SCIENTIFIC ABSTRACT STEPANOV, V.V. - STEPANOV, YE.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001653210017-5
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 26, 2000
• Sequence Number: 17
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

The Welding Industry
1113
Speshkov, V.V. Determining Regimes of Flaine Surface Hardening 41
ep!!povjL_V.V. Investigation of the Weldability of
__�k -
Martensitic Stainless Chrome Steel 50
Kopytov, G.T. Carbon-Dioxide-Shielded Welding With a
Consumable Electrode 71
Batmanov, V.A. Weldability of Low-carbon Low-alloy Steel
of Increased Strength 87
.Kirillov A A Investigation of Weldability of Grade
l0Y,hGSNJj~MS:lj Steel 121
AVAILABLE: Library of Congress
Card 3/3 GO/aak
2-10-59

8 ILI! V)
/,P. 7.? 0 SOV/137-59-5-10393
Translation fromt Referativnyy zhurnal., Metallurgiya, 1959, Nr 5, P 136 (USSR)
AUTHOPS-t Stepanov, V.V., Krokh, A.N., KIrillov, A.A.
r-AITLE, "SK-U" Electrodes for Electric Arc Welding
PERIODICAL. Sb. statey, Urallskiy z-d tyazh. mashinostr. !m, S, Ordzhonlkidze,
1958, Nr 6, pp 28 - 40
ABSMACT, Weld jointswith flaky surfaces are more prone to rusting under
*tropical conditions than weld joints with smooth surfaces. In this
connection "K5A" electrodes were replaced by naw "SK-U" electrodes
ensuring the formation of angular and butt welds wi+h minimum flaks
foripation on the surface (when welding in lower position). Ir-hese
eler,trodes co,-.-spctnd to the ftE50A" type of GOST-2523-51 and are
designed for wplding medium-carbon steel. The composition of the or
coating (in %)g fluorspar 18, chalk 23, Ti dioxide (electrode type)
7.5, Fe-Si (4% 7.5, Fe-Mn 7.5, kaolin 6.5, Fe-paoder, group A
and B 30, water glass 25, Thiciknesses of 1,25 - 135. 1.4 - I,',-
C, ax,d 112 and ),45 - 1.5 mm are recommended for the noating of el5iztrodes of

1~ 11149)
"SK-U" Eiectrodes for Electric Are 'deidix~g SOV/137-59-5-10393
4 mm, 5 mm and 6 mm diamter, respectively. Wire of SvO8 and MBA grade is
used. Weloing Is possible in all spatial positions of the seam and is c&rried
out with a short d-c are of reverse polarity. The mechanical properties of
the seam metal are 6b F~* 50 kg/mm2, ak 12 - 20 kgnVcm2 at room temperature.
At -400C, ak decreases down to 10 - 15 kgm/cm2. The electrodes are not sensi-
t1ve to rust. The seam metal did not show a considerable reduction of ak kilt"'
after heating up to 6500C, water quenching and holding for tan days, and after
mech,3nical aging. The following characteristics of electrode melting are
glven.~ atr = 10,4 g/a.hour, an - 10.7 g/a . hour.
0.K.
C ax d 2/2

8plq~!
0 0 SOV/137-59-5-103C4
Translation from; Referativnyy zhurnal, Metallurgiya, 1959, Nr 5, p 121 (USSR)
AUTHOR,, Stepanov, V.V.
Ji le
TIME: Investigations Into the Weldability of Stainless Chrome Steel
of the Martensite Class
PERIODICAL; Sb, statey. Urallskiy z-d tyazh. mashinostr. Im. S. Ordzhoni-
kidze. 1958, Nr 6, PP 50 - 70
,1 14 le
ABSTRACT, The author investigated weldability of 2Khl7, 2Khl3 and 3Khl3
steels. The author shows the erroneous classification of steels
with a high Cr content on the basis of estimating the weldability
by the equivalent of C. When welding these steels without, pre-
heating, HB of the metal increases up to 512 in the zone adjacent.
to the seam, while the plastic properties diminish by a factor
of 5 - 10, compared to the 0base metal in the initial state. Changes
in the cooling rate at 650 C within a range of 4 to 380C per
second do not have a considerable effect on the hardness. In-
creased C in steel within the range of grade composition causes
Card 1/2 graln growth and a sharp reduction of plastic properties ak 41

8149f.
SOV/137-59-5-10304
InvestIgations Into the Weldability of Stainless Chrome Steel of the Martensite
Class
(down to 0.5 kgrqlcm2). To prevent martensite formation, the cooling rate of
the metal has to be reduced in the zone adjacent to the weld joint down to
0,01, - O~0150C-/see. This can be achieved by welding with an energy of
1.0,000 - 12,000 ca.1/cm and using simulataneously preliminary preheating up
to 60000'.
Yu.K.
Card 2/2

18-3200
SO7, ~_-'-59-10-183/39
AUTHORS: Stopallov, V. V1. (Czindidati-I iii'
- Docent),
Batfulanov, V.
A., Sallok, 14. A.
TITLE: Electric Are IfeatInt;: of' 11,3ad'.;
PERIODICAL: Stal', IM, Nr 10, Pi) 913-916 (USSR)
ABS7RACT: Industrial tests conducted at "Elolctrostall", "Dnepros-
petastall" and "AZovotall" pla nts (:-,avody "EhAftrostall,"
"Dneprojpetostal,," "Aovstal, ") as well as at Kuznetsk
Combine (Kumietskiy kombinat) corroborated the expediency
of' are heatirw, of' the inj~ot fic ad metal. The portable
expevimuntal hist.aLlati.on Nt- are heating develor
by Ural. Heavy Machinery Plant (Uralmaslizavoct) proved
reliable and economic. An arc of' a carbon electrode 80
nun in diameter arid 300-800 itul, long and gripped by a water-
cooled holder is ul3ed. The el ;_~ctrode holder can be dis-
placed along the column of the iii.,3tallation bY 0.5 to 3 m
and turned around it by 1800. The circuit reGulates the
Card 1/3 length of' the arc viith the hel p ut' an automatic head A-66.

Electric Are Heating of Ingot Heads 75957
1
SOV/133-5~-10-18/39
Table 1
Pharapterl.qtIns c)f' elpetrip nro hentinir of insrot. held-c4-
Performance Arbit ary Ingot esignations
Figures A B C D E I F G
Type of Steel . . . . . . 40 40 38KhGN 110 110 38KhGN 45
Ingot Weight, t . . . . . 2 2 2 2 2 2 4
Time of ingot holding
before heating, min 1 2 3 22 1 4
Period of arc appli-
cation, min . . . . . . . 55 15 10 20 21 51 62
Shrinkage of metal, mm (:")-go 70-90 100- 80 8o 100
120
Arc current, amp.** . . . 700- 700- 750- 700- 750- 700-750 700-
800 750 8oo 75o 8oo 8oo
Ingots "A," "B," "C" were heated with flux OSTs-45, others with
FU-7 flux with magnesia additions.
** Are voltaget 60 to 40 v. Card 2/3

Elf.~c trix, A v(-. I If !at. i iw: o [' I tw:o I - I I;,
ASSOCIATION:
The a u t tic) i %'; c ui w, I udt,- L! 1,, 0, v 1 a h, L J
decv(~'JoeL; th'-, volumt-' plp'~ Col'-w'a!.;(Al 1)0.*~t-'1`i'-'-A
in thu, top part 01* tht-~ lw:)d met"ll , ~;o i-11I.-!", "Alt-,
of the head C~ffl 5f? Ly Y to of t"."'
total ingrot 14ei-irlit; (2) 3,iquation of, an"', nh",
phorus as woll aei carbiwiL~.%L.1011 ot, tiv-:
The authovs rec~ornun;--ntd 1':irth(2r L;tudif-,L to
effects of tumperaturo 1,')aramet(~.-r-2 on inl c~ t c,- r~y ~-, "a
tion and optixml ratt.--2. Th!~v,~ are
and 2 tables.
Ural Polytechnic Institut (Urai 'skiy politekhnJ*f::hes'kiy
L
institut Ui,,,:,i 1 Heavy Machinr--ry Plaht (Ural. 1 31,,1,' zavod
tyazlielogo mashinostroyeniya)
Card 3/3

