SCIENTIFIC ABSTRACT NIKOLSKIY, G. M. - NIKOLSKIY, G. V.

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• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001137210015-0
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: January 3, 2017
• Document Release Date: August 1, 2000
• Sequence Number: 15
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

III[OLISIKIT.G.M.
Prodictleg the, fore of tho solar corona for J~mmo 20, 1955.
Astromots1r,so.160ill-12 J0155- (MLRA StIZ)
1. Itsfodra extronowit Kiyewskoo ustioretteta
(fta-Corma)

simordla=1 GAS
oalo w I INVI - i,
';Irt=rn 7of sobw cor*sm. Antroo.sbur." no.2:84-86 U-7 156.
(mm 9:6)
I.Kafedra sotrosaidt KlMokago gesudaretwomwCo uaiverettata.
(saa-corems)

1"ZOLISJU. a.m.
*- *
Polar ray frossuff of Me Corona of 1954. Astreu.shw.33 **J:
87-n lopf 956. (KINA qt6)
1.9afedrs setrenoull Klyevsksco gagudarstvesnev nalverelt-sta.
(lua-Cerass)

SUMISKIT, G.M.
4 =14=r~,It cm*owmt of tho cod1wal Itrht. Astma.d=03 me.3:
(Nm 9:10)
410-413 VW-Jo 156.
(todliwal light)

VIOW
I muhhhh.
OS 9WOMI rqMo Aistrsv6 abw. 33 lw,415~84" jj - Aig._*560 (WZ" 9CII)
1. WO&A 44*rq~ll Klymbw C"Mdamtvwmww wdvwettAta.

111 1 TA"Wg 2.9e; SIOLISM . G,Ke
Observattow in Kiev of %be parttal solmw *clip" of Dacw%Wr 14,
1955. Astranoisir. no.166tz-3 T& 156. (Km 917)
I,Uf*dra "tro~ll Klyevinkago gosuda"tw*=go universitota
Imal
Oftlipsos, solar-1955)

NIMLISCIT, G.K.
".--- v~l
of the aortas In costimiame apectra without &a sellpse.
AstromAdIrt. mo.167sl2-14 IP 056e (on 919)
I.Wedre astrommall 91yovsksge ualvoreltsta.
(sma-coress)

WIMMUITI- -q-1f0
Aurora bor*&Us obsory" mar Alma-Ata, Astroneteir, na,185vZ10
0 157, (KMA U t 4)
leAstraftstchoskly Ivatitut AM Ir"SU, Alma-Ata,
(Au"res)

NML#5rU,A1X1--. -.- .
XUatroootom,stric observottlons of aurora borealis of Septomber 29.
1"7,j visor Alma-Ata. Astron,tair. no,186M-24 X 157.
(KIRA 11A)
1, Astroftsichookly Institut AX fat$$X.
(Auroras)

-- -r!
Nt tt'CL ' `.Ki IV I I -V 1 .6 -
G.R.; IULMOVA, i,,li.
Flat* on Awlter. Astr5n.teir. ito-1711tt? xr '57. (vJAA 3c: 11
(J,,miter (Pl=ot))

allovexly. (I.M.
cmmmeuto an &A. K%govick's %rttclo orominotity functlon of
not% soquemo stars qvA Its Interpretation.* Astrou.shur. 34
ito,3:493 VAY-Js IS?. (mm lo..?)
(Stars-K-igultude)

33-3-2T/32
CO-110"te by Nikolfskiy on the paper by A.G. Masevich
17juxiAosity function for stars of the main sequence" and
author's reply. (Cont.)
ant timag and N is the number of stars in the Galaxy.
Substituting for 9(R) Manevich obtains:
nt 1
22 - = -
N L LO
where L is the luminosity. Masevich argues as follms: if
in the process of evolution a star loses mass and its lunin-
osity decreases, then using eq. (2) it Is possible to estimate
the ==bar of stars f ormed in tims t . If the evolution takes
place at constant mass, then according to 9q. (2) its lusin-
osity should increase. However, it follows from equation (2)
that when LO is leas t4an L , n is always negative. This
absurd result shows, according to Masevich, that evolution is
only possible with a loss of mass. He further considers that
the n6ptive alga indicates the exit of stars, evolving at
constant masev from the main sequence.
However# the present writer points oul- that the R*H-So of
eq. (1) is essentially positive. In considering evolution

G. ME.
"Solar Cororia of February 25, 1952"
"pilotometry of Comnal Pays and Corp=cular Strewar"
"Polar Radial Systems of the 1954 Corona"
Vaeklisnataklyp 5. K. and G. M. InKOLSKIY
"Structure of the Solar Corona of June )D, 1954"
(TOUL ICUPW of the Im,, P*kvLry 1952 and Zow 30,, 1954.. Ummcuow of Um
2044"1 t'0 Mww" 9019L- NUUMM) NOOMM, Isd-vo AX ~. 1956, M V.

J. 4W 0
Translation frout Bererativnyy thumal, Geofittka, 1959, Ur 4, p 140 (UWA)
AUTMRt 91kol"ekly, GA
01
TTIU- On Uw Problem of the Night Sky Glow In the Red and Gr4en
Speetral. Lines
PERIODICALi ltv..Astrofic. in-ta AS KazSSR, 1958, Vol 7, pp 55 - 57
(Orgl-.700.)
ABSTRACTt The relative Intensity of' the lLnos [011 5577, 6300 9 and Rat
5893 2 in the spectrum or the night sky Is detemined by the
spectrographlo method. Unter the assumption that t-he glow
Is excited In the P2 layer and that electronic Impact causes
the exaltation, the author xolves the equation of thf- ml.ero-
steadiness. In this way. the population or the 132 le"I Is
obtained such lower than that corrospondLng to the relative
Intensities observed. On this basis the author draws the con-
elusion that the glows In 55T7 and 6300 9 occur at, different
card 1/2 altitudes and the w*chanlams of their excitation are dIffertnt.

90w;;ds
suv/169-59-4-4214
on the Problas of the 9103 Sky Glow In the Rod and Oreen Spectral Lines
WhIle 63W X line to oxotted ma a result of a direct ele.-tronle firpaot.
processes based an the dissociattmi of the molecular oxygen tay appear rather
as tho 4mattation mechanIsm of 5577 X-1tne.
L,M.F.
LI-Ir
Card 2/2

NIKOWSKIT _441.1".-
-F ;;P~
Nature or the red spot (with summary to SGgllabl. Irv. Astrofte.
inst. 1626kh. "17:58-(4 959. (Kau 11:7)
(Jup iter(Planst))

50) SOT/33-35-4-t7/25
AUTHORs k1kollskly. a.m.
TITLEs On the Possibility of Absorption of Solar %L Radiation by
the Interplanetary Kedium (0 vo=ozhnosti pogloshcheniya LLv
radiateli solntse methplanatnoy sre4oy)
P010DICALs Astronamitheekly zhurnal#1956, Vol 55, Nr 4, pp 657-659(USSR)
ABSTRACTs The author determines the concentration of njutral hydrogen
in the interplanetary space to nH-1- 10 ca- for nWV
1024 103CM-3 and T-40 4. The interplanetary Can posseises
in the 1.Q& line a high optical thickness between earth and
sun. There are 9 references, 2 of which are Soviet, 4 German,
2 American$ and I Kaglish.
ASSOCIATIONsInatitut astrofielki AN Kat SSR (Aatrophysical Institute AS
Kazakh SSR)
SUBMITTF.Dc Decouber 14, 957
Card 1/1

30)
AUTHORt Nikollakly,G.71. 50T/55-36-3-12/29
I& - ~
TITLEs On the Coronal Emission In X 5694
PERIODICALs Astronomicheekty zhurnalvI959jol 36,gr 5#pp 477-480 (U33R)
ABSTUCTs The author tries to examine experimentally the theory of 91wert
'CRef 6,7,7 with respect to the emission of x 5694 an4 n 6374.
For this purpose he uses the observations of the solar corona
due to Waldneler. A statistical treatment of these results
c*nftrus the theory of 91wert. Then the author gives a survey of
several opinions on this doxm1n, where he sentions especially
the papers of I.S.3liklovskiy and (;.3.1vanov-Xholadnyy. The
author to of opinion that the identification ef the yellow line
with Ca IT due to 9419n fRef 11 is correct. 7he question of
the ratio 15694 /1 5446 renains unanswered.
There are 15 referonces, 5 of which are Soviet, 4 Gerzan,
2 Swiss, I Ctec-hoslanko and 3 Axoricaa.
ASSOCIATIONtAstrofixicheakiy institut 1kadeall naak Kax 532 (Astrophysical
Institute of the AS Kazakh SSR)
SUBMITTEDo June 2, 1958
Card 1/1

