OBSERVATIONS OF A RADIO EMISSION OF THE SUN AT IZMIRAN.

 

A.A. Gnezdilov, R.V. Gorgutsa, A.K. Markeev

 

The first observations of a radio emission of the Sun at the Solar Radio

Laboratory of IZMIRAN have been carried out in the 1949 year. The beginning

of regular observation, which form the almost uninterrupted 37-year-long

line of data, was connected with a preparation to International Geophysical

Year and, after that, to IQSY.

It's clear from Tables below (Bank of data... and Database...), that

in 1956 - 1957 yrs. daily (06:00 - 12:00 UT) observations of the flux

density of the radio emission of the whole Sun have been started at the

fixed frequencies 204 and 600 MHz. The observational complex was extended

in next years.

Since the January, 1961 have been carrying out the observations by

radiospectrograph 90 - 45 MHz, which register dynamic spectra of the solar

radio emission. Up to recent time there was the only regular such kind

observations in our country. Now the observations by radiospectrographs are

carrying out at a more wide frequency range, which exceed 2.5 octaves (280

- 45 MHz).

The flux density of the radio emission of the Sun at 3 GHz has

regularly registering since the October, 1967. Since the August, 1968 and

June, 1972 some programs of an investigation of the polarization of the

sol8ar radio emission at frequencies 204 and 74 MHz have been made.

An information obtained, i.e. the data bank, is kept as records of an

analog signal at a paper tape (the flux density, the polarization) or film

(dynamic radio spectra).

The main part of data has been preliminary analyzed. By this analysis

tables of observations have been compile, the format of the tables mainly

coincide with the format of data being published at "Solar - Geophysical

Data" bulletin. In the tables averaged over a day flux densities of the

radio emission at fixed frequencies, their mean variability are contained.

A times of the beginning, the maximum, and the end of events are included

in data about outstanding events (manifestations of the solar activity at

the form of radio bursts) with the value or the ball of the maximum

intensity of events and their morphological characteristics.

The main part of this tables have been publishing at bulletins "Solar

- Geophysical Data", "Solnechnye dannye" and "Quarterly Bull. on Solar

Activity". The data of the observations of the radio emission of the Sun

are widely known and are used at investigation of scientists in our country

and abroad.

The relational database "LARSBASE" has been forming with dBase IV in

1993. It is kept at a disk memory. The database being expanded by adding

data of last years observations.

An access to the database are performed with the special program

independent from dBase IV. An essential part of data may be outputted to a

printer or to a text file. By agreement the data of IZMIRAN observations of

the solar radio emission may be submitted by E-mail for scientific

investigations.

 

142092, Moscow Region, Troitsk, IZMIRAN,

Solar Radio Laboratory

(095)-334-09-02

E-mail: agnezdil@izmiran.rssi.ru

 

 

Bank of data of observations of the radio emission of the Sun

 

at IZMIRAN

 

........................................................................

. Observed Observed parameter The beginning The end

.frequency .................................

. range Flux Degree of dynamic of observation

. MHz density polarization spectra month, year

.........................................................................

. 3000 + Oct. 67 Today

. 545 + Jun. 57 Aug. 60

. 545 + Jan. 61 Mar. 62

. 204 + Jan. 56 Today

. 204 + + Aug. 68 Sep. 73

. 169 + Jan. 84

. 74 + + Jun. 72 Jul. 81

. 230 - 180 + Nov. 68 Today

. 190 - 90 + May 73 Today

. 280 - 170 + Mar. 87

. 90 - 45 + Jan. 61 Today

.........................................................................

 

Database of observations of the radio emission of the Sun at IZMIRAN

 

LARSBASE

........................................

. Frequency Data at

. range the dBase IV system

. and the SGD format

. MHz the beginning - today

........................................

. 3000 Jan.90 - today

. 204 Jan.90 - today

. 270 - 45 Jan.90 - today

........................................