GALAKTIONOVp A.T.; DENISOV, Tu.A.; KOPYTOV, G.T.; MASLOVp YU.A.; RK011OV,
I.P.; PETUNIN, I.V.; KOCHEVA , G.N.; KUZNMOVt A.P.; IJ=Of
N.M.; RAZIKOVj M.I.; SPBSHKOV, V.V.; STEPAHOV, B.V.9 S~
tekhn. nmuk; SHEIMOV9 B.Ye.; YUNYSHEV, G.P.; TESIKOVp
K.A.t dots., retsevzont; BAKSHIp O.A.j, dots., retsoifsent; BERMINt
P.N., dots., retsenumt; PATSKIVICH, I.R.,dote.9 retsentzent;
RUDAKOVq A.S., dote., reteenzent; FIZHB M , N.B., insh., retsen-
zent; KHRUSTALRY, L.Ya., ~nzh., reteenzent; KRUTIKHOVSKIT, V.G.,
inzh.v red. BOBROT, Ye.I., kand. tekhn. naukv red. DUGINAq N.A.j
tekhn. red.
(Welding handbook) Sprovoebaik raboohogo-evarshchika. Pod red.
V.V.Stepanova. Moskva, goo. nmehno-tekhaizd-vo mashinostrolt.
lit-ry, 1960. 640 p. (Welding) (MIRA 14:6)

s/1.35/6o/ooo/007/012/014
A006/AO02
AUTHOR-, Stepanov, V V., Candidate of Technical Sciences
TITLE-. New Achievements in Welding Engineering in the German Democratic
Republic
PERIODICAL- Svarochnoye proizvodstvo, 1960, No. 7, pp. 4o-41
TEXT- A conference on the technology of weldi was convened in Halle
(German Democratic Republic) in October 1959. The Conference was organized by
the Chamber of Engineering and the Central Institule oL_WSIIW (TsIS). The
Conference participante.came from the USSR, the German Federal Republic, the
German Democratic Republic, Czechoslovakia, Poland, Bulgaria and other European
countries. The author of this report was a delegate of TsP NTO MAShPROK. During
the stay in the German Democratic-Republic, the Soviet delegation visited TsIS, the
Heavy Machinebui.~d.4n& Maat 1M E- Thaelmann- In Magdebu , and the Chomica-
Machinebuilding Plant in Leine. TsIS is developing thecalLing7of metal surfaces
with plastics by.spraying or dipping. T~e "Folyamid-V'N*Plasties on a Nylon or
Perlon base is used for this purpose. The wear resistance of steel surfaces
coated with this material is higher than without the coating. "Polyamid-V" with
,graphite is used for coating shafts. Its electric conductivity Is low and a
layer of 0.1-0.2 mm ia sufficient to insiwe a reliable insulation. TsIS is also
Card 1/3

s/i,35/60/000/007/m/014
A006/AO02
New Achievements in Welding Engineering in the German Democratic Republic
working on method of welding plastic articles by high-frequency currents or air
heatod to 3500C. Semi-automatic welding of polyvinyl chlorides is widely used
in construction engineering. Welding Is performed by lap joints using the "TA
(TP) burner. Sheets of any thickness can be lap-welded at a speed of 14 m/min.
Tile weight of the burner manufactured by Paul Reinhardt in Halle, is 170 g. The
"W" (FS) burner, manufactured by B6rthold in Goerlitz, is used for butt-welding
without beveling of edges And filler wire. 'The weight of the b3xmer is 310 9,
the welding speed is 20 m/Oh. Gluing metals with e r ris of great
interest. It may be performed in cold or hot state and will result in high
strength Joints. TsIS developed also a plasma jet for welding conductors,
conductors, insulators w�-th high melting poizzits, for gas cutting and applying
plastic coatings. For welding heat resistant steel the Berlin Branch of TsIS
developed electrodes whose coating contains 50% T102. This coating has a good
electric conductivity, ensuring easy ignition of the are and stable burning.
It can be used for vertical and overhead welding; the crack sensitivity of the
weld metal is reduced. The electrodes are 6 mm in diameter and can be used for
Card 2/3

S/1_35/60/000/007/012/014
A006/A002
New Achievements in Welding Engineerl-ng in the German Democratic Republic
building-UP 5-8 kg metal p6r hour. The Kjelberg plant designed a pistol for arc
weld:Lng of 6-16 mm pins ~o steel surfaces at a welding current of 250-1,250 amps. V/
There are 4 figures.
ASSOCIATION: Ural'skiy polittekhnicheakiy Institut Imeni Kirova (Ural Polytechnic
- Institute imeni Kirov)
Card 3/3

KOZL4DV, N.A., inzh.; STEPANOV, V.V., kand. tekhn. nauk
Regional scientific technological seminar of Ural Mountain
region welders. Svar. proizv. no.6t47-48 Ut N 163. (MIRA 16s12)

-1. - 1. - ' -
- , W, . I I I',- !1- 7.. r~ ;~ ' ! rj A j , !', r i '- _I ~. , : - ; : . : :j , 1 .1 . .. I , I :. ~ . ,
, . . , I .
Ne.; ,he a-- :E:-.*.,- - Er,: An-i
elcctri c wi:idi ng ~ 1 ~-, --t -~eF I ~Ibcr s t , N: ; --., .-- - z-~iia
n-i 3 ~ I-, , , ~.. .. il (:IT il e ! -.
I ", . .7,

STEPANOV, V.V., kand.takhn.nauk; LELEKO, N.M., inzh.
Automatic portable-type equipment for the electric heating
of ingota and c-astings. Sbor. at. NIITIAZHMASHa Uralmahsavoda
no. N117-131 164. (MIRA 170)

SHULY A X p V. S. ; A ~-*Ov, V AT.
Crveral". me&anization and automation of the section for cacting
in Gholl mGlOs. Lit. proizv. no.12:23-24 D 164.
(MIRA 1f'.:3)

^YNCPCV
surf ace. Fl z.
7 no.
n 'it! r 3

LOFA.IFV, B.Ye.; -SHTENGELIMMER,
~f flufos, used In electric a-iBg arid heating.
1vtor.i.mmr. 1~ no.11.28-30 u 165,
Uj-~Ilr!dy poll takhnichomkiy Institut im.
-.rcv. 1,4-,Tayev). 2. rrstitut raotd1lurgli
(rat -30. SubmAtted Octol-or 13,
.Y
(MIRA IP:12)
S.M.Kirova Mr
Im. %A..&ykc,.ra
1,964.

h000080 SOITFrF, CODF:
AUMOR.- Rprisovich Ye. 3; Priabraih,-n,;kIy 3 t 2
3 ~Mgnov V. V0
4
ORG: lutitutg of P~Wdt-j--WPS;PR (Institut fitiki
zemli AN SSSR) ,1q, t; 5.
TTTLEi N-002 three-channil soismic pon-recorder 0
L ;PO
SOURC9: AN 531R. Tnstltut fizikl zemill. Trudy, no. 33, 1964, 30-35
TOPTC TAGSI noismograph, soismologic Instrumnt, seismography, electronic circitit
ABSTRACT: This Is a hot-linn recorder which was developed and tested at the lllibro-
pribor" Plant and which assttrryr~ clear r,3cords of seismic vibrations In the range fro
0 to 3 cps at a doOln amplitude of up to 20 mm. nits instrument was designed for
usn as tho rocorder for capacitance or magnotoelectric seismographs usingUPN ampli-
finrs (schomatics for principal circuit, kimmatic circuit, electrical circuitt Phot
graph of instrument, am] dia am of hot pen are given), OrIg6 art* has! 5 figures,
1 tableo 'Lfj-':~3B: V, 1, ... jr
SUB COMI.: FS, M ;VD11 DATE: none ORIG REF: 002
Card

r
A C NR, AP6012280 (N) tOURCE CODE: UR/0125/6S/000/011/0028/0030
AUTHOR: Stepanov, V. V.; 49payev, B. Ye.;.Shtengellmayer, S.-Y.- 117
~6
ORG: (Stepanov, Lopayev] Ural Polytechnical Institute Im. S. M. Kirov (Urallskly
politekhnicheskiy institut); (Sht ngellmeyer) IMET im. A.-A. Baykov
TITIX., Viscosity of fluxes used for electroslgg melti and preheating
SOURCE: Avtomaticheskaya svarka, no. 11, 1965, 28-30
TOPIC TAGS: electroslag melting, calcium fluoride, calcium oxide, magnesium oxide,
fluid viscosity
ABSTRACT: The authors study viscosity as a function of temperature in 11 calcium
fluoride fluxes recommended for electroslag melting and preheating. It is found that
the viscosity of the calcium fluoride melt is low (0.2-0.3 poise) when heated above
the liquidus curve (At = 400C). Components which lower the crystallization tempera-
ture of the melt also reduce the viscosity due to an increase in superheating above
the liquidus curve. Additives which raise the crystallization temperature increase
the viscosity. Examples of Impurities which reduce the viscosity are sodium fluoride
and cryolite, while calcium oxide and magnesium oxide increase the viscosity by ra.Ls-
Ing the crystallization temperature. Calcium fluoride fluxes containing magnesium
UDC.- 621.791,92.04

L 1799.1-66 EIIT(m)/EWA(d)/EIIP(v)/T/34P(t)/EWP(k) JDIJUT
ACC NR, AP6od6j9o_ _'ij~CE CODE: UR/0135/
so
5
AUTHOR: Stepanov, V._ V. (Doctor of technical sciences); 1~ozlov, N. A. (Engineer)&g'
ORG: none
TITLE: All-Union Welding Conference in Sverdlovsk
SOURCE: Svarochnoye proizvodstvo, no. 2, 1966, 44-45
TOPIC TAGS: welding, friction welding, explosive welfflng, ultrasonic welding, vacuum
diffusion bonding, electron beam welding, pressure welding, plasma welding, cold
welding, electroslag welding, submerged arc welding, resistance welding, pulsed arc
welding, surfacing, pulsed arc surfacing, brazing, welding machiner7
ABSTRACT: The All-Union Scientific Conference on Weldjng_wqE_)je~k4 in
18-20 Novep The conference was attended by representatives of 252 organiza-
tions from 112 towns.Y'Problems of new welding techniques and improvement of weld
qualitywere discussed. A. S. Gellman and K. V. LynbavskjZ, Doctors of Technical
Sciences (TsNIITMASh), read a report on new welding methods and prospects of their
application in machine building. Friction-explosive, ultrasonic, vacuum-diffusion,
radio- frequency, resistance-are, electron-beam, and other welding methods developed
during the last 5-10 years were discussed. S. M. Tazlba, Candidate of Technical
c-
Sciences j3ajjESJ0... speaking about new welding equipment, pointed out that the ele
Card 1/3 UDC: 621.791:006.3