AMAZa
WY%My
11 4 At I/ 2-4~ 0 S
3/555160/00VOW/007/007
312312201
AUTHOR; likolleklylad No
TITU: Corpuscular radiation of the tun &ad zodiacal light
MIODICAL: Toprosy kossogonli, v9. 7, 15600 181-212
TEXT: This is a report based upon results of the author's own studies and
findings by other scientists. There are many physical theories concerning
the possible nature of the corona. L paper by 1. S. Shklovakiy pcavLdes a
survey on the subject* The streamer struaturs, of the solar oorona Is also
the object of n=y studies which are directed, above allo to the thermal
dissipation frou the corona. A great number of astronomers$ observations
concerning the notion of matter In the direction of radiation has been con-
duated under the guidance of S. L. Tookhsvyatakiy. Studies of the density
along the rays revealed its aonotanto course. re. A. Ponomarov to mentioned
for having studied the stability of coranal rays. An attempt has boon made
to associate coranal polar rays with polar faculae. The linited lifetime CIE
polar rays can be easily explained by the outflow of matter (loll c/sec)
from the corona. The thermal dissipation of the letter in dealt with in a
Card 1/2

"'5g560/007/000/007/007
Corpusoular radiation of oo, 5123 201
special section. The amount of dissipation to 109 9/soo (1033 protone/sto).
The corpuscular radiation in the polar regions of the corona to dealt with
separately, A very thomgh discussion is made of paper* by K. Waldaoior.
Spoo trographlo and radio methods are discussed In connection with the
estimation of gas concentration in the Interplanetary space# To Go Feset*m
is mentioned for having published observations of the zodiacal light. A
theory an coronal dissipation has boon worked out by So So Pikellner.
Opinions differ as to the origin of the zodiacal light. 1. S. Shkldvakiy
believes that cosmic matter surrounds the Earth as a ring, In much the same
way an happens with $&turn* Observation@ of nocturnal light by rockets or*
discussed# and the kinetic torperature of Interplanetary gas to considered.
Sir-ce this gas absorbs corpuscular solar radjetion, its energy Lncreases.
Therefore, its temperature will be Tew104-102 0K. Also, the thermal dis-
alpation of the Can component of zodiacal light is considered. Interplane-
tary neutral hydrogen, which should absorb solar L. radiation, cuts out a
narrow line from this L 12 line. There occureq of cours*0 an interaction
between interplanetary particles and the gas. V. 1. Korozov and V. Go Kurt
are mentioned, There are 5 figures, 5 tables# and 52 references: 37 sovilb-
bloc and 8 non-goviet-bloo.
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14
5/030/60/000/010/011/018
3021/1058
AUTHORS N-1kol'skly, 9. No
TITM sitendea, Plenum or the Commission for Baler Research
PERIODICALS Vestnik Akadoaii nauk 33SR, 1960P No* 10, pp. 104-105
TZXTs The Ordinary Plenum of the Commission for Solar Research of the
Astromositcheskly sovet kkadmail n&uic $591 (Istronour Council of the
Academy of Notensee IMNR) was held in riy*v from May 50 to June 4, 1960.
Paper* on the study of solar physics by the observatories and scientific
institutes of the WBU were discussed. Reports on processes In the
chromosphere dealt with the distribution of atone on the energy levels,
elosientary &taste processes, and problems of the structure of the chrbao-
sphere as well as results of the observations of chroaosph*ro flares. The
follovinC lectures were delivered next@ L. B. Sev*MU, R. No ShabanskL
and go Cordon dealt with theoretical problems of the physics or riarest
S. Gonaarsk-roport*4 on the SSovenent of the gas of the flam In can-
nootion with Its sagnetto fieldi A. T. we"Yanovich analyzed Its ray
structure on the basis or photonotrio research of corona recordings;
Card 1/2

Xxtonded Plenum of the Commission for Solar B1030
,/60/000/010/0ii/ois
Research 3021/B058
Go S. Ivanow-Kholodnyy and Go X. likolfskly analyzed the physical propwtiej
of the transitton son--o between chromosphere and coronag Ye. At FgnosuLrer
dealt with the corona theory from the point of view ,of gas kinstical 11_
Shi-khu- ("okays obe,arratortys - raw Oburrala ) and S, 0. Obashel
reported on the spectrophotoaotric study of protub*rancox, ; V. Y*. Stepanov
considered the great movements in the solar atmosphort Ott the basis of ob-
sarvations of nagnstlo phenomena on the sun; X. 1. Kaglievsk y theoretical-
ly considered the process of the penetration or the magnetic field into the
corona; To 1. A- onsldor*d the possible connection or the variabil-
ity of the general solar magnetic field with the escape of energy In the
form of beat Into tho coranal To 1. litkovic 9 If* No -One",shovs 4, ro. -
Wouggovicb, 0. J, gollfrukb, and Ae Y. Dravskikh roported on studies of
the radio frag-- .0 1. So Shklovski To 1. Moroz,
V. Go Kurt,_S. WY, a4 I reporteif on problems
K. Teekhavyst M 9. 2
of Probloas of observing the impending
total **lips* an Yetruary 15, 1961 were dealt with by a special commission
composed of representatives from observatories. The oclipa* to to be ob-
served from the Barth &a well as from hlgh-altitude planes.
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5/033/60/037/005/003/024
41#o A4v ti 07 E032/E514
J0Lqjaday_y__(' 5 , Nikol.'skiy G M ind
AUTHORS; jy_aagy-
Gulyayev, R, A. -----------------
TITLE., Ionization and Excitation of Hydrogen
1. Elementary Processes for the Upper Lmvel-i
PERIODICAL: Astronomicbeskiy zhurnal 1960 Vol 3- No 5
pp. 799-811
TErr Elementary processes as-socinted with qliantiim trnyisi
tions, such as, recombination, ionization. collisions of the
first and second kind ' emission etc, are frequently discusned In
connection withVAstrophysical problems, The prest-rit paper is I h
concerned with such elementary pror-esses in hydrogen plaRma in ifil
of imodern data for the corresponding effective cro~ws-xectionn
Particular attention im paid to the tipper quantum Ir4vels The
first section of the paper Ls concerned with the phenomenon of
pre-ionization Thias a hydrogen atom cannot extfit In a state
with a large quantum number m when placed in an electric field
since the latter reduces the height of the potential barrier and
an electron at a certain levet m () will thus become tiffectively
free.. The pre-jontitition effect orin also be "Iftsociattlif I-rith tho~
Card 1/4

S/053/6o/o37/005/003/024
E03VE514
Ionization and Excitation of Hydrogen I. E14-7-,ii-ntnry Proces'je.-l for
the Upper Levels
perturbation of hydrogen atoms by fren irng If tht! diqturbing
proton and the nuclcuf4 of the atom arp at a 'tstan~:e r then the
total potential energy of An electron in the field of tfleme two
nuclei in of the form
U(r)
Ir V r r
This is illustrated in Fig-l 'in which the dashed ~ijrves represent
the undisturbed fields. If the total enerjv of the electron in
the m-th level E m is not smaller than the maximum height of th"
potential barrter Wr /2) -- 3,-"/r then charge transfer will
take placo and the elec?ron will (-ntpor the prtential well of the
neighbouring proton. In a plasma chitrateri.*(A by an ioy density,
n1 and, consequently mean Jntf-U-10rki~ distance f'D -, .4 it1/3 the
above charge transfer mechanism will c~~,rxsr continuously throughout
the plasma. The electron will be found in a LAnd similar to tho
conduction band in solids 1-e Place
Card 2/4

5/033/60/037/005/003/024
E032/9514
Ionization and Cxcitation of Hydrogen. 1. Elementary Processes for
the Upper Levels
The Ionization continuum will be lowered to the level with the
principal quantum number m. determined from the condition
9n C U (r 0/2)
0
or
3e2
0 0 L (2)
r _ . 0,946,1 cm
0 02
When It, < U (ro/2) charge transfer can also take place as a
result of the tunnel effect, All these phenomena are estimated
quantitatively and an expression is derived for the total number
of charge transfer* per unit volume per second. The appropriate
expression for this number is given by 1Cq.(7). This expression
gives the total charge transfer cross-section for an excited
hydrogen atom and a proton, In the second section of the paper
Card-3/4

S/033/60/037/005/003/024
9032/t5lk
Ionization and Excitation of Hydrogen. -T. Elementary Processes for
the Upper Levels
a calculation to made of the total effective tross-section for the
',rR,#en plasma. Expressions are
various elementary processes in hyd
derived for the excitation (tq-15)/de-excitation by electron
collision (Zq.18) cross-secttons. Contributions duo to ionization
by electron collision (Eq.26), photo-ionization (Eq,44), photo-
recombination to all levels (Sq.33) and recombination by three-body
collisions are estimated. The relative role of these effects to
discussed for the ground and upper levels. There are 3 figures,
I table and 21 references: 11 Soviet, 2 German and 8 English.
ASSOCIATIONS: Institut prikladnoy geoflziki AN SSSR
(Institute of Applied Geophysics_AS USSR)
Inattt t remnogo magnottzma, ionoefory I
rasprostranenlya radiovoln AN SSSR
(Institute of Terrestrial Magnetism, Iono
the Propagation of Radio Waves AS, USSR)
SUBMITTED: April 1, ig6o
Card 4/4

