SCIENTIFIC ABSTRACT SEVERNEV, I.M. - SEVERNYY, A.B.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001548220005-4
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 23, 2000
• Sequence Number: 5
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

ARDASHEV, G-R. VIKHAYLOV AMO
I.N.; Z' RSKIY, V.V,j DOVGICH, I.A.,
DOMAWKOV, V.,M.; Prinimali uchastiye.-
FEDOSOV, 1Y.j KRIVENKO, P,M,; KUDRYAVTSEV, P.R.;
BAIUBANOV, Me," BRIL, E,P,, red..; PANSHIN, V.G., tekhn.
red-
(Technical maintenance of the KD-35, KDP--35,,and T38
tractors] Tekhnicheskii ukhod za traktorami ~~35, OP-35
I T38, Moskvg,, Biuro tekhn.informatsii GQSNITI, 1962. 153 P.
(MIRA 16:10)
1. Russia 192,1- U.S.S,R,) Ministerstvo sel'skogo khozyzy-
st-va- 2. Gosudarstvernyy vsesoyaznyy nauchno-issledovatell-
skiy te*nologicheakly institut remonta, i ekspluatatsii ma-
shirino-traktornogo parka (for Ardashev, I~Ukhaylov, Fedosov,
Krivenko, Kudryavtsev, Barabanov). 3. Ukrai=kiy nauchno-
issledovatel7skiy instit"u'. mekhanizatsil i elektriftkatsii
sellskogo khozyaystva (for Zamorskiy Dovglab). 4. Belorus-
skiy nauchno-issledovatellskiy institut mekhanizateii i elek-
trifikatsii sellskogo khozyaystva (for Severnev, Domanlkov).
(Tractors-Maintenance and repair)

SI-INEfulp-IVI DO,'WOK01, VJ,.; IODO, I.I.; A.G.
Substantiation for the tractor maintenance system. Sbor. rab. GOSNITI
no.17:8-13 162. (KIRA 17;9)

SEVERNYAK, S.
On the roads of Bulgaria. Avt.dor. 26 no.4:32-3 of cover Ap 163.
(KRA 16:4)
(Bulgaria-Roads)

~aj_ A - T-.
yers of the Atmosphere"
"~~--teors 3nd the Upper Lo,
I
0 19,4
Astronomicheski, Zhurnal, Vol.11, Illo. 2 1 132-13L
rl .
Tre nslDtior 56,31,69

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ifta of the Compton opadty at low tempta- _66
All. al". is. 7- 13(ligis)
..". Incth'"I -at
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Methods of determining the temperature of the earth's
atm @from bond Spectra. A.lLS--%-ernYf-
of ir Zkurt,""'PIS-501 1 (918) (in English, XPO-51). --when list
tettip. of the earth's atm. is dctd. Irani data an the equiv
widths of the absorption bands 64 Finstcin'% equation
%pectropholornettic absorption couffs. and Childs' data
'cf. C. e1. 27, 3&)-1) on the tramitions 0 - 0 and 11 - t,
the value Tjo.. me 550*K. is obtained. The ~rzlue oh.
tained fro I the rotation six-rtruto of the a-Irand of 0.
with datanol.Alavire and Child, (cf. C. .1, 25, 471111), 1,
" K. .4. bchrv" that 1,-. wally .-haracivy-
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1.11-4 .111 Wit?. Ulm-1.
M4. Coinpion Scattendgi'M AiddisOis In ft" A, D. 1* 0.
Severay. Compki R&Pdas (DokWy) if tAmd. des Zilm". *00
44-49, IM. 'In Xftiisk.-The absorption of fadistion due -00
to Compton scattering by free electrons of stellar inatter.is calculated 400
for the came (list a cvntral region of a star radiates photons of the CUVW =00
Av > mFk This region Is surrounded by matter of the temperature
AT < more anti the free-dwirons obey the laws of the Ferml statistka.
It follows from the calculationo that the absorption of nWiation. due to coo
Compton scattering is small as compared with the pbotodectric absorption 9
for temperatures T < 101" K. The two absorptions bwme comparable 400
0 if the temperature of the enveloping matter and of the core aft 100* K.
for white dwarfs provided that the vion-4egencrate layers at toe age
en%reloping gas have each a linear depth of about one-tenth of the radius. M* 0
it follows that penetrating radiation formed in the ventre of a star,
passes through the surrounding ;;~t~ in a negligibly small time out into 100
space. I- K.
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Stvnm~ A, D.
"On the Stability of Rotating Gaseous Spherea,,u Dokl. AN SSSR, 46,
No.2, 1945.
State Astronomical Inst. im. Shternberg

1W it
--ig~~ U~-A-4--

Sevemy, A. B. ~'On the -stabUT-Ot zaskaus,stals. Astr.-
n [Amr. I Zhurpalj 23, 137-7tTr(im).
(Russian. , Lfiglisfi,stj~ita
iry
purely m(lial. I I for a
osci ons.~.,Lre.consmtt( .-. stir in,
radiative equiNbrium thro-uglioui. The equation of oscilla.
tion is considered asan cl-en-valuccquation and inequalities
are obtainvA foe the lowvst TwritA. TNV-o crufleslifficient
cmiditions of stabiliLy for radial displacements are derivLd:
om! statt-'s that tile vatic) of "pecificlicats mustexceed,
IOGp.la'1(3x-j)) (p. the maximuni density, a the radiiis-i f) a
n1vall pressill,c): the otlicr, involving thc ratio of gas prt-s-
~-Ilvv Its total prussure, is satisfivel wheiiever tlvvrv*i.'; stability:
7'. G'. couling

.........