L 17993,
ACC Nks
trical equipment industry turns out at present about 180 different types of welders
and special welding machines. The 1964 output of tkis equipment was 4 times that of
1958. New equipment includes silicon and seleniumliectifiers for 120, 300, and 500
ampcurrent and multistation rectifiers for 1500 and 2000 mV, semiautomatic light-
weight welders for carbon dioxide-shleldedarc weldin Jautomatic plasma welders, and
three-phase welders for gas-shielded are welding. It is expected that lot production
of the UGER-300 type units for gas-shielded arc cutting of ferrous and nonferrous
metals will begin soon. Among new equipment an important allotment Is set for
pressure-welding machines (reeistance, contact are, friction and cold welding, ultra-
sonic welding, diffusion welding, etc.). B. S. Bril' , Chief Welder, outlined the intro-
duction and development of new welding techniques in the Central Uraleconomic region
and stated that during the last seven years the number of welded structures in general
machine building increased two times and that in metallurgical machinery, three timse
A number of Ural plants have large specialized welding shops. The share of mechanizel
welding rose from 31% in 1958 to 52% in 1965. The use of resistance welding in-
creased 4.4 times, that of electroslag veldingr3.2 times, and that of submerged-arc
welding 1.3 times. 1. F. Kobzev, Chief Welder of the Chelyabinsk Tractor Plant,
stated that dern mechanized ;We-]ding methods are applied in making tractor sub-
assemblies.Csoubmer d~arc welding, resista4ce welding, friction veldin lectroslag
welding, sed-arc welding qLnd hf-brazinglare among the methods use P "A. EsIkov,
Candidate of'Technical Scietibes, reviewed scientific research on welding carried out
at the Chelyabinsk Polytechnical Institute. The weld strength of new improved types
2/3

L 17993-66
XCC NR, AMo6i0b -
of weld designs, new welding materials, joining and repair weldIng of heavy castings,
and surfaciog with a vibrating electrodel fere discussed. M . K, Luahpe y, Ye. R. i
i Khismatulin, and A. G. Kolmakov, Engineei ~ (NIMIWASha) , reported on welding of heat-i
,treated medium-alloy steels in making high-pressure vessels* (ND)
SUB CODE: 13, 11/ SUBM DATE: none/ ATD~PRESS:-'~I
jw

Ste
Va.
,Wzuoso
Z N-if A
iso -
.or 11'reb
- 161
two 4

.-~Jn FA No r r.4.
121 r V,
ST"."Ov. V.Ya.; HASLOV. V.P.
Vasalemma facing stone; its origin and its durability in structures.
(In: Akademila nauk SSSR. Voprosy petrografii 1. u1noralogil. Moskva,
1953. voi. i, p.46o-473) (NIJIA 7:4)
(Building stonos)

STEPANOV. V.Ye., inzh.; CHEBOTAREV, Yu.P.. inzh.
Dispatcher communication apparatus with harmonic selective
sigimling. Avtom., telem.i sviaz 2 4:16-20 Ap '58-
(MIRA 12:12)
(Rallroads-Signaling) (Oscillators, Alectron)

STEPANOV, V.Ye.,
Method of allculating, call fr,3rjuinctes in dial-type co=unic3ticfj
systeran. Yost. TS1111 MPS no. 5-18-23 Jl 1.58. (MIRA 11:rl)
(1bi1rc.As-Cc,mmuni(wt ion systems)

CHIBOTAHEV. Tu.P.. Inzh.; STIPANOT, T.Ts., insh.
Duplex amplifiers without differentiating system@. Avtome
telem- I eviax 3 no.9:7-11 3 059. (MIRA 13--1)
1. VessoyusyWy natichno-teeledovatel'skly Inatitut sheles-
nodoroshnogo transporta.
(Transistor suplifterO

GHJKBOTARXV, Yu.P., Imnd, takhn. rAkuk;STIPANOV, V.Ye., insh.
Amplifiers without differentiating systems operating in dispatcher
networks. Artom. telsm6 I sylas' 3 no.21:10-1,3 N 159 (NnA 13:3)
(Transistor amplIfUrs) (Railroads--Zlectronio e(pipment)

STIPANOV, V.Ye., inzh.
Iffect of interferences on the receiver of harmonic selective sigmling.
Vest. TSNII MPS 19 no.3:46-50 16o. (MIRA 13:10)
(Ilectric railroads-Signaling)
(Radio frequency modulation-Receivers and reception)

STEPANOV, V. Ye.
Cand Tech Sci - (diss) I'System of tonal selective call for train
dispatcher communications." Moscow, 1961. 16 DP; (Ministry of
Railways USSR, Leningrad Order of Lenin Inst of Railroad Trans-
port Engineers imeni Academician V. 14. Obraztsov); 200 copies;
free; (n, 6-61 sup, 226)

USTINSKIY, A.A.; starshiy inzh.; LYUBIMJV, A.V., inzh,;
SIIATOKHINA, A.A., i Y.OVGANKO, E.I., starshiy laLorant
Measures for improving railroad radio communications with selective
ringinr. Avtom., telem. i.sviaz' 6 no-3:21-25 Mr 162.
(MIRA 15:3)
1. Rukovoditel' laboratorii provodnykh i radioreleynykh svyazey
Vsesoyuznopo nauc)-no-issledovatel'skogo instituta zheleznodorozbnogo
transporta Ministerstva putey soobshcheniya (for Ustinskiy).
2. Laboratoriya provodnykh i radioreleynykh svyazey Vseroyuznogo
nauchno-iss].Pdovatel'skogo instituta zheleznodoro7hnogo.transporta
Ministprstva putey soobshcheniya (for Stepanov, Lyubimov, bhatokhina,
Yovpanko).
(Railroads--Communication systems)

STEPANOV. V.Ye., kand.tekhn.nauk; CHEBOTAREV, YU-P-., tekhn.nauk
Railroad comminication equipment with selecti audio ringingo
Av-tom,, telem.i sviaz2 6 no.,4:9-10 AP 162. (143RA 15:4)
(Railroads-Communication systems)

CHEBOTAREV, Yurly Pavlov.i.~,-h. 21Lj~.ANOV
-, Vladimir Yevgenlyevich;
TUNIARKINA, I.I., rri~.
[Station selective counnunication system with voice-
ft-equency ringing] Pootnntsionnaia lzbiratelInala sviaz'
S tonalIrrym vyzovc,.T. M11r,:Ava, Transport. 1965. 79 p.
(MIRA 18:7)

USSR/Phyelcs Jul/Aug 48
Solar Phenomena
Sunspots
ORegularitles in the Formation Of Sunspots," V. Is.
Stepanor, Astronomical Observatory, L'Yov State U
Imeni I. Frank, (4 pp
*Astron Zhur* Vol XXV, No 4
In7eatigates relation between occurrence of sun-
spots and position of sun's magnetic axis, using
data from Greenwich and USSR observatories.
4MP 14/49T103

ZTEFANOV, V. YE.
Sun-Prominences
Observations of chromospheric ejections.
UchazapeLlvovoune 15t No. 4, 1949-
9. Monthl List of Russian Accessions, Library of Congress, August 1952-XM, Uncl.

STK?AI.ICV, V. YE.
Sun Spots
Electrom-,gnetic nature of sun spots.
Uch.zap.Llvov.un 15, No. 4, 1949.
9. Monthl List of Russian Accessions, Library of Congress,August 1952 W, Uncl.

