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RATAN­600 OBSERVATIONS OF MICROWAVE STRUCTURE
OF THE QUIET SUN
T.I. Kaltman, V.M. Bogod, A.N. Korzhavin, S.Kh. Tokhchukova
Special astrophysical observatory of RAS, Saint­Petersburg, Russia
arles@mail.ru
To investigate microwave emission of the quiet Sun the observations with RATAN­600
from September, 2005 to March, 2006 in the range 6­16.4 GHz with the 1% frequency
resolution were used.
We present an analysis of observational data for several days with di#erent positional
angles. A small­scaled structure with the size of 20­40 arc sec is regularly observed with
RATAN­600 one­dimensional observations. A high degree of correlation for separate ele­
ments of the structure in the di#erent frequencies channels at all band of the observations
exists. Our estimates of an average life time are several hours. There is a direct dependence
between the sizes and life of time for separate elements.
The spectra of brightness temperatures grow with wavelength. The emission polariza­
tion is very likely negligible. The characteristics of presented observed structure are very
close to ones of a super granulation (chromosphere network) which is not su#ciently inves­
tigated in microwaves. The separated bright sources are identified with bright X­ray points
or bipolar magnetic structure.
Our modeling demonstrates that the structure of the chromosphere network can exist
in a wide spatial range, but really only the sources with the sizes of 20­40 sec of arc can be
detected at microwaves. Possible mechanisms of such radio emission are discussed.
The daily monitoring with RATAN­600 observations provides possibilities to regularly
estimate a state of the quiet Sun by emission characteristics of microwave small­scaled
structure and to trace rises of new centers of activities.
This work was supported by the RFBR grants 05­02­16228 and 06­02­17034a.