Solar S-bursts at Frequencies of 10 - 30 MHz

Details Solar S-bursts at Frequencies of 10 - 30 MHz Solar S-bursts at Frequencies of 10 - 30 MHz

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010soph..264..103m&link_type=abstract

Solar Physics, Volume 264, Issue 1, pp.103-117

Physics

3

Corona, Radio Emission, Magnetic Fields, Corona, Radio Bursts, Dynamic Spectrum, Radio Bursts, Meter-Wavelengths And Longer (M, Dkm, Hm, Km), Radio Emission, Active Regions

Scientific paper

Solar S-bursts observed by the radio telescope UTR-2 in the period 2001 - 2002 are studied. The bursts chosen for a detailed analysis occurred in the periods 23 - 26 May 2001, 13 - 16 and 27 - 39 July 2002 during three solar radio storms. More than 800 S-bursts were registered in these days. Properties of S-bursts are studied in the frequency band 10 - 30 MHz. All bursts were always observed against a background of other solar radio activity such as type III and IIIb bursts, type III-like bursts, drift pairs and spikes. Moreover, S-bursts were observed during days when the active region was situated near the central meridian. Characteristic durations of S-bursts were about 0.35 and 0.4 - 0.6 s for the May and July storms, respectively. For the first time, we found that the instantaneous frequency width of S-bursts increased with frequency linearly. The dependence of drift rates on frequency followed the McConnell dependence derived for higher frequencies. We propose a model of S-bursts based on the assumption that these bursts are generated due to the confluence of Langmuir waves with fast magnetosonic waves, whose phase and group velocities are equal.

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