STIEPPANOV, V-Ya.. datsent.
ll~--Vopx -Methods for determining temperatures of sunspots. Dop.ta
poy.Liviv.un. no*4, pt.2*73 153. (MLRA 9:11)
(Sunspots)

STEPAIM, V.Ye., doteent; KOPYSTTANSKIY, A.A., starshiy nauchnyy
Diffraction spectrograph with double image and great resolving
power. Dop.ta pov.Llviv.un. no.4. pt.2:74 '53. O"k 9:11)
(Spectrograph)

SWIRM, A.B.; STZPANDV. T.Te.
First observations of magnetic fields of sunspots at the
CrlnwzmL Astrophysical Observatory. Isv.Xrym.&strofix.oboqro
16:3-11 '56. (KIRA 13:4)
(Sunspots) (Magnetic fields)

STEPANOV. V.Ye.; KLTAKOTKO, N.A.
Large-scale notions In subphotoopheric layers of the sun.
Izv.Krym.&9trof1z.obser. 16:80-99 '56 . OGRA 13:4)
(sun)

STAPANOV, V. Ye.
Problems In determining the temperature of mwsPotse Soob.
GkUSH no.100:3-36 '57. (Him 12;1)
(ghmspots)

sm"Ov, V. To.
Distribution of the intensity f orA34M. 3670, 4370, 4625,
5310, and 6055 A. at the border of the sung@ disk, Soob.
OAIMI no.100:36-50 '57. ' (MIR& 12:1)
(Spectrun. Solar)

PAMOV, V. To.
Stopped structure of sunspot penumbra. Soob.0415H no.100:51-
56 '57. (NIPA 12: 1)
(sunspots)

14Y) Iffv t~
NIKULIII, N.S.; SIVIMN"', STIPAHOV~, V.Te.
Heamtring weak magnetic fields and radial velocity on the molar
MWface-Astron. tair. no. 183:9-13 -T1 '57. (MM 11939
1. Krymkays astrofixicbeskaya obmarvatorlyn.
(Photoelectric measuremonts) (Magnetic fields)

STEPANOVO V.Ye. j PXTROVA, 11,U.
Polarities and maximum strongrth of vagnptic fields of
sunspots In 1956. IsvArys.astrafix.obser, 18:66-93 138.
(sunspots) (*,.gnetIc fields) OG" 130)

STIPANOV, V.Ye.
local magnetic fields, fine chromospheric structure, and filaments
in the line H#(, Isv. Irym. astrofis. obser. 20:52-66 '58.
(MIRA 13:3)
(spectrum, Solar) (magnetic fields)

67215
j- SOV/58-59-7-16531
Translation from, Referativnyy Zhurnal Fizika, 1959, Nr 7, p 267 (USSR)
AUTHOR, Stepanov, V.Ye.
TITLE. The Absorption Coefficient of Atoms in the Reverse Zeeman Effect In the
Case of an Arbitrary Direction of the Magnetic Field
PERIODICAL; Izv. Krymsk, astrofiz, observ., 1958, Vol 18, pp 136 - 150 (English
r65umb)
ABSTRACT, The author carries out a classical calculation of the complex refractive
Index and absorption coefficient of atoms In a magnetic field of arbitrary
direction in the simplest case of triple Zeeman splitting. In the general
case when a blending of the Zeeman components Is present, the absorption
decomposes Into two Independent parts with the coefficients S+ and s_,
corresponding to the mutually orthogonal polarization of the absorbed
radiation. The character of the polarization of each component depends
on the direction of the magnetic field and, in addition, varies with the
frequency within the line limits, In the general case elliptical
polarization takes place, which changes into linear polarization in the
Card 1/2 line center and Into circular polarization at the two symmetrical points.

67215
sov/58-59-'1-16531
The Absorption Coefficient of Atoms in the Reverse Zeeman Effect in the Case of an
Arbitrary Direction of the Magnetic Field
In longitudinal and transverse fields, as well as in the case of the complete separation
of the Zeeman components, the polarization of the s+ and s_ components becomes independent
of the frequency. The mutual orthogonality of the two absorption coefficients enables one
to make allowance for them independently of one another and to set up two independent
transfer equations when solving astrophysical problems. The bibliography contains 12
titles.
L.A. Vaynshteyn
Card 2/2

81463
/1:2/ 0 SOV/35-59-8-6359
Translation from- Referativnyy zhurnal, Astronomiya I Geodeziya, 1959,
Nr 8, p 3B '
AUTHORS, Nikulin, N.S., Severnyy, A.B., Stepanov, V.Ye.
TITLE: 1~v Solar Magnetograph of the Crimean Astrophysical Observatory
li-S
PERIODICAL. Izv. Krymsk. astrofiz. observ, 1958, Vol 19, pp 3 - 19 (Engl.
summary)
ABSTRACT: A device of the Crimean Astrophysical Observatory of AS USSR,
designed for measuring weak magnetic fields is described. The
device is based on the design of Babcock magnetograph (RZhAstr,
1955, Nr 3, 1072). The measurement method Is based on the
alternate suppression of the components of magnetically split
absorption lines. It is shown, on the example of the line
5250.218, that the fluctuation of the flux amounts to 0.8% when
this line is split in a field of t'-10 gauss. A theoretical
analysis of the capacities of FEU VEI photomultipliers, employed
jointly with the tower telescope of the Crimean Astrophysical
Card 1/3 Observatory, yields - 0.2 gauss as a limiting magnitude of

~1103
SOV/35-59-8-6359
Solar Magnetograph of the Crimean Astrophysical Observatory
measurable fields. A 10-m spectrograph with a grid producing the light
concentration of the 5th order In the green region (dispersion is 0.2 A/mm)
Is used In the design of the magnetograph. Two slits, 0.04 A wide each,
separated from each other by 0.06 A are located In the spectrograph focal
plane. In front of the entrance slit of the spectrograph, there is an electro-
nic optical modulator, a plate of ammonium hydrophosphate out out perpendicular
to the crystal axis. When the voltage r1 4.6 kv) is fed to the plate, it be-
comes double-refracting; if the voltage is varied, one can modulate by the
circularly polarized signal. In this way, a constant flux cp with the modulated
addition (~ T hits the FEU photocathode through each of the exit slits. Signals
from two FEU are fed into a differential amplifier employing a 6N2P tube; the
oonstant components of the anode voltage are mutually compensated in the ampli-
fier, and the modulated (at a frequency of 124 cps) signal is doubled. Then
the signal is amplified in narrow-bandpmplifier (of the 28-IM type) and, after
demodulation, is recorded by an EPP-091,3
self-recorder. The modulation is performed
by an electromagnetic relay which is fed through a phase-inverter from a fre-
quency modulation pickup and which is connected, through an RC filter, to the
Card 2/3

8lh63
SOV/35-59-8-6359
Solar Magnetograph of the Crimean Astrophysical Observatory
control grids of a differential cathode follower. In distinction from the
Babcock magnetograph, the compensator of radial velocities functions auto-
matically. When the lines In the exit slits are displaced, a difference in
voltage arises between the PEJ anodes. This difference is amplified by the
amplifier and gives rise to the rotation of a line-shifter which brings the
line back into a symmetric position relative to the slits. The method of
adjustment of the device Is described. The authors show the reproducibility
of recording, the recording at different time constants and different slit
heights. The operational slit height is 10 to 30". An example is presented
of the chart of magnetic intensity isolines for a portion of the solar surface.
G.M. Nikollskiy
Card 3/3

SOV/169-59-3-2997
Translation from: Referativnyy zhurnal, Geofizika, 1959, Nr 3, P 139 (USSR)
AUTHOR: V.Ye.
TITLE: on the Theory of the Formation of Absorption Lines in a Magnetic
Field and of Fe N 6173 X Line contours in a Sunspot Spectrum
I "
PERIODICAL: Izv. Kr-jmsk. astrofiz. observ., 1958, Vol 19, pp 20 - 45 (Engl.
Res.T
ABSTRACT: The article has not been abstracted.
N
Card 1/1

P735?
7 35/60/0-X/012/015/019
AOOI,/AO(,)'
Translation from: Referativnyy zh-arnal, Astronomiya i Geodeziya, 1~6C,, No. 12,
PP. 52-53, # 12292
AUTFORS: Stganov, V. Ye., Petrova, N, N.
TITLE: Brightness of Floccull, Magnetic Plelds and -Heating Me~ruiisms
PERIODICAL: Izv. Krymsk. astrofiz. observ., 1959, Vol. 21, pp. 152-179 (English
summary)
TEXT: In fields with H 70 gauss,
the brightness of flocculi decreases with increasing field Intensity. AS a
result, formations acquire the annular structure, sometimes of irregular snape,
but centers of the rings, i. e., their darkest parts, coincide witt the strorgest
in4 --ersity of the field. Flocculi surrounding sunspots are also of the ann-ular
shape. A study of flocculi appearance variations and magnetl~ fleld--j with time
Card 1/3

87357
S/035/60/0oo/o12/015/019
A001/A001
Brightness of Flocculi, Magnetic Fields and Heating Mechanisms
has shown that magnetI2 fields affect the formation of flocc,41i. Ivonvergence and
divergence of magnetic force lines renders flocculi more compact or diffuse
respectively. The origination of a weak field leads to floccull appearance. In
regions where flares occur, the brightness of chromospheric formations does noT,
follow the above mentioned regularities on the day of a flare. There exist two
mechanisms of flocculi origination. I"he first mechanism is connected with develop-
ment of fast processes: flares and, possibly, "whiskers". in these cases the
floccula appears as a result of the flare afterglcw and the propagation of a shock-
wave. The second mechanism is also of electromagnetic nature and apparently
connected with the absorption of magnel-ohydrodynamic waves and dissipa-fton of
disturbances in regions where the in-tensity of a field, carried by the wave, is
higher than the Intensity of theerternal field. The magnitude of intensity in
magnetohydrodynamic waves is estimated. The absorption of the energy of these
waves gives rise to the heating of flocculi region at frequercies W > 0.1 Sec-
In the region of sunspots the energy of ,he waves is higher, ty 'Iwo or-lers of
magnitude, than the energy of waves in oteer regions: of the active zorc. TiiE-
regions of maximum field mwy appear as those region!F t!-,rcugh wn-llrfl~ treTrendo-.is
Card 2/3

