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USSR
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I
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AFFAIRS
,
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COSMOS 425 LAUNCHED
CARRYING SCIENTIFIC EQUIPMENT
Moscow TASS International
Service
An Russian
0703 GMT 28 May 71
L
[Text]
Moscow—Scientific
satellite
"Cosmos
425" was launched on Thursday in the
Soviet
Union.
The
satellite has been put into orbit with
the
parameters;
initial
period of revolution
,92 ,2 minutes, maximum distance
from the
surface
of
the
earth.
511 kilometers, minimum distance
from the
surface
of the earth 262 kilometers,
inclination of
the
orbit
71 degrees.
Apart
from scientific equipment on board
the
satellite
there
is
a radio
system for
precise measurement of the
elements
of
the
orbit and
a radio-telemetric system for
transmission of data
to earth on the work
of instruments and equipment.
Equipment
is working normally.
SCIENTISTS EXPLAIN
NEW'^ SOLAR RADIOTELESCOPE
Moscow PRAVDA
May
p
5 L
[Correspondent
N.
Kamenskiy Interview with Soviet
scientists Stepanov and Smolkov]
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[Text]
Scientists of
th/ Siberi an insg&n5if '"ofj§f>rini"mflpnetism.
the
ionosphere,
and radiowave
propagation have
started
a dioramlc test
of
a
solar radiotelescope
project.
Its
complex of structures will
occupy approximately 50 hectares in
the
area near Baykal.
Our correspondent asked institute director,
USSR Academy
of
Sciences corresponding member t Vladimir Yevgenyevich
- Stepanov and
radioasftronomy
laboratory chief Gennadiy Yakovlevich Smolkov to comment oh this new project.
Bodar
Question;
What has necessitated
the
construction of such an instrument,
Vladimir
Yevgenevlch?
Answer;
The
24th party congress directives
provide
for scientific research in the
new 5-year plan with the aim of developing long-distance
communications,
television,
and weather forecasting.
Scientists
are also continuing fundamental research in
the
sphere
of astrophysics, interplanetary space,
solar physics, and solar-terrestrial
communications.
Before
us
is
the unsolved enigma
of the sun—sunsports
,
chromonspheric
flares,
and
phenomena accompanying
them.
During solar flares
a. colossal amount of energy
is released in the
form of wave
and corpuscular radiation.
The
former reach the
earth in 8.5 minutes,
and
the
latter in a matter of several days, interrupting radio
communications, upsetting the magnetic
field,
changing the weather,
and even
affecting the health of people
suffering from cardio- vascular complaints.
The
radiation level of the earth's environment during
such periods increases
to such
an extent that space
flights become dangerous.
In order to
learn how
to
forecast these
processes and,
consequently,
predict
the
geophysical
consequences
of solar flares,
it
is essential
to have
a
complete
concept
of their mechanism and dynamics.
Question;
But are
there
not many solar observatories in the world already?
Answer;
Yes,
there
are,
and our institute has
several optical telescopes
of
various
kinds.
They permit
us
to observe
the
solar surface--the
photosphere
and' the
lower
strata
of
the
solar atmosphere,
the chromosphere.
With
the aid
of an artifical
solar eclipse
in a
coronographic telescope
it
is also possible
to observe
the
upper
strata
of
the
solar atmosphere—the
cornoa—'but- not in a direct
line with the earth
but at an angle
of
90 degrees.
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Solar Magnetograph Described m
ne tail
^mr
'
During the years 1963-1966 specialises
at
the Sayan Observatory
of
the
Sib IZMIR (Siberian Institute of Terrestrial Magnet
i sin,
Ionosphere am
Radio Wave Propagation)
have worked on
the design and
testing of
instruments
for measuring the Zeeman and Doppler effects
in
the absorption and emission
lines
of solar plasma.
This
article describes
in detail
these instruments^
designed for the simultaneous registry
of magnetic
fields
and radial veloci-
The principle
of these
total vector
and three—
he Crimean Astrophysical
V
ties
in one and three lines,
line registry magnetograph
Observatory and IZMIRAN primarily
in
differs
from
those, at
t
method
foi
modulating the polarized
component
of
the light flux carrying information on strength and orientation
of the magnetic field vector and in certain design features
and tnerefore.
^
these aspects
are stressed.
In the variant
for measurements
in one line
it
is' possible
to determine three components
of
the magnetic field strength
vector-
velocity of plasma movement along
the
line of sight,
emission in-
tensity in the central part
of
the magnetically active line
and
_ the inten-
sity
of
the continuous spectrum near the
line.
The instrument
is designed
for operation with
a solar telescope and spectrograph with
the photometer
in a light-insulated part
of
the spectrograph.
The optical system and
block diagram of
the instrument are shown
in Figures
ana
4 in
the
text.
The magnetograph
in the three-line variant
is
for determining m the
first
line the three components
of
the vector
of magnetic
rield strength,
the
velocity
of plasma movement along
the line
of sight,
emission intensity
at
the center of
the magnetically active
line,
and intensity
of
the con-
tinuous spectrum near the
line;
in the second and third
lines measurements
are made of the longitudinal component
of
the vector of magnetic fiel
strength,
velocity of plasma movement along the
line
or sight and emission
intensity
at
the center of
the
line.
Figures
and
in the text
are
a
schematic representation of
the path
of the rays
in the optical system
and a block diagram of the instrument.
Instruments
or
the
first
type have
also been constructed for the observatories
of
the Academies
of
Sciences
of the Kazakh, Azerbaydzhan and Georgian
SSRs.
(Abstract
Magnetism,
o
_
D.
A.
Kuznetsov,
V.
S.
Koziovsxxy
,
Moscow, Novaya Tekhnika v Astronomii
berian Institute of Terrestrial
STEX Wave**Propagation, " by
S.
V.
Aleksandrovich,
"Solar Magnetograph of
the
Ionosphere
N.
N.
Lebedev and
V.
Ye.
Stepanov;
No
3,
Izd-vo "Nauka,"
1970,
pp
52-62)
Information
Corn
ruction of
Six-Met
telescope
5 01116
O l
C ilG
XX*iX t -t- ci -t
L c*
nreceding the
construction
:he
six-
meter teles cop
.re discussed.
Initial planning oegan
1959
at
the
ite
tronoraical Observatory under
the
diirection of Prof.
D.
D.
Maksutov.
Subsequent design work was performed for
the most part
Ln the Large Tele-
scopes
Oi.fxce
att
‘C'CiQ
Lii Xiingracl
0'Dti.cal—Kecrian.ri.cal
cotctid xiio xn
c. .ose
collaboration with specialists
and engineers
of
the Astronomical Instrument
Making Section
at the State Astronomical Observatory.
The initi-1
were approved in November i960 by the Astronomical Council and
a specie.
Jws nvva
, /^r7/
u.2-m
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