Thermal Cyclotron Radiation from Solar Active Regions

1980 ◽  
Vol 86 ◽  
pp. 87-99
Author(s):  
V.V. Zheleznyakov ◽  
E. Ya. Zlotnik
Keyword(s):  
Fine Structure ◽  
Radio Emission ◽  
Frequency Spectrum ◽  
Solar Radio ◽  
Active Regions ◽  
Solar Radio Emission ◽  
Kinetic Temperature ◽  
Frequency Spectra ◽  
Solar Active Regions ◽  
Thermal Cyclotron Radiation

Various frequency spectra with the fine structure resulting from the thermal cyclotron radio emission from solar active regions are discussed. The conditions in sources (distribution of magnetic field and kinetic temperature over the height) are put forward which provide the frequency spectrum as a set of cyclotron lines and high frequency cut-offs. For each kind of distribution the frequency spectrum and polarization are of peculiar character. This permits one to find the conditions in the source through the properties of the observed microwave solar radio emission. To obtain reliable data on the fine structure and judge about conditions in the sources it is necessary to study microwave solar radio emission using the swept-frequency or multi-channel receivers combined with high directional antennae.

Fine structure in solar radio emission

1977 ◽  
Vol 20 (9) ◽  
pp. 975-988 ◽  
Author(s):  
P. M. McCulloch ◽  
G. R. A. Ellis
Keyword(s):  
Fine Structure ◽  
Radio Emission ◽  
Solar Radio ◽  
Solar Radio Emission

scholarly journals Structural and Evolutionary Features of Flare-Producing Active Regions During 1988-1990

1993 ◽  
Vol 141 ◽  
pp. 388-390
Author(s):  
A. A. Golovko
Keyword(s):  
Solar Activity ◽  
Radio Emission ◽  
Solar Radio ◽  
Active Regions ◽  
Magnetic Activity ◽  
High Solar Activity ◽  
Solar Radio Emission ◽  
Evolutionary Features ◽  
Siberian Solar Radio Telescope ◽  
Flare Productivity

During the period of high solar activity (1988-1990) the Sayan and Baikal Observatories of the ISTP carried out observations of the chromosphere in the H-alpha line, the photosphere and of sunspot magnetic fields; at the Siberian Solar Radio Telescope, solar radio emission observations at 5.2 cm wavelength were made. Using those observations a study is made of the evolution of “centers of magnetic activity” (Bumba, 1986) in nine active regions with different flare productivity, for which the most complete observations were available. In three cases (NOAA Nos. 5229, 5643 and 5669) they were the targets of the cooperative international Max’91 program.

scholarly journals Estimation of Magnetic Field Strength from Enhanced Solar Radio Emission

1994 ◽  
Vol 47 (6) ◽  
pp. 811 ◽  
Author(s):  
SBSS Sarma
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Radio Emission ◽  
Solar Radio ◽  
Active Regions ◽  
Shock Velocity ◽  
Solar Radio Emission ◽  
Type I ◽  
Radio Noise ◽  
Coronal Magnetic Fields

The manifestation of solar activity on radio noise records at 28.6 MHz is discussed with special emphasis on Type-I noise storms and the associated coronal magnetic fields above the active regions in time. Magnetic fields are estimated, assuming that the Type-I radio emission at decametre wavelengths is due to shock waves, by making use of the observed shock velocity. The results are comparable with the existing estimates.

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