N 35 7
S1034c-V6010001012110 1 r,/(-):9
AOO I/AOO I
Brightness of Plocculi, Magnetic Fields ard Heating Mechanisms
amounts of energy are transferred by waves from s,.ibphotospherl:~ and phctospherl;~
layers Into 4-he corona, without a noticeable absorption In the chromosphere. Tte
difficulties are listed which arise in explaining the heatirg of flcc,~ull by he
absorption of magnetohydordynamic waves. There are 29 references,
Autnors' E-ammary
-4
Translator s note: This is the P411 tranz1a-on of the original R-,jsZ!a-n
Card 3/3

n '--e
Su,A Lcnin,~rao, 19 0, 12' Y-I-)25C) ".OP. (,"air, kstronornical
US-3-R) (U,

89789
S/169/61/000/003/006/022
AO05/A0O5
Translation rror;i: Referativnyy zhurnal, Geoflzlka, 1961, No. 3, PP. 5-6, # 3042
AUTHOR: Itep ov,
_ _f
T17LE- The Mo-.1.cr, of Ca + in the Chromosphere and the Connection of the
Motlon With Magnetic Fields
PER1IOD16AL: "Izv, Krymsk. astrofiz. observ.", 1.960, No. 23, PP. 184-211 (English
SUMMM!7)
TM-1 The Krymskaya astrofizicheskaya observat!~;rlya,(Crlmean Astrophysical
Observatc-tv" carried c*.~*. me&sirements of "lie magnetic: field fr9m the
line Fe A 5',250 R, the ray speeds, apd the brightness In the line H Ca+ by the
aid of a magretograph and a recorder of ray speeds, Th-A ray speed Keld above the
active siLn regions in tte f 1 octcult axed !Aa x.4-iAis-"rbPd regions of the oll-'romosphere
was Investigated. The ray ;peedz were compared with t-e distribution of the mag-
netic fleld on the phatsspk1,,!.-:,P !eve'.. '1'he exizten..-e of w',d-3 regions with liftings
a.-id sinkings of gas I-- tilu chromosphe:~e was establ" !shed, the extens1cr, ol" whilch
attains to 200,000 lan. T'he motic;-.. In these reg.1:nz- has the ~,haracter of a large-
scale tarbulence. Trt- chara,-teristi:&I scale of -,he elements Is 5,000 - 20,000
Card 1/3

89789
57/16 916 1//(._,00/X,,1/G06/022
AckVA005
The Motion of Ca+ In the 3hrcmosphere azid the Conmkzzti,~r. of the Motion !41th
Magnetic Fields
km, and the life-time is he~urs. The total speed of the turbulent
elements is evall t-- 3.6 km/se-,. In the undist'arbed chrc:ncsphere, the average
speed of liftIng of gas Is equal to -0,96 lv;/sec, and that of sinking is +1.25 kmV
see, The area, in which the liftings proceed, is 56% of the tctal area of the
undist-arbed chr3mosphere. The total stream of -e lifted mass is eq7jal to the
sinking stream. in the f1cociall, the average gas lifting speed is equal to -0.97
km/sec, and that of sinking Is +1.7 km/sec. The sinking of gas proceeds in an
area which is more than t1arice as muoh as the lifting area. The mass stream of
sinking gas is fcur times greater than that'- of the lifting mass. Apparently, the
excess in sinking mass Is compensated by ejections of matter in Instationary
processes (flares, ~Pwhiskers% ejections). The speeds of lifting and sinking
Increase with increasirg br-Ightness of the floccull. in particularly bright
floccull, the lifting speed is on an average equal to -1.3 kmilsec, and the sinking
speed Is +2.3 km/sec. if 'he flocculus exists above a section with a magnetic
field with one polarity, the gas is sinking in "he flo2l-Llus in the line H and
lifting motions take place around the fio~2culus. III the flocculus Is Re
loca d
Card 2/3

89789
3/169/61/OCO/003/006/022
A005/AO05
The Motion of Ca 4- In the Chromo3phere and the Connection of the Motion With
Magnetic Fields
above magnetic fields of different polarities, the variation In the polarity is
accompanied by a varla-.~Lon in si&-i of the ray speed. Herear., gas sinking proceeds
over sections with an Inten5a magnetic field. In the vicinity of regions with
intense magnetic fields and high values of dIfIvar, tne zero line of speed passes
through near the zero line of the magnetic field or coincides with ihis. Between
two considerably remote sections with intense magnetic fields, two lines of zero
apeed pass through. The existence of a magnetic field considerably varies the
shape of the speed distribution cur-,re. Speeds of ))(I >,- 1.2 km/sec occur twic-e as
much and higher more often than In the absence of a magn5tio field. The general
character of motion above magnet',-,~ fields corraonata-s thA --rnception on a gas
mot1cn a1orig the I-ubes of rorce of a magnetic field,
Author's summary
Translatorss note; This i's the Pull translation of the original Russian abstract.
(1,Ard 3/3

BOYARCMX, A.A.; yEpimoV, Yu.S.j-'STEPANOV, V.Ye.
Magnetic intensification of absorption lines. izv.Krym.astrofize
obser. 24:52-77 160. (MM 13t12)
(Magnetic fields (Cosmic physics)) (A-boorption spectra)

22105
AGO I /A 10 1
0
AUTHOR: 3-tepanov, V.Ye.
TITLE: nie determination of' magns-tic tl,~?Id grddlent- in ttie sun,j pt,.otospherp
PERIODICAL: Referativnyy ZhUrnal, Astronomiya I Geodeziya, no, 3, 1961, 53, ab-
stract 3A1153 (" Izv. Kry-msk. astrofiz. observ." , 1940, v, -~-2, 42-48,
Engl. summary)
TEXT: Magnetic fields at two photcspher1c levels, d1i'f'ering in altitude,
are determined from the reccrd~~ of the- 1-~ngltudinal cl majznetf~~ flE-ld In-
tensity in the, active zone ~3f tne Sun's surface, Tade wii~ti ttc- magmetograph, --f ti,e
Crimean Aztraphysi~~al Observatory AS USSR, cri the ba-s-Is of' near and f'ar wings of
the NaD I line. It has teen established that magnetic i'-Ield in the pho!'-:E~phere in-
r~ 0,026-C.0' -, 3
g uss.
creases with the ttepth, and ItF cnauge is equal on an averaga - ::
km. There are 6 recerences.
Aut~,or's slummary
[Abstracter's note: Complete translation]
Card 1/1

29108
S/035/61/000/)09/030/0-36
3, ISVO A001/AlOl
AUTHOR! Stepanov, V.Ye.
TITLE; Dependence of solar magnetograph readings on the strength and
orientation of the field
PERIODICAL- Referativnyy zhurnal. Astronomiya i-Geodeziya. no. 9. 1961, 58, ab-
stract 9A519 ("Izv. Krymsk. astrofiz. observ.", 1960, v, 23, 291-
298, Engl, summary)
TEXT: The author considers the problem of the range of strength variation
of a magnetic field, measured with a solar magnetograph, for which the signal
in the magnetograph still remains to be proportional to Hcos r, where pis angle
between vector H and the line-of-sight. The signal in the magnetograph, while
measuring the Zeeman effect in a corresponding absorption line, is proportional
to function ~ (H,'P) determined by the profile of the line. The author uses
the theory of origination of absorption lines at the Zeeman triplet effect and
a certain model of the photosphere; he calculates the profile for the FeI line Py
~ 5250 and the magnitude of signal deviation in the magnetograph from the pro-
portionality to the Hcos-y-value, The calculation is carried out for both in-
Card i/2

29498
S/0-35/6 1/000/009/030/036
Dependence of solar magnetograph readings ... AOOI/AlOl
finitesimal narrow and Finite widths of the magnetograph output slit, At a
finite slit width (0.035 A), the signal in the magnetograph is proportional to
Hcos -j, for H -,'- 200 gauss. For higher values of magnetic field, underestimated
field strengths are obtained. In large sunspots, where ~-, - and T -ccmponents
can be observed simultaneously after the analyzer (depolarization effect), these
estimates of accuracy are inapplicable, In the case of a longitudinal effect in
the D, Na-line, at symmetrical position (in relation to the core of the line) of
the magnetograph slits, the signal is proportional to field H at H _e- 500 gauss.
In this case it is still possible to determine the gradient of the magnetic
field by singling out, by the slit, of different sections In the line wing, For
large field magnitudes, even at a purely longitudinal case, underestimated values
of field vector are obtained. There are 8 references.
E. Mogilevskiy
(Abstracter's note; Complete translation]
Card 212

