Microwave type III pair bursts in solar flares

0457489 - ASÚ 2017 RIV US eng J - Článek v odborném periodiku
Tan, B. - Mészárosová, Hana - Karlický, Marian - Huang, G. - Tan, C.M.
Microwave type III pair bursts in solar flares.
Astrophysical Journal. Roč. 819, č. 1 (2016), 42/1-42/9. ISSN 0004-637X. E-ISSN 1538-4357
Grant CEP: GA ČR GAP209/12/0103
Grant ostatní: EC(XE) 295272
Program: FP7-PEOPLE
Institucionální podpora: RVO:67985815
Klíčová slova: Sun * corona * flares
Kód oboru RIV: BN - Astronomie a nebeská mechanika, astrofyzika; BN - Astronomie a nebeská mechanika, astrofyzika (ASU-R)
Impakt faktor: 5.533, rok: 2016

A solar microwave type III pair burst is composed of normal and reverse-sloped (RS) burst branches with oppositely fast frequency drifts. It is the most sensitive signature of the primary energy release and electron accelerations in flares. This work reports 11 microwave type III pair events in 9 flares observed by radio spectrometers in China and the Czech Republic during 1994–2014. These type III pairs occurred in flare impulsive and postflare phases with separate frequencies in the range of 1.08–3.42 GHz and a frequency gap of 10–1700 MHz. The frequency drift increases with the separate frequency (fx), the lifetime of each burst is anti-correlated to fx, while the frequency gap is independent of fx. The type III pairs occurring in flare impulsive phase have lower separate frequencies, longer lifetimes, wider frequency gaps, and slower frequency drifts than that occurring in postflare phase. These results provide new constraints to the acceleration mechanism in solar flares.
Trvalý link: http://hdl.handle.net/11104/0260893