fisicheskikh uslovii na Lune i planetakh.
Kharlkov, Ixd-ve
Kharlkovokogo gee. universitsta, 1952. 270 p. (MLRA
7:7)
1. Deyetvitelinyy ohlen Akademii nauk USSR.
(Moon-Observations) (Plaztets-Observatiors)

BARABASHEV, X.P.; OMIRD&. A.T.
Red-, yellov-, green-. and blue-light
speetrophet*metry of Mars.
TSir. Astr*n.obser. Khar.un. no-9:3-28 My 152.
(MIRA 9:4)
Otare (Planet)) (Spectrophotemetry)

BARABASHEV, N.P. PA 2341P.58
WSR/Astronowj Mars Sep/Oct 52
"'Investigations of Various Formations on Marsp" N. P.
Barabashev, Ast-r Obs, Khar1kov State U
"Astron Zhur" Vol 29, lqo 5, PP 538-555
During the next favorable aspects of Mars, its sur-
face structure, lands and canals, polar caps, etc.,
will be studied. Author describes results of his
30 years of observation; of Martian sees, vegetation,
polar caps, atm, etc. For better results more power-
ful instruments are needed.
234T58

Rh'RA ASM, N,P. 0
" ~ ~ Zut%p~, I
~dwi. , P.-
Possibility, of seing the sun's reflection in
Martian "seas'.
Tair.Astron.abser.M2ar.un.no-10:3-6 15z. (MIRA 9:4)
(Rare (Planet))

1. BARABASHEV, N.P.
2. ussR (600)
4. Mars (Planet)
7. Oppositions of Mats. Astron. tair. no. 126, 1952
9. Monthly List of Russian Accessions, Library of Congress,
PA'hri3a= 953. Unclassified.

2. ussa (6oo)
4. Astronomical Photography
7. Color photographs of the moon and the planets. Astron. tsir. no.
127, 1952.
9. Monthly List of Russian Accessions, Library of Congress, May
1963. Unclassified.

BAtUBASHLV, Ili. P.
Razv-itie vzgljadov v oblnsti kosviogonii solnechnoi
sistepT, (Development of
theoriec in the field of the origin of the solar --ystem).
Kharlkov, KnarlkovE~kii
-univ., 1953. 162 p.
010; T,onthly List of Rw9sian Accessions, Vol. 7, No. 7,
Oct. 195h

BARABASL, Y, _14- T,
The COMItUM QU ft43 J- ftIS" (of tjA ftMU of kWgte= UW) In the
fields of
selew* "d lumt1c" &MMM tb&t the fG11001ft 5OL44WIC Wfts,
popular sciet-
tific booits, and textbooks hom bem-m*xItted for compstitim
Zor attain F~-jzes for
the Y"" 1952 and 1953- (ftV&t!M Matura Moscow, mo. 22-k), 2o
ftb Apr 1954)
Fmo
Barab~-,.shev, 11. P.
Title of Work
1%saarch on ?hysical Con-
ditions on the Moon and
Planets"
"Development of Views on
the Cosmogony of the
Solar System"
"The Struggle Against
Idealism in the Field of
Cosmogonic and Cosmo-
logical lly-?otheses"
Nwdmted M
Kharikov Strite Univei,sitY
imeni A. N. Gorlkiy
901 W-30604,, 7 JUY 1954

J, T'
1 . E'I.%.I'k-~"-"'* Ev)
2. (600)
4. Cosmocrcnv
7. "Fight against ide-~dism In the f!F-!dF !-f cc-smr~7,onlcal -,,d
"-Y .1 G. ---sevich, Scv. 'K-ira Nc, 2,
9. Monthly List of Russian Accessions, Library of Congress, June
1953. Unclassified.

BARABASHEV, N.P... professor.
I _..~ , b M ~- , " ,-. __ , - -- ,
- MM",
Color contrasts on the moon's surface. Prirods, 42
no.12:88-90 D '53.
MRA 6:11)
1. DeyBtvitel'My chlen Akademii nauk 'Ukrainakoy SSR.
(Moon--Surface)

IV
V
predsedatel, planetnoy komisaii; SUMIIOV, V.V.,
Some considerations on the orgaLzation of photographic,
photo-
metric. and colorometric observations of the planet Hare
during its
1954 opposition. Astron.tair. no.143:20-21 N 153. (MLELL
7; 8)
1. DeystvitelInyy chlen AN USSR (for Barabashev)
2.Zamostitell
predeedatelya planetnoy komiseii (for Sharonov)
(Rare (Planet)-Oppoeition, 1954)

BARAB&SM, N.P9; GORDON, I.M,
'I
Relationship of sunspots and non-uniform solar radio
emissions. Dnb.'
AN tRSR no.It6-8 054. (NUU 8: 0 -
I Deystvitellnvy ohlen Akademii nauk USSR (for
Barabashev).
2: Astronomichns observatoriya, Kharkivelkogo
derzhuniversitetu~
(sunspots) (Radio astronomy)