Line!) It-& t"I'l Chronosphor.-
C'urd 2 14
wa~ the f iz 3t to h t - :'r.
the effect Cf 1.11 i:3 t ~.r
f
at mo ai~h,j. Yor tKilm pl!" 3 r. _1
9 c f 0 1 r c
for 1344 N 'r, t 1.1 rr t I
tt'.S r invo st t:!,tti 1,
L c 1v - Ttf) V
141
0 Fie FF
t 1'. e f C, -1
t('.4
17 7 7 14
tioll of 'the ground l(tvol P; A, 3
f b% t Ni.
b the
d.~nsitj ~rf the ex:AtInt- radi,,tt.4.0a. .)w
-- be re- r
chrmosphori) in Lq vali
TA j :A
a bla-k brAy with 1. .000
e
--',040 .0
14"Lp 44,

Ultraviolet Radiation and Excitation of Oxygen
Lines in the Chromosphere
3
B14 RLO /bi3'00 . The estimation strongli d*pvnds on the
assumed Intensity of Lp radiation and oa the electron tempqra-
turs T of the chromosphere. When kA440; to not excited bj
Lp radfation, the intensity of the chromosphere lino3 is bound
to be low. In the absorption linex,',kO446 Pic' IF174, 11,55131
/'7774 1$ almost equal to unity. The ohiracteriatic features
of the excitation of the chromosphere lines ~ 8446 ierrft the
measurement of the Intensity of LO in varioua ret;tcns of the
chromosphere. This method otbvioustj has ad-rantpgea over the
measurement of Lp with rockets, however, it supplies only In-
formation about the density of Lp radiation In those chromo-
sphere layers where the emission lin,., ?4.16 Is formed. In
such observation It 13 recommendable to record AXP446 and 7774
simultaneously. The condition I 8446/177Ti >1 directly in-liclates
the additional excitation of A8446 by L railatti-ri. There are
X0 Soviet.
I figure and 6 references, 2 of which A q1
ASSOCIATIO14: Inatitut z,?mnorn maenetizmsk. Armonfor-, I
Card 3/4

Ultravlolot Radiation and Exottation of Oxyetn
Lines In the.Chromosph*re
re4iovoln Akademli nauk SSSR (Inatltut,?
t
__MaCn!!tjAT, Ionosphere, and h c. 0
1~~
of the ka 0- thi
PRESISTED: August 25, 1959, by T.G. lesenkov, Acmlex.L.clan
SUBUITTED: August 20, 1959
Card 4/4

Rio
Iroa the imization ard excitation in the regiort- betueea chmmosphem ix
corma."
report to be oubmittect for the IAU Symposl= on the Corona, Cloudcroft, New
mexico, 28-3o Aug i96L.

G. H. &m-1 I=TL-VVSKIY, ED. !.
'10a the polarizatLort of coronal emlasion, lines."'
report to be submitted for tb-- IAU Symposium on the Coronat Cloudcroftr Ifev
Ktxicqj, 28-30 Aug 196L.

HIROWSM, G.H.
Photoeleatric ob"rvations of codlacal light mw Alm"ta.
Gamag. i aer. I no.3:354-358 My-Je 161. (HRA 14-9)
le Astrofitichaskiy Institut AN Ka6SR L Inatitut rAmmogo
nnwtism,, lonoafery I rasprostrAmnlya radlovoln AN S-SjR.
(U41acal, light)

89321
S/033/61/038/001/004/oL9
E032/E314
0
AUTHORS*. Ivanov-Kholodnyy, G.S.
TITLEt Ultraviolet Solar Radiation and the Transition
Layer Between the Chromosphere and the Corona
PERIOUICALs AstronowLeheskly churnal, 1961, Vol. 389 No. Is
pp. 45 - 65
TEXT: Preliminary results of the work now reported were
described by the author In Vestnik Am sssk, 196o, No. io,
po 104, The physical properties of the solar chromosphere
and corona are now relatively well known. It has been
reported (Petri - Ref. 1) that the emission maximum in the
inner corona occars at a height of only
1.03 Re - 2 K 10-9 cm Thus the Intermediate layer
between the corona and the lower chromosphere. in which
the temperature changes from about 6 000 deg to about 10 6 dog,
the concentration of atoms from 1016 to 3 X 10a cm-3 and
the c~egrse of lonination from 10-4 to 107 to a relatively
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S/033/61/059/001/004/oig
t032/t314
Ultraviolet Solar Radiation and the Transition Layer Between
the Chromosphere and the Corona
narrow region and physical parameters change very rapidly
within It. The present paper is concerned with the upper
part of tke intermediate region, which is also called the
"upper chromosphere" or the "sub-corona". This part of the
solar atmosphere suits a strong line spectrum in the ultra-
violet region which Is LargeLy responsible for the state of
ionisation in the upper layers of the Earth's ataosphere.
It is shown that the line intensities calculated by
Woolley and Allen (Ref. 8) are always lower than the observed
intensities. particularly for low ioniestion potentials.
It to said that the Wootley--AlLen wodeL to not satisfactory
because it does not reproduce even the relative intensity oC
the lines. twission lines originating in the soLar corona
are also found,,In the region under investigation
(100 to 2 000 A). The wavelength and the intensities of
same of the coronal ultraviblet lines were predicted by
Shk1ovskiy (Refs. 10, 11) as far back as 1945. Shklovskty
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89321
Sj033/61jo36jooljoo4/O1q
E032/E3L4
Ultraviolet Solar Radiation and the Transition Layer Between
the Chromosphere and the Corona
has predicted the intensity or the resonance doublets or
No VIII (768 and 776 i) and Mg X (610 and 625 k). ilia results
are-said to be in conflict both witli the data of Allen and
Woelley (ReC, 12) and with observation*4 Other theoretical
work in this field (Elwart, Refs. 13, 14).has &Lao Led to results
which are said to be in disagrtement with obx*rvations. The
present authors have therefore attempted to set up a new model
of the intermediate region using recently published dat& on
the shortwave emission spectrum (Johnson at at - ReCs. 2.
Jurxa at at - Rer. 4, Behring et at - Ref. 5, Aboud et &I
lteC. 6 and Violett and Rease - ReC. 71. Analysis of expert-
mental data carried out by the present authors has Led them
to the following two basic CormuLaes
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s/m/WoWool/ooVaI9
Ultraviolet Solar Radiation and the Transition Layer Between
th* Chromosphere and the Corona
we
AT 0.5T0
In theme formulae x gives the ratio of the abundance of the
given element t to that of hydrogen, n M& n() Le-its
proportion in the given stage of lanLaotion, I to the
2 0
intensity in erg/cm at the Earth surface, X is in A
fL2 in the oscillator strength for absorption,
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49321
8/055/61/038/001/004/019
E032/9314
Ultraviolet Solar Radiation and the Transition Layer Between
the Chromosphere and the Corona
We a WT3/2 /r 12 and i)Tacorresponds to the maxiatum or
the expression [nl IF- n.()]W . To is close to the
average temperature of the given radiating region and
AT represents the difference between the boundary tempera-
tures. Fig. 5 shows the relation between AT determined
for a number of Lone an a function of To . The points
are experimental and the straight lines corresponds to
,AT a 0.5T0 .
Fig. 6 shown the relation between the '*partial emission"
.491 and the temperature To for different Lone in the
transition region. As can be seen, there to a satisfactory
correlation between the points, except for N IV and N V
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E0121
S/033/61/038/001/004i/019
C032/C314
Ultraviolet Solar Radiation and the Transition LAyer Betwoen
the Chromosphere and this Corona
It is shown that aftaidi the optical thickness in a number of
these lines to greater than unity, self-absorption to absent.
Estimates carried out by the present authors show that the
nitrogen concentration on the Sun Is
DIIAN] "... 10-5 , which is lower by a factor of 1,5 than the
usually accepted figure., The continuous emission of the Sun
in the region 50 - 1500 A in computed. It in concluded
that the X-rays recorded in rocket experiments form a line
spectrum (Kasechovskays and Ivanov-Kh*Ladnyy. Ref. 27). 90%
of the ultraviolet emission during 1958-1959me emitted by
active regions occupying 1/10 of the surface of the Sun.
The surface brightness of the undisturbed regions in lower
by two orders of magnitude than the brightness of the active
regions. It to claimed that the model or the transition
layer not up in the present paper for active and undisturbed
Card 6/8

89321 . I
5/035/61/o3g/001/004/019
E032/F,314
Ultraviolet Solar Radiation and the Transition Layer Between
the Chromosphere and the Corona
regions In In agreement with optical, radio and rocket
observations, The model leads to &.steeper temperature
variation with altitude as compared with existing models.
Acknowledgments are-made to I.S. Shklovskiy for valuable
advice.
There are 9 figures, 6 tables and 42 rererencost
11 Soviet and 31 non-Soviet.
ASSOCIATIONS: Institut seenogo "gnotimm. ionosrery L
rosprostraneniya radiovoln AN SSSR (Institute
of Terrestrial Magn*tism, Ionosphere and
Propagation of Radlo*Wavos of the AS USSR)
Inatitut prikladnoy geoCitiki AN SSSR
(Institut* of Applied Geophysics of the AS USSR)
SUBMITTEDs September 230 196o
Card 7/6

5/033/61/038/001/ook/oig
IC032/9311a
Ultraviol*t Solar Radiation and the Transition Layer Between
the Chromosphere and the Corona
F i's. 's I WWO FLZ,06s

