On the Envelope Soliton – Like Fine Structure in Solar Radio Emission

2003 ◽  
Vol 288 (3) ◽  
pp. 293-303
Author(s):  
DE-YU Wang ◽  
G.P. Chernov ◽  
V.N. Oraevsky
Keyword(s):  
Fine Structure ◽  
Radio Emission ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Envelope Soliton

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 Dynamics of Flare Processes and Variety of the Fine Structure of Solar Radio Emission over a Wide Frequency Range of 30 – 7000 MHz

Solar Physics ◽  
2014 ◽  
Vol 290 (1) ◽  
pp. 95-114 ◽  
Author(s):  
Gennady Chernov ◽  
Valery Fomichev ◽  
Baolin Tan ◽  
Yihua Yan ◽  
Chengming Tan ◽  
...  
Keyword(s):  
Fine Structure ◽  
Radio Emission ◽  
Solar Radio ◽  
Wide Frequency Range ◽  
Solar Radio Emission ◽  
Frequency Range

scholarly journals Development of solar flares and features of the fine structure of solar radio emission

2017 ◽  
Vol 57 (6) ◽  
pp. 738-751 ◽  
Author(s):  
G. P. Chernov ◽  
V. V. Fomichev ◽  
Y. Yan ◽  
B. Tan ◽  
Ch. Tan ◽  
...  
Keyword(s):  
Fine Structure ◽  
Radio Emission ◽  
Solar Flares ◽  
Solar Radio ◽  
Solar Radio Emission

Envelope Soliton in Solar Radio Emission

2000 ◽  
Vol 17 (5) ◽  
pp. 355-357 ◽  
Author(s):  
Wang De-Yu ◽  
G P Chernov
Keyword(s):  
Radio Emission ◽  
Solar Radio ◽  
Solar Radio Emission ◽  
Envelope Soliton

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.

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