BARAUSHIV, N,P,; GORDON. I.M.
Chromospheric eruptions of a special type and their
geophysical con-
sequences. Dop. AN URSR no.1:9-12 154. (MA 8:4)
1. Deyetvitellnyy chlen kkademii neuk USSR (for
Barabashav). 2.Astro-
nomichna observatorlys, Kharkivslkogo derzhvniversitetu.
(magnetic storms)

BARABASHEV, P.
"The Improtance of Studying the Physical Conditions on the 1-bon
and on. the Planets
for Cosmogony," Uch. zap. lGiarkovsk. un-ta, 3, NO 55, 1954, Pp
5-11
Author considers systematic studies of small lunar areas and
spectral and polarized
iant types essentiel for cosmor, . Advocates
studies of -olanets of terrestrial and F gony
the necessity of founding a,special institute for the study of
planets equipped with
powerful instruments. (RZhAstr, No 4, 1955)
SO: Sum. R0- 568, 6 Jul 55

USSRAstronorw
Card
Authors I BarAbashev, N- P*3 AC Oerber of Acad. of Sc. Ukr--R~
Deputy of
prer6 ovLeT'
Title I Propress in astronotV in the Ukraine
PericdiCR1 : Nauka i Zhiznl.:5, 24 - 25, I-Liy 1954
Abetract : The progress in astronomical research in the Ukraine,
since its
annexation by Czarist Russia,, and particularly during the Soviet
regime, is described. Illustrations.
Institution
Subratted

BARABASHEV, N. P. and GORDON, I. M.
"Chromospheric Eruptions of Peculiar Type and the
Geophysical Aspects".
Byul. Komis. Po Isled. Solntsa AN SSSR No 10, PP 46-481
1954.
Data of Quarterly Bulletin of Solar Activit describing
chromo-
spheric eurptionso radiatmissiono and terrestrial magnetic
fields for
assumption that solar emission affecting the earth does
not always
exhibit visible flares. Among 35 cases of raido fading
chromospheric
eruptions could not be observed in 11 cases. This leads to
the con-
clusion that invisible perturbances are affecting the
earth as well.
An invisible solar event may be detected by the vanishment
of emis-
sive lines, probably due to high electron temperature on
the sun and
the ensuing total hydrogne and calcium ionization.
(RZhFiz, No 11, 1955)
SO: Sum No 884, 9 Apr 1956

stronomy Ukrainian astronomers
Vara 1/1 Pub 36 10/36
Autbors i Darabashev, N. P.., Act. Mem. Ukr. Ac. Scl,
Titia Development of astronomy in ths,Ukraine
PerlodIcal Priroda 43/8, 75-811 Aug 1954
Abstract I Some history is given of. the development of the Ukrainian
observator-
ies and the-training.of the-astronomers at Russian institutions.-
Numa-
erous astronomers are cited by name and their individual roles are
briefly outlined. The best-equipred observatory is found to be the
one at Kiev, built since the second World War. Illustrations.
Institution
Submitted

A/, P,
PHASE I BOOK EIPLOITATION 334
Barabashov., Nikolay Pavlovich, Active Member Ukrainian S.S.R.
~-~A~cae~~yo ~c- e5ces. ~'
0 proiskhozhdenii zemli i drugikh nebeanykh tel; kratkiy ocherk
(Origin of the Earth and Other Celestial Bodies; a Brief
Study) Moscow, Goskulltprosvetizdat, 1955- 105 P- 30,000
copies printed.
Ed.: Golubkova, V.A.; Tech. Art Ed.:' Pergamenshchik, Ye.N.
PURPOSE: The purpose of this book is to show-the progress of
the
field of cosmogony, beginning with at~cient, naive legends
and ending with the formation of the materialist hypo-
thesis presented by Soviet sdholars.
COVERAGE: See Table of Contents. There are no personalities amd
no biblographic references.
Card 1/4

Origin of the Earth and Other Celestial Bodies (Cont.) 334
TABLE OF CONTENTS:
Introduction 3
Cosmogonic Myths and Legends 5
From Legend to Science 14
Structure of the Universe 23
General review of the structure of the solar system 23
Sun 26
Mercury 29
Venus 29
Mars 31
Asteroids 37
Jupiter 37
Saturn 38
Card 2/4

Origin of the Earth and Other Celestial Bodies (Cont.)
Uranus and Neptune
Pluto
Moon
Comets and meteors-
Zodiacal light
The universe beyond the solar system
334
39
40
40
46
49
49
About the origin of the Earth and the Planets 66
Buffon's hypothesis 69
Teachings on Cosmogony of M.B. Lomonosov and I.D. Yertov 70
Kant's hypothesis 71
Laplace's hypothesis 72
Faye's hypothesis 76
Ligonde's hypothesis 77
Card 3/4