3/058/6 1/'000/007/t 14/086
J4.-3 A001/A101
AUTHOR: Stepanov, V.Ye._____
TITIE: Coefficient of absorption of atoms In the reverse Zeeman effect at
arbitrary multiplicity
PERIODICALt Referativnyy zhurnal. Fizika, no. 7, 1961, 105, abstract 7Vl4("Izv.
Krymsk. astrofiz. observ.", 1960, v.24, 293-300, Engl. s,.mnary)
TMI The author proves coincidence of-coefficient of emission and coef-
ficient of absorption with reapdot to the form of their dependence on t6 wave-
length and the angle between the direction of magnetic field and propagation of
light. In his proof, the author made use of the method of decomposition of po-
larized triplet radiation in.the Zeeman effect into two beams with mutually or-
thogonal polarization. The expression for coefficient of absorption presented
in beams with mutually orthogonal polarization is generalized to the case of
arbitrary splitting at dipole radiation for such fields in which the effect of
Paschen-Back does not appear.
[Abstracter's note: Complete translation]
Card 1/1

85107
5/033/60/037/004/013/015/XX
660 fild 9, -E032/E314
Inverse Zeeman
Splitting aWd-
with Mutually
Perpendicular
PERIODICAL~ 'I rnal. .1960, Vol. 37., No. 4.,
XAstronomiclieskiy Zhu
pp'. 651 - 641.
AUTHOR: Stepanov, V.Ye.
TITLE.., The Ab~orption Coefficient in the
or an Arbitrary Multiplet
tile Transfer Equation for Light
Polarisations
TEXT.~ A magnetic field gives rise to tile splitting of
energy levels and thus removes the degeneracy. The contours
and the equivalent widths of absorption lines alter when the
magnetic field is introduced. An increase in tile equivalent
width leads to an effective increase in the turbulent velocity,
when the latter is determined from the growth curveand thus
introduces an error into the estimation of the chemical
composition., The form of the contour and the distribution of
polarisation within all absorption line can be used to obtain
information about the magnitude, the direction and also the
variation of tile magnetic-field strengtilidth altitudeo These
spectroscopic data can only be interpreted if the mechanism of
Card 1/k

85107
S/035/6o/o3?/oo4/ol3/0l5/XX
E032/E3.14
The Absorption Coefficient in the Inverse Zeeman Effect for
an Arbitrary Multiplet Splitting and the Transfer Fquation
for Light with Mutually Perpendicular Polarisations
formation of the absorption lines is known, Thus"
Unno (Ref. .1) and Warwick (Ref,, 2) have discussed the theory of
formation of absorption lines in the case of tyiplets. The
transfer equations derived by Unno are., however., not, very
useful in practice. On the other, hand, the theory developed
by Warwick is said to be incorrect. The expression for the
absorption coefficient in the inverse Zeeman effect for a
longitudinal and transverse magnetic field has been widely
used in astrophysics (Refs- 3-7). The approximate expression
for the absorption coefficient in the case of an inclined field
was given by Lorentz Ref~ 8) for some special cases
= 0 and -y = 45 ), However, in general, one has to
deal with magnetic fields having an arbitrary orientation,
In previous papers (Refs. 3-7) the present author has given
a derivation of the absorption coefficient for the case of
Card 2/t

85107
S/033/60/037/004/013/015/XX
E032/E3i4
The Absorption Coefficient in the Inverse Zeem~n Effect for
an Arbitrary Multiplet Splitting and the Transfer Equation
for Light with Mutually Perpendicular Polarisations
triplet splitting in an inclined fiel.d. Derivations were
also given of the radiation transfer equations and these were
solved for a number of special cases,. It was shown (Ref. 9)
that the effective absorption coefficient can be expressed
in terms of the following two coefficients--
.1 1 2
S; (S .1 + S2) + --(2SS 1 -,S2) s.1 n y,+-
2
2 4 2 2
(2S S -, S ) sin -Y -t (S Cosv
V4 0 1 2 1 -,S 2)
where y is the angle between the direction of the
magnetic field and the line of sight, and S S and S
0 2
Card 3/6)"
T)

85107
5/033/6o/o37/004/013/015/XX
E032/E3.14
The Absorption Coefficient in the Inverse Zeeman Effect for
an Arbitrary Multiplet Splitting and the Transfer Equation
for Light with Mutually Perpendicular Polarisat.ton
t%
are absorption coefUicients in the case of the transverse and
longitudinal Zeeman effects. S corresponds to two mutually
perpendicular polarisation states~:
2 a
(D,*L (2S Sl "S2)sjLn Y+'%',,,' iV2S 0 -,S1 -, S2) sin y-+(S I -S2) Cos Y
+ (S. I '' S2)cos Y (2)
where Du and D, are the components of the displacemenL
vector in the light wave absorbed by the atoms (Fig. 1). In
the present paper, this theory is generalised and an expression
is obtained for the ab3orption coefficient iLn the inverse
Zeeman effect in the general. case of multi-plet splitting.
Card 4/5

85107
S/033/60/037/004/013/015/XX
E032/9314
The Absorption Coefficient in the Inverse Zeeman Effect for
an Arbitrary Multiplet Splitting and the Transfer Equation
for Light with Mutually Perpendicular Polarisation
A general transfer equation is also obtained for all the
mechanisms of interaction between the medium and the
radiation for rays with mutually perpendicular polarisations.
The intensity distribution in the sub-components istaken into
account. Various theories of formation of absorption lines
in an inclined magnetic field are discussed and it is shown
that Unno's transfer equations (Ref. 1) are equivalent to the
transfer equations for rays with mutually perpendicular
polarisations in the case of pure absorption,. The formalism
developed in the present paper is shown to have advantages
over the represnetation of the transfer equations in terms
of the Stokes parameters.
Card 54

S/033/60/037/005/004/024
E032/E514
AUTHORS: Boyarchuk, A,A.,, Yefimov., Yu, S. and Stepanov, V,Ye.
TITLE- The Increase in Equivalent Widths of Absorption Lines
in a Magnetic Field
PERIODICAL-, Astronomicheskiy zhurnal, 1960, Vol-37, No.5,
pp, 812-823 1
TEXT: The theory of the inverse Zeeman effect$'developed in
Refs. 1-3 is used to determine the magnetic broadening of equiva-
lent widths as a function of the nature of the splitting, the
strength and direction of the magnetic field and the physical
state of the atmospheres. The magnetic broadening of an absorp-
tion line is defined by
q = In W (1)
W
0
where WA Is the broadened line width and W is the line width
0
in the absence of a magnetic field. The calculations are carried
out for the following lines~ FeI, FeII, NdII, EuII and LaII, it
is found that the magnetic broadening in a longitudinal field
Card 1/4

S/033/60/037/005/004/024
E032/E5i4
The Increase in Equivalent Widths of Absorption Lines in a
Magnetic Field
increases linearly with n6, where n is the number of
components and 6 is the distance between neighbouring sub-
components, It is assumed that LS-coupling is operatixre-. When
the magnetic field is at an angle to the line of sight, there
is an additional broadening due to blending of sub-component
groups with different polarizations., In this case the broadening
depends on the intensity distributions in the sub-components of
the splitting and increases with this angle. This increase is
most rapid between 0 and 50c and then tends to level off, The
magnetic broadening is proportional to the intensity of the
magnetic field for all fields observed in the atmospheres of
magnetic stars,, The broadening decreases with increasing turbulent
velocity and damping constant. The dependence of the magnetic
broadening on the number x0 of absorbing atoms is more complica-
ted, At first, the broadening increases with x., it then
reaches a maximum at x0 = 160 and slowly tends to zero thereafter,
General expressions are derived for calculating the magnetic
Card 2/4

S/033/60/037/005/004/024
E032/E514
The Increase in Equivalent Widths of Absorption Lines in a
Magnetic Field
broadening as functions of the magnetic field, the angle between
the magnetic field and the line of sight, the number of absorbing
atoms and the damping constant. It is shown that the formula
given by Warwick (Ref.9) is incorrect and cannot be used in the
calculation of the equivalent widths of lines in a magnetic field.
An estimate is given of the role played by the magnetic field in
determining the abundances of elements in the atmospheres of
magnetic stars. It is shown that the magnetic field cannot give
rise to the observed broadening of rare-earth lines and that
their excess abundance in peculiar A stars is real. A study is
also made of the effect of the magnetic field on the growth curve
for sunspots. The magnetic field tends to produce a rise of the
curve as a whole. In the linear part of the curve the broadening
is very small and tends to zero for large x 0 In order to
determine the effect of the magnetic broadenIng in%unspots, it is
necessary to plot growth curves separately for spots in the
neighbourhood of the centre of the solar disc and those near its
Card 3/4

S/033/60/037/005/004/024
E032/Z514
The Increase in Equivalent Widths of Absorption Lines in a
Nagnetic Field
limb. In order to determine the physical conditions in sunspots,
the growth curve must be corrected for the effect of the magnetic
field. Acknowledgment is made to T.. S, Galkina for assistance in
the numerical calculations. There are B fiiu-res, 4 tables and
15 references: 6 Soviet, 2 German and 7 English.
ASSOCIATION: Krymskaya astrofizicheskaya observatoriya
Akademii nauk SSSR
(Crimean Astrophysical Observatory, Academy of
Sciences USSR)
SUBMITTED: April 19, 1960
Card 4/4

