scholarly journals THE LARGE CROSS RADIO TELESCOPE OF THE PHYSICAL INSTITUTE OF THE ACADEMY OF SCIENCES (FIAN)

1963 ◽  
Vol 49 (6) ◽  
pp. 786-786
Author(s):  
V. V. Vitkevich ◽  
P. D. Kalachev
Keyword(s):  
Radio Telescope ◽  
Physical Institute ◽  
Academy Of Sciences

scholarly journals Polarization of 10-cm radiation of the Crab nebula

1959 ◽  
Vol 9 ◽  
pp. 305-308
Author(s):  
A. D. Kuz'min ◽  
V. A. Udal'tsov
Keyword(s):  
Crab Nebula ◽  
Physical Institute ◽  
Academy Of Sciences ◽  
The Crab Nebula

In October and November 1957 at the Physical Institute of the Academy of Sciences of the U.S.S.R. a search was conducted to detect the plane polarization of the radiation from the Crab nebula at 9.6-cm wavelength [1].

scholarly journals Radio picture of the sun at 3.2-cm wavelength

1959 ◽  
Vol 9 ◽  
pp. 129-135
Author(s):  
V. V. Vitkevich ◽  
A. D. Kuz'min ◽  
A. E. Salomonovich ◽  
V. A. Udal'tsov
Keyword(s):  
Radio Emission ◽  
Radio Telescope ◽  
Intensity Distribution ◽  
Focal Plane ◽  
Meridian Plane ◽  
The Sun ◽  
Two Dimensional ◽  
Daily Movement ◽  
Academy Of Sciences ◽  
Astronomical Station

In 1957 July the two-dimensional intensity distribution of radio emission over the solar disk was determined at 3.2- and 10-cm wavelengths. The observations were carried out on the radio telescope 31 m in diameter at the Crimean Radio Astronomical Station of the Physical Institute of the Academy of Sciences of the U.S.S.R. The radio telescope was an immovable parabolic reflector with the axis set in the meridian plane on 22-degrees declination [1]. Scanning the pattern of the radio telescope in the declination range ±32 minutes of arc to obtain the intensity distribution was done by setting the feed and preamplifier on a movable carriage reciprocating near the focal plane. In combination with the sun's daily movement it provided the two-dimensional solar distribution along a zigzag line. These sections gave the radio picture.

scholarly journals The search of radio transients in the RATAN-600 radio telescope surveys

2016 ◽  
Vol 12 (S325) ◽  
pp. 270-273
Author(s):  
Olga P. Zhelenkova ◽  
Elena K. Majorova
Keyword(s):  
Radio Telescope ◽  
Special Astrophysical Observatory ◽  
Detection Level ◽  
The Third ◽  
Radio Range ◽  
Transient Events ◽  
Radio Transients ◽  
Optical Brightness ◽  
Academy Of Sciences ◽  
Archive Data

AbstractWe present the results of the search of variable sources and transient events in the archive data of the sky surveys conducted on 3.9 GHz on the RATAN-600 radio telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences (SAO RAS) in 1980-1994. 17% of the total studied sources can be attributed to the variables in radio range. About half of them has significant variations in optical brightness according to the data of the catalogs. At the level of 3-5 r.m.s. we found three transient events. Two weak events probably associated with AGN activities or with cataclysmic events such as GRB and a supernova flash. The nature of the third event has not been established. According to our estimation the surface density of radio transients is 0.03 on one square angular degree with the detection level 8–11 mJy on 3.94 GHz.

scholarly journals OBSERVATION CONTROL DEVICE FOR THE URAN-4 DECAMETER RADIO TELESCOPE

2021 ◽  
Vol 34 ◽  
pp. 74-75
Author(s):  
V.V. Galanin ◽  
V.G. Komendant ◽  
V.V. Yasinski
Keyword(s):  
Radio Telescope ◽  
Directional Pattern ◽  
Control Device ◽  
National Academy Of Sciences ◽  
Current Time ◽  
Discrete Movement ◽  
Decameter Radio ◽  
Academy Of Sciences ◽  
Observation Period ◽  
Made In

The URAN-4 radio telescope has been operating at the Odessa Radio Astronomy Observatory of the Radio Institute of the National Academy of Sciences of Ukraine since 1986. The telescope is an element of a decameter long-base interferometer – the radio telescopes which are located across the territory of Ukraine from west to east. The URAN-4 consists of antenna and upgraded radiometer. Antenna consists of 128–element with phased array with dimensions of 232.5 x 22.5 m. The telescope operates in the 10 – 30 MHz range. Its receiving equipment is capable of separating two polarization components of the received signal. The radiation pattern of the radio telescope is 2,7x22 degrees at 25 MHz. The resolution of 2 seconds is realized in the interferometer mode. The instrumental complex of the radio telescope includes the upgraded device for controlling its operation. This device is made in the form of a separate unit. The ATMEL AT90S8515 microcontroller with registers and a communication circuit between the unit and the computer are mounted in it. The discrete movement in space of the antenna's directional pattern and sets the required attenuation in the attenuator during calibration are carried out with the upgraded controlling device at a given time during the observation period. The controlling device also allows adjust the current time of the computer using GPS.

scholarly journals 69. Disturbed radio emission from the sun as a sum of small monochromatic peaks

1957 ◽  
Vol 4 ◽  
pp. 363-365 ◽  
Author(s):  
V. V. Vitkevitch
Keyword(s):  
Radio Emission ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
The Sun ◽  
General Increase ◽  
Quiet Sun ◽  
Small Areas ◽  
Physical Institute ◽  
Academy Of Sciences

Observations of the radio emission from the sun carried out during recent years at the Crimean Station of the Physical Institute of the U.S.S.R. Academy of Sciences showed that the occurrence of spots appreciably increases the intensity of the solar radio emission in the range of metre wave-lengths. This increase of intensity has two components. The first (S-component) changes comparatively slowly with time. The second (P-component) consists of individual brief bursts (of the order of a second and less) of small amplitudes (10–100 % of the intensity of the quiet sun). The P-component is manifested most clearly in the emission connected with spots of small areas, when the general increase of the intensity is insignificant. Such a situation has been utilized for the study of the spectrum of individual small peaks.

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