Card 8/8

IVMV-KROLMXIIO- G.S.t NUMISMI-G.M.
IMMMUD& AM& "OLt&Uoa akf wirw". ru-t 2t The mm"r of
obmwvo& limo in a mies., Astrou.shur., 36 00.3s455-44 W-A
161'. (KML 1416)
1# ImUtut PrLkladnor goofLaLkL All OU L Iwtitut mmogo
n%p*tL=&j Lonomforr i resprostramnLya radioTola AX SSSR,
(Hydroges-Speatra) (Hydrogenp-ion coamutration)

S/033/61/038/005/ooa/015
9133/9435
AUTHORS: Ivenov-Kholodnyy, G.S, Nikol'skly, GIM,
TITL&i The prediction of solar *m1roJon lines in tho extromo
ultraviolet
PERIODICAL; Astronamicheakly shurnal, v.38. no.5, 1961, 328-843
TXXT., Although many spectra have been obtained in the extrtmo
ultraviolet in recent y;ari. line identification to often doubtful,
particularly for X < 3 0 Previous theoretical work of the
authors (Ref.l: Astron. sh., 38, 45, 1961) on the intensity of
lines In this region of wavelength does not agree with
observation. The present work gives & full list of the
Og ultraviolet, The
estimated brightest resolved lines in th: f-
maximum temperature was assumed to be 3 1 0K. The methods of
calculation used were developed In the earlier pap*r (Ref,l).
A parameter AVI to employed which depend* on the Ionization
temperature Ti, The relationship betwoon 441 and Tj was
determined from observations of tho Intensities of 27
sufficiently bright lines lying near X ;,01200 A (Table 1), most
of the ions chosen have hydrogtn-like configurations and have been
Card 1/ 0 'A

I( P 1J4
S/033/61 -i8/005/002/015
The prediction of solar 9133/9435
observed several times in rocket *poctra. The absorption
int-n4ity Is given In column i of the table (I(La). erg/cm2/xec).
It mumt be remembered that there appears to be a variation of
intensity with solar cy:.le, The authors calculate r, for
50 ions, by the method described in Ref,l- and hen,-e derive t4c.
The ratio I/af can now bfi expressed as a function of ~k ani TI,
Nomograms are constructed in order to simplify the cal.~ttlat&Dns,
The tr&neitions and wavelengths are listed In a long table,
These were calculated on the basis of the tables of Ch,E.Hoor*
(Ref.10; Atomic Knorgy Levels. Washington, w-1, 19~9, v.2, 1952)
Where terms are omitted in this work, they wore obtained by
extrapolation along lsoolectroni-. sequences, (Where this hao been
done, the lines are shown In brackets in the table Lines
belonging to a single multiplet are bracketed togo,~her,)
This table consists basically of transitions fur which the Lapirti
rules hold. The most ~-ompll---,mtod problem in the calculations it
the determination of the probability of ex,itation by electron
collision. In many %ases, the oscillator strength t^n only be
estimated. Values of lu-g T, greater than 1,6 it 10C' Are shown
(in brackets). since this is believed to be thc MAjLLMUM
Card 2/if ~

308 iL
s/o33/61/o38/oo5/oO2/O15
The prediction of solar 9153/9435
to"rature of the inner corona,, CorroorondIngly, inequality
signs are put in the intensity column.- The relative composition
of the Sun to taken from the work of C.W.Allon (Ref,3, Astrophys.
Quantities, 1955, London Athlono Press). The astount of nitrogen
present in taken to be 10,5. future articles will compare these
predictions with observations. There are 3 figures, 2 tables and
11 references: 3 Soviet-bloc and 8 non-Soviet-bloc. The four most
recent references to English language publications road a* followei
ReC.5: A.Aboud, W.C.Behring, W.A.Rense, Astrophys. J_, v,130,
381, 19591
Ref.6t H.C.Hinteregger, "Preliminary data on solar extreme
ultraviolet radiation in the upper atmospheres" (preprint),
Symposium, Florenz, 1961;
Ref.B: T.Violett. W.A.Rense, Astrophys, J., v.130, 954. 19!9.
RefAt J.D.Purcell, D.H.Packer, R.Tousey.. The Ultraviolet Spectrum
of the Sun, Sumpostum Nice, February 11-16, ig6o.
ASSOCIATION: Institut prikladnoy Stofielki AN SSSR,
Institut zemnogo magnetiama, tonoofery i ramprost-
Card 3/6 ~A ranentya radlovoln AN SSSR (Institute of Applied

The prediction or solar ,,,
SUBMITTED.~
Y,814
5/0~3/61/038/005/OP2/015
C133/g435
Geophysics, AS USSR. Institute of Terrentrial
K%gnetism, the Ionomphfare and Propagmtion of
Radlowaves AS US5R)
may 16 , ig6i
L-f
Card 4/$\~

S
.,/203/62/002/001/001/019
1023/1223
A71-A'110H:
MILE_, f1hort-wave rRdiation or the tun (Review)
?'EHIODICAL: Goomngnetl.-m I Aeronomlym,, v*2, no,l, 1962, 3-37
77AT : The article reviews 71?estern and Soviet literature covering
the period up to 1961o The topics treated are: experimentftl dixta
on short-wave rAdlation of the sun and the identiricAtion of
spectral lines; short- wave radiation intensity of the sun and
the Ionosphere of the earth; short-wave radiation and the
structure of the sun's atmosphere* There are 20 figures, 7 tables
and C5 rererenceso
Card 1/1

0155
$/2O3j62/OW/OW/OW/021
1023/1250
AUTPORe Ivanov-Kholodny7. G.S. and U11coltskiye G.M.
T ITTA. Identification of Sun's r4distion lines In this short-
wave reeton or the upectrum 0!!~_ 1100A)
PERIMICAL: GoomagnetIsm I Aeronomiye, vsZ* no*30 1962g 425-442
TUT: Out or ^-,225 lines of Sunta shortwave rRdiatlan (60 tc 110*
obtained by Mdan* or rock:tl, 180 lines are ldenttrt~d In thin works ,
The Intensity of the line taken Into acclounte A orItteal anslyms,*
is of former IdontIf test tons In givene rn the spectral envgy dis-
trIbutlan Iftxims, in the follovIng wavelength regions were founcls
00-200 (corona), 200-450, 550-650 750-8500 950-105OAt A mlplmum
"t'nots' Rf the tatn I energy or t4e I tne rM Istion ( A t-_ 1100A ) Is
25 org/on- see at the gartho Half or this energy to concentrated In
the region of #2300-JOO As Tho relatIve content of n1troCen on the
Slin Is H/H 0 WO-uo Thc Identification of the lines was done by
comparison with a list of 540 spectral lines, In the ran 19-2lbAt
taken from s work by the same authorst Astrofte%h*19 T 928o The
610
Caid 2/2

S/29.3/62/002/003/003/022
102311250
Identification of Sunts rRd1nt1on,..o
Interattles, of the lines In this list oxesed 340" - 20'3 erg/cW
sea. Thert Is I tablas 4 f1Gnir*a,, 19 - *ferences.
ASSOCIATIONs Institist prIkladnov goorlxlkl Akadamil nalik W5H
Inatitut Zemogo magnettxamo ionosfery I resprostra-
nonlys rqdtovolu Akadsmil nouk SUR (Instituto of
Applied Geophystess Academy of Sciences of the USSR;
institute of Terrastrial 14tgnotlawo Ionosphere aml
Radlowave Fropseation, AG&d&vW of Soleness or the ussR)
Sq3HITTED: September 2. IOG1
Card 2/2

AUTTIVIt
TiTUP.
1023,1260
3 "12
Mikolsklys G.,Mo, Proxhino V.P., &M Saxanov# AsAs
A shadowlese coratiaGraph wIth a stationary spactraeraph
of high dispersion
MIOVICALt Qeot*Cn*tixm I. Aeronamlyag v.,2v no.,3p 19G2j 532-540
TEXTs The eoronograph described wax constructed In the IZKMANO
Ito aim to to obtain 11 Peetra or the corofis and or the chrowtoopherot
with rt dialTerstan or 1.5A/mm. in tho, range: or wavo langths 3600 -
1200G A. Tho coronogrnph convints of & matille pnrt ensuring a nre-
clan diroctior and focutt or the ohjective and trRnamitting tho rays,
into the atationary part - thn dpoetroerapho IM ona-lona objeatIve
iO rwV4000 mm) produenit tha Mints image on & aurved alit which ofin
turn Rrmand, the optlooLl axia of the objective by 3600s, & ayatetaof
mirrors finally produces the izvge or the objective In the: plarta of
diffrection grid (600 lines/mm,, aropi of l5Dxl5G niK). Thex spoet-
rum obtained may ba photo opliod directly or deflected by P~n auxil-
i#Lry plane mirror to an Zoetronia reorvaing evster4o. The, narono-

-U&*jLW.rG-K,.
0 0
Selm todUU= in ro~v Umm lkil 3WA =A Nor 04t,
Goom4gal &w, 2 jw.64025-1032 X-D 962. (M&A'26tl)
"Wlo"U AN SM*
(spur radfation)