S/035/62/000/005/044/098
A05-5/AlOl
AUTHOR: Stepanov, V. Ye.
TITLE: On the problem concerning the movement at various levels of the
Sun's atmosphere
PIZ-KODICAL: Referativnyy zhurnal, Astronomiya i Geodeziya, no. 5,1962, 48,
abstract 5A368 ("Izv. Krjmsk. astrofiz. observ.", 1961, 25, 154
173, English summary)
TE(T: On the basis of photoelectric recordings, the author investigates
the tangential movements in the chromosphere in the region of the floccull fields,
~-,d the movements at the photosphere level. He shows that, in the case of 70% of
all flocculi, gas flows in through their outer boundaries. The flow-in rate is,
on the average, 0.6 kn,/sec for all flocculi. At the photosphere-level, the field
of velocities has a very complicated structure. The regions of upgard and down-
ward movements of the gas have an extent that reaches often 1-5-10;~ km. In certain
parts of these regions, there are zones with opposite direction of movementp which
renders the velocity field picture multiconnected. The average characteristic
CaM 1/3

S/035/62/000/005/044/098
On the problem concerning the... A055/AlOl.
size of the movement elements depends on the maximum velocity. In the presence
0~ a v~locflty superior to 300 m/sec, 'he average characteristic size is equal to
0.5 1 The maximum velocity or large-scale movements observed in the photo-
sphere outside of the sunspots is equal to 450 m1sec. The distribution of the
velocities corresponds - as it does in the sub-photospheric layers (RZhAstr, 1957,
no. 10, 8233) - to the Pearson distribution. The R14,3 velocity is twice the velo-
city in the sub-photospheric layers; it is equal to 76 m/sec. Th6 comparison of
the movements with the magnetic field charts reveals that, in the photosphere,
matter can move easily in the direction perpendicular to the magnetic field force
__nez, and that a polarity change is not accompanied by a change In the direction
if 7his indicates the absence of the "freezing-in" of the magnetic
f =,atter. The velocity field in the sunspots and in their vicinity
a flo-o:-cff of the gas Trom the active region at the photosphere level. The
fl_,w-in of the gas through the flocculi boundaries, the downward movement of the
--as i- the flocc-ull, its flow-off at the photosphere level below the flocculi and
.-s upwara movement in the nearczt vicinity of the flocculi are indicative of the
presence of a gas circulation, similar to the circulation that occurs over the
spots. However, the flow of the gas entering the flocculi is by an order smaller
Card 2/3

Cn the problem concerning the...
S/035/62/000/005/044/098
A055/A1OI
7~~ian -he flow of the gas in the downward radial direction; this shows the reality
01 he observed excess of the downward flow of gas over the upward flow. Apparent-
ly, small-area sections do really exist in 'the chromosphere, from which matter is
ejected into the corona at enormous velocities, that are not recorded by the meas-
uring device. High tangential velocities in the chromosphere and the relative im-
mobility of the fine structure flocculi elements, observed in the H3, K3 and CaII
lines, are indicative of the localization of the exciting agent in the photo-
spheric and sub-photospheric layers. Large-scale movements, whose characteristic
Z`ze is -105 km, are observed in the chromosphere, the photosphere and the sub-
Photospheric layers. Medium-scale movements of elements, whose dharacteristic
size is 4-103 - 2.164 km, also occur in the chromosphere and the photosphere.
The existence of smaller-scale movements speaks for the hierarchical structure of
turbullent movements in the atmosphere olf,the SuAn; the turbulent movement energy
dissipation in the Sun's atmosphere is by 3 orders greater than in the chromosphere;
4n the sub-photospher'c layers, it is by 4 orders greater than in-the chromosphere.
There are 27 references.
Author's summary
[Abstracter's note: Complete translation]
Card 3/3

S/035/62/000/005/048/098
A055/A101
'j
Jkj`-~ R: Stepanov, V. E.
TITLE: Determination of the average gradient of the magnetic fiel-d-in the
chromosphere
?Z-1-10DICAL: Referativnyy zhurnal, Astronomiya i Geodeziya, no. 5,.1962, 51,
abstract 5A381 ("Izv. Krymsk. astrofiz. observ.", 1961, 25, 174 -
179, English summary)
On the basis of photoelectric recordings of magnetic fields in the
c*-romosohere (fron, lines H3, CaII) and in the photosphere (from line FE-7L5250),
t1le au-.hor determines the variation of the field strength with height. The mag-
netic field gradient at 50 gauss strength in the photosphere is 0.01 gruss/krn.
7,-e magnetic field penetrates easily into the chromosphere, and its variation
with height is slower than in the photosphere. The greater is the field strength,
the greater is the field gradient.
Author's summary
Card 1/1

45126
S/712/62./027/000/007/015
A001/A101
AUTEOR: Stepanov, V. Ye.
TITLE: Radiative equilibrium equations in atmos-iheres of magnetic stars
SOURCF: Akademiya nauk SSSR. Krimskaya astrofizicheskaya observatoriya.
Izvestiya. v. 27, 1962,140 - 147
TFXT: The author derived in a previous work published in the same jour-
1, v. 19, 1958, p. 20, equations for radiation transfer at the presence of a
magnetic field. Conditions for radiative equilibrium were expressed in -4he foi-
lowing form:
k+ ~ IV + (0) V-, + k-
4fr (4)
dw
jo- or- !m+ IV+(()) -Wr + M_
IV-(e) A4 V
4 41r
In the present work the author develops a method for calculating coefficients
Card 1/2

S/712/62-/027/000/007/015
Radiative equilibrium equations in... A001/A101
k+ and m+ on assumption of purely coherent scattering in frequency and condition
of stationary state. The expressions derived for these coefficients are func-
tions of optical depth. Under certain conditions these quantities are equal to
unity; if they do differ from unity, the amountof difference indicates the
degree of optical orientation of atoms arising due to their excitation by po-
larized light with intensities I+ and I_. Therefore, the angular distribution
of re-emission (effective) depending on direction does not follow the angular
distribution ..;hich takes place in processes of absorption. The formulae of
k+ and m+ are derived for some particular transitions, such as j - 0 ~)j = 1,
J_= I -,~ = 0. and j - 1/2 --~,j = 1/2. It is shown that equations of radiation
transfer taking Into account scattering of coherent re7emission can be solved
by the method of successive approximations, and the wanted accuracy can be at-
tained. There are 5 figures.
SUBMI-= May 190' 1.
Card 212

S/712/62/028/000/008/p2o
E032/E314
AUTHORS: Stepanov, V.Ye. and Gopasyule, S.I.
TITLE: The structure of magnetic fields in active solar
systems
SOURCE: Alcademiya naulc SSSR. Kryniskaya astrofizicheslcaya
observatoriya. Izvestiya. v. 28. 1962. 194 - 223
TEXT: The transverse and longitudinal components of the
magnetic field were investigated for an active solar region,
using the method described in a previous paper (Stepanov and
Severnyy, present issue, p. 166) The magnetic field was recorded
using the Fe X5250 X line (splitting factor 0-3/1), for which
calibration charts were available so that the absolute magnitude
of 1i and its angle to the line of sight could easily be deter-
mined. The active regions was followed for 8 days (September
1-8, 1961). Charts showing the magnitude of the field and its
orientation aide reproduced. Analysis of the charts showed that
in sunspot regions the average transverse field was higher than
the average longitudinal field by a factor of 2.3. This factor
became 1.6 and 1.7 in the penumbra and umbra, respectively. The
Card 1A

S/712/62/028/000/008/020
The structure of .... E032/E314
recorded distributions-show that the structure of the magnetic
field at the level-of the photosphere in the multi-centre sunspot
group resembles, in general, a dipole interaction pattern.
Hoi-rovor, when the distance between the sunspot umbras increases
an eddy structure appears in the penumbral region and its vicinit3s
This is due to the appearance of a finite azimuthal field
component. The direction of the azimuthal field for the leader
of the group was clockwise. The variation in the magnitude of the
field vector for the leader of the group is found to be in
excellent agreement with previous work (A.P. Severnyy - Izv.
Krymskoy astrofiz. obs., 2.2, 12, 1960). The field falls off most
rapidly in the penumbral region. The magnitude of the field at
the penumbra-photosphere boundary is 500 Oe, while the angle
between the field and the line of sight increases from zero at the
centre of the spot to 600 at the above boundary. It then falls
off slowly with increasing distance. Fig. 13 shows the variation
in the field components with distance (in units of 500 km) for the
leader of the group on April-5, 1961. A study of the bipolar
structure of the umbra of the follower revealed the presence of
strong azimuthal field components in neighbouring umbras. The
Card 2A