334
Origin of the Earth and Other Celestial Bodies (Cont.)
See's hypothesis
The plan6t~simal theory of Chamberlin and Moulton
G. Darwini's hypothesis of the origin of the muon
Jeans" and Jeffreys' hypothesis
The cosmogonic hypothesis of 0. Yu. Shmidt
The Formation and Evolution of the StarB
Conclusion
79
19
0
81
83
92
105
AVAILABLE: Library of Congress JS/Is.b
Card 4/4 27 May 1958

BAR&BASHOV, N.F.
00WOMM11,
Idfe in the universe. Znan.sila no.1:6-9 Ja'55-
(MIU 8:3)
1. Daystvitellny7 chlen Akademii nauk USMo
(Plurality of worlds)

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-----------------------------------------------------
-,:S kA ~)
USSR/Optics Photometry. Colorimetry. K-10
Abs Jour Referat Zhur - Fizika, No 3, 1957, 8o96
Author Eqr-qbashoy
Title Remark on the Determination of the Color of Light-
Reflecting Surfaces.
Orig Pub Dopovidi. AN UM, 1955j No 4., 3"-348
Abstract It is shown that it is impossible to employ a
general
color index for the characteristic of the color of a
white reflecting surface. This leads to incorrect ideas.
In particular, the apparent single color of the moon's
surface, observed by several investigators, is ascribed
to a color criterion that is applied without foundation.
If the color indices of tvo light-reflecting surfaces
turns out to be different, this is evidence that the co-
lors of these surfaces differ from each other. However,
this difference does not say anything about the true co-
lor of the surface. If the color index is the same for
Card 1/2 - 132 -

USSR/Optics Photometry. Colorimetry. K-10
Abs Jour Referat Zhur - Fiizilm, No -R, 1957, 8o96
many objects, i'L-1 cannot be determined whether the color
of these objects is the same or different, since equal
color indices may correspond to objects that are colored
quite differently. The only correct comparison of color
of two light-reflecting objects will be comparison over
the entire range of the energy distribution curves in
their spectra.
Q A" U ff.5C 19 7"k'
4c-r z h'qV1VIY UIVIVO-1c sda.;~.
Card 2/2 - 133 -

BARABAMM, N.P.; CMMIMM. A.T.
Color of bright rays from the craters T~cho,
Cepernicas, and
Kepler. Teir.Astres.obeer. Mw.Un. no.13:3-13
155.(MLRA 9:4)
(mooz)

W'LA~SHOTO H~ikol ftVI 8GOLUSKOVA, V.A., redektor;
TVSYIU, I.L..
1 ".1
to ,
o Meriskiy
t
Mars. [Moskva] Goakulltprosvetizdat, 1956. 12 p.
(NIU 10:6)
1. Daystvitel'nyy chlen Akedemii nauk USSR (for
Barabashov)
(More (Planet))

RARARASHOV. N.P.; GUROV, K.P., redaktor isdatelistva;
KASHIMA, P.S..
'~~--ftkbrrteWRskiy redaktor
(Instructions for observing Mara] Instruktaiia dlia
nabliudenii
Marsa. Boat. N.P.BarabaBhoy. Koskya. Izd-vo JLkademii nauk
SSSR
1956, 17 P. (HIBA 10:4i
1, Voesoyuznoye astronomo-geodezicheakoye obshchestvo.
(Mars (Planet))

BM~4SHOV, N.P.
NEWPI,
Determining the color of surfaces reflecting light.
TSir.Astron.o'beer.
Khar.un. n0.15:3-7 156. (MLRA 10:5)
(Color me"urament)

BARhBASHOV JIL,-,qHXKIRDA, A.T.
.0001011W
Comparing the color and the luminosity ratio of
different regions
of the moon's surface with some terrestrial rocks.
TSir.Astron.obser.
Khar.un. no.15:9-15 156. (MIRA 10:5) '
(Moon-Surface)

MMIMP AOTO
Comparing the color and the luminosity ratio of
different regions
of the moon's surface with some terrestrial rocks.
Aotron. shur. 33
no.4:549-555 Jl ---Ag,156. (MLRA 9:11)
1. Mw Ikovskan astronomioheakava Oservatoriya.
(Moon--Surfaoe)

BARABASHOV, N.P.; KOVAL, I.I.
- -
Differnes in the photographic diameters of Mare
photographed in
ultraviolet and red light [with summary in Engli4h].
Astron.shur.
33 no.6-890-892 N-D 156o (MLRA 10:1)
1. Aetronomichaskaya observatoriya TharIkovskogo
goandarstvannogo
universiteta.
(Mars (Planet)-Diameters) (Astronomical photography)

RAj9Q]6-A-i,--. E'P'-~7
---- I-
Unusual brightness of some regions on Mara$ surface.
Astron.tair.
no.172:2-3 Ag 156. (MTRA 10:1)
(Mars(.Planet))