AUTHOR:
TITLE:
PERIODICAL:
RikolO.okiy, G.
304 1 H*II and
Akademlys, nauk
SIOROJ621141100410091027
BM/3186
V.
584 1 Hel resonant lines in the sun
SSSR. Doklady, Y. 147, no. 4, 1962, 809-812
TEXT: The intensity of 304 and 584 2 solar radiation was studied, its
distribution over the solar disk and the fotmation height of these lines
In the solar ataosphere being based on results of earlier rocket probes
G. S. Ivanov-Kholodnvy, G. M. Mikollskly, (;eouqp. I seronQmiya, 2, no.
~1962); R. A. Gulyaytv K I Nikollskaya, G. M. 91kollskly, Astr. zhurn.,',
40 (1963) in the press$. 'It*waa shown that practically all He atoms in
the sun exist In their ground state. Essentiai proc~osses are electron
collisions &ctinor on the Eround level, and recoubinations. These processse
excite the 22po nit,., 1 evel whic itsleft, by &tons in spontaneous
processes. It was found that 304 ~ radiation In the bottom layers of th*
solar atmosphere is "optically thick" although neglIgible, owing to low
temperatures (Ir0a--jo5oK). The width of these lines, calculated by the
Doppler effeat, is 0.04 7/10 of the 304 2 radiation is saitted by the
Card 1/3

S/020/62/147/004/009/027
304.1 Hall and 584 1 HeI... B117/B186
active regions of the nun, The emission of active regions Is six times
Ito -0 2.5ec.
that of nonexcAted regions. of 4,,% ezission or the sun to 0.9 erg1cm
584 1 and 304 1 radiations are "optically thick" and also neglii;ible. 7hey
are generated in an optically thin layer in the Te,-63000K region. e0j~
of this radiation to excited by recombination The m..13sion of active
regions is 3-5 that of nonexcit;d regions. T;e 584 1 emission of the sun
near the earth Is - 0.03 erg/om -sec. Approximately half the radiation is
attributed to the active regions of the sun. Intensification of the
spectral. lines observed during outbursts 0e. 6. Behring,.W. k. NejPLrtq
J. C. Lindsay, Preliminary Solar Flare Observation with a Soft A-Ray
Spectrometer on the Orbiting Solar Observatory. Freprint by Solar Phys.
Branch Space Sci. div. COSPAR 111, 1962), is interpreted by the author as
implying that outbursts in the chromosphere should not be considered as
explosions, but a permanent source of energy emission. There are 2 figures.
ASSOCIATION: Institut temnogo magnetizma, ionoafery I resprostraneniya
radlovoln Akademil nauk SSSR (Institute of Terrestrial Magnet-
leaq 16nosphere Ind RaUd Wavo Propagation of the Academy
of Sciences USSR)
Card 2/3

S102OV62114710041009102?
304 1 HOII and 584 1 Rol..- 2117/ '. is6
PRESENTED: July 4, 1962, by V. G. Fesenkov, kcad*s1olan
SUBMITTED: June 28, 1962
I
. 0
; . Card 3/3 . 4

\-I ,
k1"If 0 (Ok -
M.
Star ooronas. and their study In the field or I-rays " extrem,
ultra-violet. Osm)
Roport, submittod for the 4th InternatiorAl Space Symposium (COSPAR)
Warmav,, 2-12 -Tune 63

ftpan to be subWltftd for UW Ilth GICWMI A"41ably, ratl. Won af (kOdfty
=4 aeop*Lce (MM), Imimler lg~.SL Aug 63

LMHIT5# N. At, j, JQ~~~
ob"GUIX AdtrWUichsskoCo Instituta AN Zft,SR,2 (@a N. G.
garimr's work)@ Astron. shur. 40 no.ltl99-201 J4 63.
(XIU 1& 1;
1e lUtitut Smago lmgmttsm, loomfory I mpt traumdju
rMiavoln AN SSSR.
(&M-Corona)

ACC90ION Wit A?)W12)7 Sic~0).Ie/63iO4f.'/003/0433/U-~43
AL1111DRt Gulyayey, R. A.; Nikollskaya, K. I.; Nikollakiy, 0. M.
717LICS * Stma~'tllof the
ospA~rs~..'Ln active and unperturbed regions.
IfydrDgen and holi= Ionization
SOURCE: A3tro-_--micheskly zhurnal, v. 40, no. 3. 1963, 433-445
TOPIC UGSt solar atmosphere, solar chr=osphere, Balmer contlnu=, solar efurt-
wave radiation solar temperature, solar electron wrcentration, neutral hydrcgon,
1:)nAted hy'drog;n, solar hall=, Ionized heli=
A35MAM This paper analyzes observations of the active and u;nperturbed regi-)na
of tha solar atrosphere. The distribution of -the Wmperature T. neutral hvdrogen
n-sub-HI, and electron concentration n-vub-e In th-i lover chrowsphere at h *q-,al
to ov greater than 1,000 k% was obtained from eclipse observations im the Sr Il
Ilmes anti In tho Balmer conti=n, (Tlbr=an. R. N., Athay, R. a.. Fvsics of the
solat chromosphers, Intersalance Publ., N.Y., 1961,';. see Figs. I and 2. The data
obtained are in grood agreement with the model set forth by 0. 3. 1vanov-)Diolodryy
and (1. X. Hikollskiy (Astron. zh., v. 39, 1962, 77,') for t1he trarsition region an
tho norona, at h from 5,000 to 7.000 ka. Variou.i meichAni=s of the ionization of h
.......... . .......... 4 ........ ~ . *:.'._~^.' 1.'. - . . . , . , . , . . . 1. 0'." , , , - - - - -
........... -..% ...........

T. I'll;I14-o
A(;iX!jZj0J1 Mi A?3001237
and It are postulated and examined. The di3tribution of HI, HoI, HeII, and HeIII
f(rand for elevations from 1,000 km up to the inno., wrona (Figures 4a and 4b).
-imve solar rudiation participatea effectivaly 'A tlh~ ionization of H and He
the ohrawsphere and the transition re4ion. The theoretical calculation of Lhe
Wksa-1-11 mkt-way6iormthls- 50-4 and 220 anistro
aro In good agrement vith rocket observations (HintarvFgar, H. E!, J. Geopkqs.
-F~as.j-y. 66,--wi 80 1961, Z367; A.trophyi. J., V. 132, 1960, 601). Thlare are 4
flgiwes and 5 tables.
A.330i;IATTON: In-t Ze=jgo m4gnetizza, iononfery*1 m3prostranenVa radlovoln,
Akadmii mik S~J'SR (In3titute of Earth MiZnotimA, t.%e ionoqhero, and Pzd,lowava
Propligatio __0 -2-fence'3, sssfl)
L, Acadmy
EUIRMTED: Zlmay62 DATZ ACQD- O'-,,Tu.163 ENGL- 03
XB COIE, AS, PH 4w REF SOV: 006 OTHER: 017
C:
.jfd 21

KIKOWSKIrv G.M.
Struettwe of md sbartuave radLation from the upper atmq*arce of
sUrs. ftrt 1. ContInuotts eateston of hydro~m wd heLLwm.
Astron.shur. 40 zo.4t668-677 JI-Ag 163. . NSA 1698)
1. IneUtut mmogo mgmetL%m, Lonamfory i raxprostrawaiya
radLovoln All MM.
(Stitro-Atmomphorem) (Casale rays)

IfMOVSKITO G.Ke
Energy of abort-wave solsx radlatioa Lu tho opmtral regl=
IIW R. Ge=a,,. i aer. x n'o.5&793-802 S-0 f63,
(K= 16t1l)
2. Inatitut, sumoed m4kvO
radlowla AX &WR. . &ms, Lonoefery I rasprostrazwnlya

ACCESSION NA: AM017615 S/Coij/641041/041/007514079
AUTHOR: Livshits, M. A.; Nikollskly, G. Me
TIhE: The ne and T relation to the chromosphere - Corona tr4Asltl4n region
SOURCE: Astranomicheskly zhurn4l, v. 41, me 1. 19", 75-79
TOPIC TAGS: atmosphere, chromosphere, corona. Spectroscopy, stellar 4tWAKPh4r**#
transition region. stollar-radiation
ABSTRACT: The authors discuss the formation of t.- transition region between the
chromosphere and the corona, painting out that the nergy ablated by radiation from
any*'Ievel of the transltl~n level Is camp-aced of ths dissipulan energy of the zKock
W s at that level and the energy carried upward a; a result of heat conduction.
Meeauthors call "important" the conclusion accordl g to which, I he transition
region, both In undlsturb4d as well as active regions, the low ",024 a const. has
been found to be valid. It Is affIrtred that In a stable condition the energy bal-
ance In the transition raglan of stellar 4twasph4c" Is descelbod by the equation:
(n*gT) - Edtsg* (n*,T);
-that Is, by the equality of two independent functions: the emission and energy of
card 1/3