5/712/62/028/000/008/0
20
The structure of 9032/Z314
azimuthal component If reache's its innudinum on the 1111 W 0
The maximum value is equal to the value of H, noar the centr*
of the main umbra. The lines of force are pa(~allel to the H a 0
line and characterize the'direcilon of the azimuthal componant of
the transverse field. The variation of H, i and H 9 with * distanc
to similar to their distribution In a force-rree field with
cylindrical symmetry if it in assumed that the azimuthal components
of two force-free fields of regions of different polarity can be
added. An estisitnto 13 made of the conductivity coefficients for
the partially ionized gas in the umbra and the neighbouring photo-
sphere, using tho.magnetic-fiold data. The valuts of X 9 hl, X2
-k._e wabra a.re 12, 9 10 0 10
and X_ for ti 10 6 x 10 , 10 and 4 x 10 OOD&U60
;0' 12 11
while the results for tho photosphere are 2 x 10 9 x 10
-C 10 11' and 2 x 10 12 where IX is the conductivity along the!
0
field direction, X is the oonductivity In tho diroction perpen-j
dicular to the fielks, A is the Hall conductivity. and X is
.2 3
C6rd

S/71'1/6n/028/000/008/020
Tho structure of .... W3 2/ Eo ilk
the conductivity associj~ted with Joule losses. It turns out that
the conditions existing at the sunspot umbra or* favourablo for
the existence of near-force-froo rieuse Thoro.are'17 figuras and.
3 tables.
SUBMITIA~20: December 22, 1961
Aw -
AW
Card piz.~ 139

5/712/62/028/000/012/020
E010/E401
AUTHOR: Stepanov, V.Ye.
TITLE: The atomic absorption coefficient of light with
mutually perpendicular polarization, taking into
account anomalous dispersion in the presence of A.
magnet:Lc field
SOURCE: Akademiya nauk SSSR. Krymskaya astrofizicheakaya
observatoriya. Izvestiya. v.28. 1962. 252-258
TEXT: The author extends further the formalism developed by
D.N.Rachkovskiy (Izv. Krymskoy astrofiz. obs., v.27, 1962, 148)
for absorption coefficients with allowanco for changes of
refraction indices within absorption lines. Using his
expressions for absorption exponents and presenting different
polarizations in the complex-vector form, the author derives the
following final formulas for the effective absorption
coefficients of light with mutually perpendicular polarization
taking into account anomalous dispersion
Card l/ 4

S/712/62/028/000/012/020'*
The atomic absorption ... E010/E401
+
2
+ (36)
co~
The polarization state for these coefficients is determined by
the f ormula
DO) y ~2#* - el - It) etas (2.s Q%1n' 't + (I, - 46 900 It
VA - as) coo T
(37)
where so, sl and S2 are absorption coefficients (per one atom)
for subcomponents of splitting (so corresponds to the transition
in = 0) Y - inclination angle and 6 - a quantity depending on I
the strength of magnetic field H , refraction indices, angle yo
and representing the effect of anomalous dispersion. Its change
as a function of distance to the middle of a spectral line is
Card 2/4

S/732/62/028/000/012/020
The atomic a6sorption ... EGIO/VjO1
r4hoi-m iii tbe figure. Tho effect of' anomalous dispersion rexults*
Jn a decreame in-tim difference between the two absorption
C 0c rf j c I vil't"A8and s , for staten with mutually perpendicular
PfilarizatAon. + The autrior then.considers the effect of
-1jovia],usis J1.9persion in the magnitude of signals from the
I i I ~;al. componnnt.9 of it wagnetic field, in the
titlibal and trnnsver.
car4ii o)' an optically thin absorption line at a narrow slit of the
ma-vic-togrnph photomcter. The corresponding expressionx for these
.-il_vnala are
AN (I Cos T;
A611:%- 06) (2s, - 11 sj MO T sin 2X.
(112)
'lliese equations show that the nnomalotin dispersion effect
decroases the magnitude of' signal.5, mince 0 Fj The author
Concludes that the use of narrvow photometer slits for photo-
electric recordings of imignotic fields may noticeably Aft"tort tile
mamnitude of signals in the ense of strong niagnetic fieldso,
grauss, and inclination nngles 2 0 to 400, The
Card 3/4 -------

S/71-2/62/C28/000/012/020
The atomic absorption Ec I O/E1401
efrect on signal magnitude or anomalotvi dft4pnr~iion is negligible
for sJ*1tx used in the Crimean Amtrophyxicol Observatory for
recording magnetic fields. Tbojre in I figure.
SUB61ITTED: DO'comber 22, 1961
its
Fig. Change of IS 6 as a function
or distance to the line center. in
terms of Doppler half-widthm,
for H = 1700 Sauss, y 400
Ve X 5250
A.
41 to 11 40
Card 4/4

STEPANOV, V.Ye., doktor fiz.-matem. nauk
The 22d Symposium of the International Astronomical Union.
Vest. AN SSSR 33 no.12:71-72 D 163. (MIRA 17:1)

ACCESSION XRs AP4007513 S/0214/63/000/001/0055/0067
AUTHOR: Kuklin, G. V.; Stepanov, V. Yes
TITLEs Motion of gas and magnetic field in a sunspot
SOURCE: Solnechny*ye danny0ye, no. 1, 1963, 55-67
TOPIC TAGS: gas velocity field, magnetic field, magnetic field con-
figuration, sunspot, penumbra, umbra, effective mass rotation, rotation
templet, magnetic force line, sunspot photograph, chromosphere,
spectral line. magnetic force tube
ABSTRACT: The rotational motion of gas masses in a large sunspot vas
studied by means of several maps drawn each day. with time intervals
of 30 min to 1.5 hr. Radial velocities of gas motion changed from
day to day. The effective rotation of gas was computed from mean
radial velocities for the umbra. the penumbra, and the whole spot.
The rotation is clockwise, with a mean velocity of 179 248 m/sec for
the whole spot. The angular velocity of gas rotation in the umbra is
twice that in the penumbra. The direction of rotation of gas masses
in the spot coincides with tvists in the magnetic force lines. The
Cord 1/2 '

ACCESSION NR: AP4007513
vertical motion of gas to unstable, with rapid changes of direction.
The mean lifting velocity is -150 m/sec and the sinking velocity,
+120 m/sec. The spiral structure of the penumbra is surprisingly
similar to the spiral form of magnetic force lines. Kuklin and
Stepanov conclude that streams of gas flowing from a sunspot follow
along magnetic force lines, pass through the photospheric layer, and
go into the chromosphere. Orig. art. has: 8 figures and 3 tables.
ASSOCIATION: Inititut zemnogo magnetizma, tonosfery* i racprostrane-
niya radiovoln Sibirskogo otdeleniya AN SSSR (Institute of Terrestrial
Magnetism, Ionosphere, and Propagation of Radio Waves, Siberian Depart-
m e n t I AN SSSR
SUBMITTED: 00 DATE ACQ: 21Jan64 ENCLt 00
SUB CODE: AS NO R&F SOV: 006 OTUZR% 011
Card 2/2-

DATIDUROV, Mesrop Ivanovich., prof.; KOHOLIKOV, Nikolay Mikhaylovich,,
inzh.; LDWIOV, Yu.A., prof., retsenzentj STEPANOV, Ya.I.,
inzh., retsenzent; YJULLITSEEV, I.A., inzii.-J, -r;de-s- =RDVA,-
N.A., tekbn. red.
Naintanance and reconstruction of tumelalSoderzhanie i re-
konstruktsiia tomelei. Moskvao Tranzheldorizdat, 1962.
185 P. (MIRA 15:11)
1. Chlen-korrespondent Akademii stroitellstva i arkhitaktury
SSSR (for Dandurov).
(Tunnels-Repair and reconstruction)

STEPANUV9 le.p ekspert vsesoyuznoy kategorii po sluzhebno= sobako-
,06d6tvu.
Raising and training dogis. Voen. man. 37 no. 2:36 F 161e
(MIRA 14:1)
(Dogs-Training)

jV'J'ANOVp Yv.
Liquid disinfection. Zashch. rast~. ot vred.iba, 10 no.9,
7--9 165. (MMA 1.13111)
1. Gl.nvnyy hgronom KgrRpandinikoy stantsij zashchity rasteniy.

MUIRmlo-Sweivers, Crystal Contro1W Jan 49
"crystadnm" Ye- stepanov, 3 Pp
'TAdIo" No 1
Design of various crystedynes, and device for
checking effectiveness of various crysta]A vhen
paired v#h other elemments (zInelte paired vith
carbon arA steel, ferrosilicon vith gmphite,
etc.).
V& 26/149M

STE-,PAKOV, YE.
USM/Radlo Receivers, Crystal Controlled Apr 49
Batteries, Radio
"As Attachment for Crystal Sets," Ye. Stepazov, I p
Omdio" No 4
Photograph and diagram of attachmmt consisting of a
91wite-steel crystal and an 8-12 volt battery to
increase the range and volume of crystal sets.
PA 42A9TI1G6
42/4"206

ST--IPAI,IOV- , YE.
16
"A Low-Frequency Amplifier forte #Komsowlets' Receive!-," Irid,10, No. 7. 1949.

1 - -,
.. 1. , ,
:,, y~~. rooslat llr~:ala- q," . o, r4 C, rj. -, S. 61.
u I , I I I t
Z,~
. 1171.
SO: L-~toTl-js, "Ir;. 52,

STOPAITOV, YE-
"A Ho-,ae Mado Filament RheOstats" RacUo, No. 7, ig4g.
.1.

STEPANOV, Y9.
"iln Out put Transformer," RADIO, No. 12, 1949. Moscow. -o1949-.