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00 Alikux-ZANV-2J.221-40M), Che,.,c#mfr.I947,l,2Wj.
P
i
rev
ously. the source Of energy and the structu" of
tht Si"t $Urs havr been expLined on the basis 01 nUdcw

-CtWns' Oa (he bu's Of CA
kns- Of the temst. and life -
*0 Of these 0,1"- It I' shown thAt such an explanation will
00 not willistAnd cfit- CIATIM and th,st the problent of the
rrv u( tht energy o( the jimit star, 6 by no means to be
M.. G.. Mome
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motion and oren"
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d
1l k
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um to we
w" Amm Rw mastic, nw&ls; an
anablis 0( *A 0 'awe( I " ofabionstion
a W. wi* Wwo. is NNGIL Applisawdon to ~Wn with
vft* 9.00 to Is a

~ 01181- - bow is bw - 6w mkn m Ift).
Parlors , ' A "', so Of peowme. An expression
a I" dw is" fmcdom of awrimmiant vcbc* is
sumvw& The N~Wb we "Wisal on c4ph".
Wolf-Rayet mW odaw stairs.
*
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ow of ontfashcac wbukw (men tb* expw*m
00 9 chwwwdmk,* lAbw. 1070 (19M)1 wo *Msmod ov

1 dw smwnds o( rdw sapmom mid kftrtW
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0 -3 W. W~ m
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40 0 & o *I* * * 0 0 0 : : 0 *10 0 o1@ 0 0 0 0 0 0 4 0 0 0 o
L

szvmy-,-A.- BO
A.
oulent Stato of The llol= llhrc=phcre
Turb
DoUat%y Akadaniya Neukl.* =R
Vol. 58, 1947, pp. 1617
From: B. H. L. Guide to H-Sciontifia Per-Lit. Ho. 2p Vol. la fty 1948, Ps 4

0 * 0 0 0 11
9 so 0 q 0 0 00 0 a 4 1 1 0 4 6
4"

00 A fit A-Q Off VAP&M
am@ lick
00 A! 523.8n Man IV > 413X In b8twass, ft- W The a- Of

0,
7715. On dw MAM) mW swIlladviss of 11111IM1111111 ictotabdity which gradually dWW"M with WIT"

: AW NUM A. D. rowr. 01MIRVIII!
"
M
j Vowth of num usid WrigpWatM. In the 0
0 it 1.0-
Artrwkyr. Mr.. I (PnM Russis".
N
'
, owr this am WA dwins 0-1-m- IV
ttwoloon
o0s. - 11ve maNlily was studied by the thftiry of small ~%pa"ejoes of thd mar. it onlimpecia. WhIM dviefts
rwillatiotu, -"W stability doisgods on 3 fjklon: thir ram Un "Wes advatimovina, coritivisas- 'Alwn
mum am vWY WM& bowevisr. avaia few
*0 A the prixna, of screratitm or cncW*. and the Mile Q( an am of WMITIlity amsed by dw KWO off-va-
041 11: dissipefing; the coolly. The faw of thew produces mw digggang cm posisibly expkin *A boWe Cmn of
ly
*Zia Instability when v ~- 4/3; if y > 413.
(he stu Is sable the HeruVruitig-Russell di;W'sirgs as wen as *a UPPe,
1 ~
:0 j uSd is able to pilsate hargnookaHy. Dissipadvig limit of masses. A low frequency of liants of late
i rorceit (uxh as forbulence and mfbthv yWasity) dasm in out plaxy &W the fast evolinion o( these
00 1 tend go stabilize the star: when y > 4/3 vulutim Kars stapat thal the kka o( temporary stability of
are damped anil when v < 4/3. these Imm retud don stairs nay be CWTWL

1
"
he instability. This Is condftioned by The nsean A low maw IN the period of hu ptilludon with
d
.
risny ofthe Mar which. in turm is a gunctiong of its the density In Emden Vhwft has ban derlimel
019 Miss. The dissil;wtion of encrily in stars of modowe Cun"tatioris show better aggromicist wM obscria-

00 MILAS is much knW than the e=m of beat produced tions than sumlar con"atiow of EdMislim and of
by the nuchw rawtiona. but in the %cy massive start; Udma and Pickeris. The turtulcat I 19 - of
U-19i *hem 11 tends to 0, any nxxjv of verterallgif fracra pulaslions Is rovithly lilt-me y Promniorw to the
Crevics; instability. mesin density: cisvisectuemly stars wkh dim iseriods
Suirso(vtry siviallmam turnout to bealviVastablic. hav% statisticaltY wevikins. smaller amilslitudes, It is
As the awn Srows law, 2 classeft with the um lilt* that In tars with pernionent pulsotions ft
c9ccuire wriperature Lan be distinguished: dLMtse
varve, tration o( the soumvi of trmW toward an
OWN'.- IaW Mars (y < 4/3. p. < p critkal) xrW dervic small Centre is very hilth (rcenvuls, or AlkhmoniI. It tm
IbuW
AS..SLA tYALLUPfKAL LIVENAIL419 CLASSIFICATION
S
to at 19 04%% vic"t It
0 0 0 0 0 0 0 0 o t 0 o 0 0 0 0 0 0 0 0 0
so go a 0io 0 0 0 0 0 IN 0 0 00000 0
been
analytically that slow rotation o( a star
makes it urmatic with respect to nonr&dW pub&-,
tions, This nay kad to the formation of& double star.
I so two 011111KIMIna 3
to go 00 0 e 0 0 0 0 0 9 0 00
1.00
j-*9
* 0
.so
- 0 is
-00
IF 0
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also
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SEVERNYY, A. B.
Severnyy, A.B. "Internalstructure of stars: in symposium:
Astronomiya v SSSR zatridtsat' let, Moscow-Leningrad, 1948,
p. 179-83
SO: U-2888, Letopis Zhurnallnykh Statey, No. 1, 1949

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