'ACCESSION UK: AP01761IS-,
dissipation per cm):. In this arttcte,~tha authors 4tteWt;tG &ter"ine-the we(.
versallty of the fo6nd dipandence of4f oh density and tamporaturo~ noting that.
-since, tha emission 6f thi transition reg~jon Irn It stellar atmospheres (having In
mind 11stabit" starsl Is loused by the radiation of an optically thtnlaytr in
Shortwave lines (with thtt radiation belonging to different'lons'formed and exc[ted
by electron coll[5116nt) !then C trt the funct-ton OL and T can bo found theoretical-
ly. Thus. the tow n&Z.�T = const., found (or thensoter transition region, it
generaEtzed to apply to the *tmospher*0of "s't&btd!1 start. it is, assumed, In this
connecti cs. that the coot Ing source of toe; transition rogt^ is tine; emission by
highly tonizod atom; this cooling is compensated by the; dlistpaton energy of wask
shock waves. From this, according to.the, authors, it follows, that, in the first
approximation, this law holds for the transition r"tons of 11stabl4el stars. Some
peculiarities of the transition region ar*,0scussed, it being demonstrated that in
the chromosphere and coronardanstty distribution corresponds. to the hydrostatic (in
the chrowspher* the logarithatc gradient [a not more than two ;fmes, I"& than the,
observed, while In th* coraw thoy are identical w0hon, Ortgo art* host
3 flour" and a formula*.
ASSOCIAVOR: (nstttut xamogo magnettma, tormfory* t resprostrainentya radloveto
Akadami I 9"k SSSk. (institute of Terreigtrial 14"nottsm, tonqwipwo MW 1144to W4W4
Propogation of thal;Acad~wr G! scietwose ASSR),
Card 213

RIKOLtSKIr, GA.
I
Itrwtwo ad slarowa" *aloslon of Ittallar uMr atnespber*s.
Part 2t bletrifttion of *Isatron density and temperature.
Astrouahw. 41 no.2t251-254 Mr-AP 164. (MIRA l7c4)
1. Institat manogo, nognetisma, tonotfory i rasprostramniya
radtavals AN SM.

A C-I.MINION URs AP4031623 UkI10) FV64/004/002/01WO
MI'L E -. Thn absemUm o( oxygam m ultiplets La Tn5tia 7? 7 4 *,M L.P"nbda 9f"6 ta the
q,,)Imr !hmmomphare
~~VJIICE3 GetimlignsUirm I aeronomiya, v. 4, mr.~. 2. 19&4, 209-212
J
"DAPI F.: TAGS: ophere. kiolar rpectrnRmphy sohrr mpec~,.. oMem line
LOAL-OK 9FM9~
Earhe- thimpratte-ij dIF,4-vA~imA t4hvx(*I that Vie orygem muIttpleta #47774
.,% 4+46 could be excitad either h APCItrort impAct or, in the c~axo dN
M4 6. by
c i -onnospheric FU L,*� 10021-1. 7. x1 Inp. 1. 3. ShkolovAiy trlt-d wtthf;ut success
I
Ouitr(m. ths. , 1957, 34, 127) W observo t1w )N 44ji; line tn Lhe F-q:tb'm atrn(ophere
Wwri'49 M110t). In the NGIBr VMWI)hore the-ne hm^s were, b~ mo resoarebars
. - - I - A A -,-I- v t 4.A ill

1'774 muldpW tsmststs of three empments, whilex 4U4 fis--iviirf -FOW
-,miponmta. The observid intmistty radoo are m-spectIvAly 7.-6-4 (tboarry- 1;5,.3)
vid F-:3,,6 (5-4, or 5:3-.1 for the thoorebeally exprcW trif let). The width of the
niulOpIfirtA FLnd c4her effocu in ocmiurvAlona -wWh the *jLeervf.?d Imax, Inclueltag the
. - -- --ot%hArIv. mhs~Jrvtton~ ptrp slti;o tuaru-%ved tn comMolav-

Mt. I
gut AA --
UDM63 HNCL: DO
,
lqc~ RAT sovt 005
, i
2
,4 - -
()rTyE I.: W7

----------
,xp
N
ACCESSX N M APS025569 UR/0031/65/000/000/0081/0001
1ATMORt N1k*j1skk,_Q* M. I OkLahty-, S. 0.
;TITLEi Extraeoliptic observations of coronal lines In the infrared region of the
specti'm
SOURCES AN xamssRe Vextnlk~no. -0, 1955, el-
441
sltauvn telescope, solar _qMnLas 'Sol" IR radiation, IR telescopes
,solar. telesacps
'ABSTAAM the development and use of electron talssco;mv in the Soviet 1.1ninn has
made it possible to observe inftv~rsd spectral lines in the corma after extresely
short wi"sur* times (%1 *in) in the region of %12,000 X, A Zeiss extraecliptic
c 0'rqmm'_8 nh- as ~mod at- the Htith-Altitude C2rqpaUt i the A3t
~_~ty_te -MN 1ING-Jor obaemati f camnal lines in the vear-infrared region of the
:spec~r=. ff 'p
L _MCt1=_xp=tmDZrap~ was built for this urwalk by
Prqpagatiq
,the in
:cooperation with, the As"bysics Institute (F m 3400 am. grating 600 M-1
Mdlapor-
.;uion 5.6 X/m.in order 1). The re4littion receiver was a SOYLet-ma" single state

L 193646
AC'MSSIOK XR: AP50255611
rk- op --co"*rter-7vit1viM cwle4 by dry ice. 95~
'=/1. S Aamen wsre used for the transfer optical system. A number of
spectrograms In the re X1 A 7892 and re X111 1 10747 regions w*re taken between 17
rebruM and 10 March 1965. Examples of these spectrograms am shown in the article4l
in spit* of the low chlorosphere-photo3phers activity and poor atmospheric condi-
t1ons during this period, it was posst)ls line -
In many cases to record the-A 7892
Both thesellnes were bbser-red during the complete abtrence of the Fe X A 6374 Una
In the jioUr corona. OrIS. art. has: 2 figures.
ASSMIMM
SUBMITTIT: 00 EHCL: 00 Stm CODC'. M OP
1'0 RrF sova -000 OTHM 000

L 36609-M r.,,r (I ) Ivec, raw
7CC RRt ATW23722 SOURCE CODE; UIR1283IM1000101-410005/0008
-AMOR: Iv=av-1a*olodnyy, G. S.; Mikol'sklyG. M.
ORG: none
TITLEt Short-wave solar radiation, structure of the solar atmosphere and the
lonospher \IJ(
SOURCE: AN SSSR. Mezhduvedomstvennyy geofizicheakly komitet. V razdel programw
MGG: Ionosfera. Sbornik statey, no. 14, 1965. lonoofernyye issledovaniya, 5-8
TOPIC TAGS: solar sp6ctrum, F layer, solar corona. chrownsphere, solar UV
radiation, solar cycle, atmospheric ionization, Ionosphere. solar activity,
solar atum3sphere
ABSTRAM An examination has been made of 225 spectral lines obtained from various
spectrogram In the short ultraviolet range to Identify them with known line-s. Such
identification requires the knowledge of physical conditions In the solar corona
and the Intermediate space between the corona and the chromosphere. A theory of
ionization in the solar atmosphere was developed, and, on the basis of this theory,
lines were computed which must appear in the solar ultraviolet range. From spectro-
grams 180 lines were identified with 11nes computed theoretically. Fc, Si, and
hydrogen lines were the brightest. A model of active regions on the sun was composed If
card 1/2

Li f-~
36
AOCNR: AT6023722
-to explain geophysical phenomena. The brLghtness of the active regions In ultra-
violet light was found to be 30 times that of the quiet areas. The Intensity of
ultraviolet radiation varies from day to day and depends upon the phase of the solar
actIvLty cycle. The total flux of solar ionizing radiation was determined, and during,
maximum solar actility, It was equal to 15 ecg/cm2 - sec. New data an tLe short-wave
spectrum (0-1100 A) were uced for computing the speed of Ionization in the atmosphere
A model of the Ionosphere for the heights of 100-800 ka was Jeveloped for various
moments in the day. The saxtmu= ton formation occurs in the FI layer during the
day and In the F2 layer at night. Variations of ion formatLon are great In the
F1 layer and small to the P2 layer. The asymmetry In the density of the upper atmos
phere at moon causes an any try In changes of the speed of Ion forsatLon and the
nuwher of elactrons. Ibis phenomenon contradicts Appleton's method for determining
the recas6leatlan coefftclento New date require a change In earlter concepts of the
processes of ickiltia-tion and recombination In the Ionosphere. OrIg. act. hes: I
f1gure, (EGI
sum oams o#/ s= am awe/ ouc wir: oaq/ o= nn ow ATD rmm:5031(
Cmd 2/2

r-M35-67- _EWt1L_GfT_
~"A~RS03028 SOURCE CODE: UR10131GG/000400fi/003810038
AUTHOR, G. NikeEi-WY. 0. M.
atmosphere and
TITLE: Short-wave solar radiation and structure of the p9lor
ionosphere
SOURCE: Re(. zh. Issledovaniye koomicheakogo prostranstva. Abs. 8. 62. 260
REIF SOURM 8b. tonaefern. tasledovanlya. Wo. 14. M.. Nauka, 1065, 8-8
TOPIC TAGS: solar atmosphere, spectral distribution, solar radiation, upper
atmosphere, Ionosphere
ABSTRACT: The problem of investigating the spectral distribution of intensity
of the short-wave solar radiation is discussed. A brief survey Is given of articles
devoted to this problem. The results are presented for determining the rates
of ion formation In the upper atmosphere at different times of day. Bibliography
of 10 titles. (Translation of abstract]
SUB CODE: 031

-02097-67 Wr(I
r444~-14~--"1101116i-
V
SOURCE CODE: UR
AUTKORt 91kallekly, a. M.; saxamor, A. A.
--.--,W ------ ooww~ 4
On: institute or Terrestrial Magnetism, the Ionosphere and Re"o Wave Pr4
Ac!!!W--0r-M1Q-n-Cqft Sm titut zennogo mWetL=m, Lonoaferr I rasproa,
rMovoln AMMON&L nauk MR)
IV
TITIZ: The mation mad nature of R. spiculev In the solar chrmomphero
SOURCXt Astrodamicheekly shurnal, v. h3t no* 5# N66s 926-935
TOPIC TAM: solar chro a phere, chromosphere spicule, phoLoqAmrIc radiation, corma,
radial velocity I Jkle.49g 40ewL F-
ABSTRACT: The He line profiles In 11 spicules and their radial velocities Vr am
Investigated uaing successive photographs of the spectra of spicules taken at a
height of about 6000 ka. Altogetbir 26 photographs of the spicules vith an everme
interval of 20 see vere taken In 8 aln with the IKIRAW (Institute of Terrestrial
Magnetimisq'Jonompbere, and Nadlowave Propagation) coronomraphr(principal objective
25/cm/4~4 2A/m, equivalent focus 7 m). The radial veloctties are random with time
with an averqp perLod of I als. The stgm of Yr can alga vary# The mfo mcheatem
or % admalam or splea*m to scattering of photospberic radiation. At the hei#t
of 6000 ka the spicule to optleaLly thin In W4z Ut % 0.0 and has the following
physical parmsUrs: T Ob 600001, an % 2.011 cm- 11, no % 20-1011 cors. Tb* cheatto

motions of separate clots of =tter with Telocitles of 10-20 kn/sec ploy an
essential kolo in the flormatiom of the % line yiroftles. About one-third of the
spicules abow a Nkmblet" structure, the doublet car4pocents having praeticaLly
identical drmosic and photometric characteristics. It to possible that one-third
to the lovest estimate, " the distance of %r-4" between the components of tbAt
oboex. d&Ablets colseldes with the revolving power of the instrument. Orig. art.
has: T f1juve =A I ftnowles
M COM 03/ ~ MISS 209ov65/ ORIO AV: 007/ OM Wi 007/ ATD I
OWN

45-6"" E:WTW o"14
Nita
Ap6o288cia
SOURCE COLE:tJR/00,33/66/o43/oo4/o868/o872
AUMOR: likollskiy, 0. M.; qmzmav, A. A.
ORG,. Institute of TeUggtrima -MaKnotiss, Ionof phere. and Rodloweve ProsiCkat an
or sciencesi'sSSR (In-t temoso Magnetirma, iononferr, r"prZ;i_t
,n kkademIL nauk SSSH)
TITLE: Noneallase coron2ffaphs
SOURCE: Astronoxicheekly thurnal, v. 43, no. 4. 1966, 868-872
TOPIC TAGS: eclipse, cormagraph, spectrograph
ABSTAACT# The simplified typvb or the noneclipee coronograph am critiveny analyzeLl
The necevislty of constructing a large Lyot-type coronagraph equipped with a I
stationary high dispersion spectrograph to discussed. An optical schematic dlWm
Is given and the main characteristics are described for such an instrumient, which fA
underconstructlon maJe at the Instituto of Terrestrial lbgnetiss and Pulkovo
Observato_q under the supervision of the authors. Orig. art, has: 3 figures- LC=6
SM COM. 03/ SUBM DATE: 20gov65/ ORIO-EMIP: 003/ M JRW: 002
Cd 1/1 Qt, UDC: 522.56

ACC �,Ri AZZ1010GOG
SdJaCEE CODEz Va/0364/66/00010041000010OL6
AUTLOR: MkOlTsk1YO__(;,._jj. (Doctor of physica-mathemistical. science[.)
ORD: none
TI=s Short-wave molar radiation
SCURMS Zemlya I vsQlQM%&yA* no. 49 1.9660 9-16
TOVIC TAGS: solar rediationg solar etvaosphore
SU3 CODE: 03
ABSTMCT: 12w article cited below reviews the history of study of solar
short-wave radiation. It Is noted that such study to now an Important
research toot for the astrophysicist for Immstigation of the phys,cal
processes in those layers at the solar abwsphere uhich In large part
cannot ba observed (too the earth's surfdOO. In the short-wave region
a',*. the spectrum the relatively cold layers at the solar atimosphere --
tho photaspharo ad lower chroomphere - have virtmLly no emtxsi,~n
and the entire speettun with wavelengths shorter than 1000 A Is deter-
nined by the hottest layers -- the coronA and upper chrq,-qapher*. Usually
almost all the mitans (or torA) are in the gmrd state od therefore
chemical quantitative anstysts Inewitabty Laraly" oonverstan to as
cAniff *f 'tom In the groom stste*

ACC W4 AP7010686
Since tho o"zvfwlmtvg majority of the shorc-wom Itries are relarer., to the
around state of &coms (or tons) the mat pmcise data on the chemical
composition "a be obtained fm an ansLysis of short-wave data. %he
article makes clear the importance at such studios and CLY86 brief data
on the niathods and insts. nts used in such studiteg together with the
=oat iap*rtent results obtained by SavietZ mg American researcheru, but
on the whole to of an Intro " to and superficial ammeter. orig. "-t-
hass 6 figureso Z
JMg 40.Z;
4C

t
fit i
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140 1
Ar.

Mat I BOOK ZVLOITATIOU 34OV/5456
ftraft6viche Nava ft1gorlyovich, D"tor of Ttehnlaal Solma*e, tm-
fossar# ed.
Spravochnik po chugunnom Utlyu (Nandbook on Iron C"Ungs) 24 *400
raw,, and Onle Moscow, FAshgIs, 1961. SW p. Errata allp Inserted.
16pOOO copies prlnt*d.
Ravlevere F. P. Berg, Doctor of Teohntcal ftLena*~, frofessori Xd.t
1. A. 2kranov, Engineers Zd. of PubUshLng Smsos T. L. ZeykinaS
Tech. Zda.c 0. V. Speranskara and F. S. Fromk1n; Managing Ed for
Literature an KachIne-&dldInS Uohnoloa (Leningrad Dop4Q;nt.
xGshgiS)$ re. P. Naimov, Engineer.
IWOOZI ThIs handbook is intoft4ed for t*4hni4al personnel at
cass-1ron faundrIes. It my also be of %be to aklll*d wocksm
In foundirles and atudents apoeftlIzIng Ln fowAlng,
COTMUs The handb"k dontalne InfomatLon an beale problesm In
the modern sanufaetuxe of iron c"tings. The following are dis-
cuss"# the aawpoaftlon and Properties of th* motall ths making
of moldej op"lal dastlag mothods; the aharge proparatIon; aeltIng
C

Mindbook on Iran Castings
and moafying the cast iron; pouring, shaking out, and eleadng
of castings; heat-treatment methodal &A the inspection and re-
jectlon or castings. Information an fdunAry eqalpu*nt and an
the mechanIzatlon of c"Unr production to also presented. Me
authors thank Professor P. a Berg, Doctor of Technical Seleases,
" staff members of the KoastankoUt Plant, headed the ohlof
metallurgist 0. 1. Xletakin, Candidate of Teahnl4al ::160444, car
their assistance. Weren4se follow sash chapter. Move are 28T.
roferenaes, mostly Soviet.
TANA OW CORTZRISe
to rd IN. 0. Girshaviall)
Ch. 1. OomposItLon and Properties of Cast Irim (W. 2. 41rabovieb)
1. Equilibrium dlegremoslaself1datIoup and Mis atmeture
o-i-cast Inn .
2* West of various Casters an t1w strasturis OC Gast
cam efti-
1

Handbook on Iron Castings SOV/5458
5. Designing the gating systems and risers (B. V. Rablnovich) 93
6. Drawing designs of castings and patterns with acces-
sorles (N. N. Vyahealrekly, and To. B, Imerman) 140
Designing of flasks (I. P. Tegorenkov and Q. N. Nikollskly) 180
Preparation of drawings (Ye. B. Inneruan) 202
Bibliography 212
1
. Molding Materials and Compounds
Ch..11 L-13
1. Basic properties of molding materials and compounds (P.M.
Platonov) 213
2. Clanalfication and specifications of molding sands (O.V.
Kolacheva) 223
3. Refractory materials for large Iron castings % V. Kol-
achava) 229
4. Clanalfication and specifications of molding clays (O.V.
Kolacheva) 230
5. Classification and specifications of special bLidIng
agents (0.V. Kolacheva) 233
Caro:*/It

Handbook on Iron Castings
SOV/54-58
1)
6. Auxiliary molding materials (0. V. KolacheVa) 238
7. Selecting molding and core covqeounds; their covoosition
and properties (P. X. Platonov) 238
8. Composition of washes, glue, and special coatings (0. V.
Kolacheva) 247
9. Preparation of Initial materials, compounds, and washes
(0. T. Kolacheva) 249
10. Rqulpment for preparation of molding mat*rlals and com-
pounds (N. 1. Dunarevokly) 252
11. Mechanization and automation In the preparation and
transportation of compounds (B. P. Yegorov) 265
12. Safety measures 274
Bibliography 275
Ch. IV. Kaking Holds and Cores 276
1. Tools for sold trImalnS (I. P. Yegorenkov and 0. X.
Xjkol ~qkjy) 276
2. Nanitail, molding (M. M. Tyshemirskly 276
3. Machin* molding (V. L. Loecnlchenko~ 309
Card-75/21

i.4

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Av 1; rf)r)o-.ul rhnnk Io"m q
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i- I i tin .In the- avmm~r ;i. -1 14!%; wvr,~ T4, 'lit , 1
a r aph r) -,.,t. a 14,- r
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I h n 41 r qt e a t h xt h. v o :v~ I I t. h
10, w Pup f "l w t, C, 1.~r n r4 ,n
: i t y-)r the woitr
I izorp ; and I tabip
-nil
tr r4 ! I no tj t Ut 9 e Mt~,) go
PL uk SZSP t no t L T, ut f
Or4 :~tl PI r-31 Figa-
o rC Cl 5,
M, rTI7 - AA
Ov A 71'

G. -., Ync.
,!,L wLj L"; & -.
Concrete Construction
Using pumps ror cement In constructing electric .-ower plants. Elek.xta. 23 No 5 11452
2
9.. soathly USt of ftillan Xecossions, Library of Congress, (,ctobor 195$. Umclassiffod.

- 1: G. 1c. (Entn% )
a
KCIL'aaerf ..,L-
*Hjftaullo ad 5arA-3j4:rsUlc CUMirW of CastL-,68,-
report prevented at Conference on Comtructlon arA Utlllratlan of CwtMg EquIpment.
Gar'klY, Doc 1957.
K"hinoetroltoll, 1958, NO* 50 P. 480
( ,V/ / 4 / - /~, )

Akadadys sook Kessiftboy M. Astreficidiodidy LmUtat
rzvestin,, tm T (5m of jjw Aatre"Its rostitaft, Acehm of Selowtop
F"aMiekaja Mv VWj7) Alms-Atat 1958. 210 P, hTsta 021P 10mrUd,
9W coges Winted.
Sdo: 7*149 fteWdy; Tfth. ZO.: Z.P, Novoklm; Witerial Board: G.K. r4LUdo
X.O. MWIMWO - Z.V. Karyagina. (Secretary),, D.A. MoshkarokIrp ad V-2. I%oenbw
(Xeope~ "*)* I
HUMt . rM bwk to InUaftA for seUmmmors ad satriophvale late,
CQVI~t this lo; a collactlau of 12 artlelms, In Uw fint few wtieles
T.G. Fessabw fm&U wift the formation of stwo and plameteg describes star
chaim ont dark filsommU in the region of galactic nobulasp =I roporU on the
obeerqMUM of Ows wilik an 8" rarractor &wing tAs -Ippo Wor of 19561, and an
photometrical observation of the nortbarn zotlac&L Lt&t in Zaly 195T using a
vieval binoculw of the wathorra deolga, The resolving artieles.. written br
Ufferent watbors,, deal, mainly with problems; of spectroscoff such "
scattering of 11*t in the ationphere in the nearest infraret region of tbw
card 11-3

Nevs of the Astrophysics rbstitate (Cont.) WY/3823
apectrump oscillation of star images and its relation to the zenith Aistanc*p
degree of polarization of the prismatic spectrographo reflecting capacity of
magnesium in the ultraviolet and visible regions of the spectrum, and the in-
restigation of certain star clusters and determination o: their luminosity
functions, References accompany most of the articles.
TAMM OF COMMITS:
Fewakov, TA. Evolution of Btars and. the &rigin of the Solar
sywt4a 3
Fesenkoy, T.G. Star Chains and Dark I'llements In the Region
of Galactic Nobulao 11
Iresenkovp T.G. Observation of Xan with an 80 Refractor of the
Astre"Ical, Institate Dwr1mg the Opposition of 1956 19
ftsenkoyp TA. Northern Zodiacal Light at the Beginning of
JUY 195T 28
Card 213

~~ -- ~ v I - ~T,
I.zr-r;.- 'T'~ ~~. f tU~V~
MIKOLISKITO G.V. ...I~yby Tafthikistana. Pod red. EpIl. Pavlovskago. Voskya,
All WMO 1930. 22a p. (Akedodis Hauk "35R. TwIshikskit &111IA1, 'StAltnatAd.
Trudy. T. M. Zoologlia i pamtitologiia).
"Literatura": P. 226.
Cu 101 DLC: rjK"I. T3A13
SO: LC9 Sovit Geography, Part 11, 1951, Unclassified

tfixty, T.
T- "~'t
The fiaboo at tho Aral Iss, Moskva. 1940. 216 F. (IkUWL&ly k POSBaRiiu towsw L flOCY
"a. at"t 9- d"&~"g Ow"O 1)

NIKOLISKIT, 0. V.
"This bioloU of fishoB,* Moscow,, 191J4

*Am Upedition of
Owcow Uhiveralty
Kkollakly, 3 pp
mirtrow IFO 5
aw 194T
the Wological InstItids of the
to the RITer Amur,,"G, V,
105 and 1946 expeditims spousored by Kintatry of
Uw Flablag radustry of the UBOR to deterulne
oz- tly tbo hablUts of the flab of that area.
1016o

-mL'SKIYI, Gewgiy Vasillskiy
UTM low-hes of Ddmd Wat"s of Turk $SRO* Byul, Fook, Obsboah. lspyUto
Prirocir, otdol., Blol.s, 520 Xo.30 1947

tny' 0- V.
gedloine Taxoncmy
wIte Order Hem1culter (Floc a C rinidas) in the
Anur B"In," G. V., fflikol'skly: Appp
*Dok Akad Nauk ZM, Nova Ser" Vol LVII No 7
Material collected by Amur Rxpedition of Ro"ov
State University. Briefly describwo characteris-
tics of RmIcultor located In Awar River basin.
Submitted by Academician L. S. Berg, 26 Doc 1946.

1.
Nikollsmk-LY, G. V. ;-nd VOLF.9 A. X. - 'Q:)zta reletille, 'D t_c -:,.- ~,_' *.*.-.0 -~-rt
of the SVr-Darlya river ted," In cy,:--poRium: Akad. S.A. Zernova, R.D.-Cow-
Lanln4,rml. 194P), P. 132-43 - Bibliog: 2i; Items
So: U-1/600, 10 July 53, (LatQP1c IZ'iuriial In.-kh StAI.C.1, N,). 6.

Him- 1-,t SUM a. T.
Oleonation an Zoology In the Popular Geograpitic Utwature.0 Prircda
1b.6,0 190

Medicine - Jhvirc=ect
"The Pemeptim of ftecial Features in the Foraatim
and Davelopsent of Ichthyofauna in Water Pooervoire
in Various Oeograplileal Zonso of the UM," 0. V.
likol'okly, Icbtbyological Lab, Zool Inst, Moscow
state U, 10 pp
*Zool ZhW Vol IMIp go 2
Arplaino fccruatlon of lchthyofauna in varlous
watormhole, vh1ch ara clcwolj allIed to dqflnlte
googmphIcal moo. Materlale obtained during
studlee conducted from 1941 to 1945 at Uchinsk and
M13rgaba.
Aw

G. V.
Oaheatflah (Famil; Sllurldae) of the ftir Main,' G.
V. filkol'Bkly, S, G. Soin, 4 pp
!a* Akat So* SM, Nom Sw" Vol Ut', 11* 7
-V"Ing f I*)A stOy b7 -th*,Amr Up"itiew Of XCOCA-V
-Valfer-61V in-1-07, 12 ormplea of aboatflAsh ob-
tained having three pairs of antmums, and sharply
distinguished from ParasIlurus amotua U. geneml or-
pearance. More detailed study showed that fish un-
doubtedly representative of genus Silurus, brut dis-
tinguished both from Silums aineDsis Bara, =4 from
the European Silurus glants. Describes structure of
fink In &stail. SUI=Itt" by Azaamiclan L. S.
ikwiz. 6 jan i9Q. am 47M
I-A47r55

akn/fob 49
Medicine Food
"Upl&rittes of rntruspects Yook Ublts of
Tnek4ktw vlak,- G. T. Ntk~Llsidy, 24 pp
"Ismal Nook Owdwk 167Y ftlrodp Otdol llolog"
To I UT# go L
COWIVAse tbut met, Intam fgaing In w fam
ocawe In paeol vim the fam tic beat mWpU*&
with food. lk me fo=e this oamwo in wamwr;
In another, In vinter.
4w
41/49%5