Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...705.1063h&link_type=abstract
The Astrophysical Journal, Volume 705, Issue 1, pp. 1063-1072 (2009).
Astronomy and Astrophysics
Astronomy
Sun: Flares, Sun: Radio Radiation, Sun: X-Rays, Gamma Rays
Scientific paper
We analyze the M1.1 flare event peaked at 07:20:00 UT on 2004 December 1 mainly from radio and hard X-ray (HXR) observations. By eliminating the thermal component from the observed total radio emission flux, the non-thermal part of the radio and HXR burst process is investigated in a self-consistent way. The spectral index of energetic electrons deduced from the radio burst evolves as a Soft-Hard-Hard pattern and that from HXR as a Soft-Hard-Soft pattern corresponding to an initial-main-decay phase. The trap-plus-precipitation model is applied in the kinetic process of energetic electrons for this flare event. The radio fluxes at six frequencies selected from the 2.6-7.6 GHz range are fitted with a gyrosynchrotron radiation mechanism. It is found that a linearly increasing electron escape rate can best fit to the observed radio fluxes from 07:00:00 UT to 07:40:00 UT and the slope of the electron escape rate for the six selected frequencies decreases with increasing frequency. During the decay phase from 07:15:00 UT to 07:20:00 UT, the hardened spectrum of the radio burst may be due to the increasing amount of trapped electrons with higher energy by a lower escape rate. Meanwhile, the increasing amount of precipitating electrons with a lower energy band may soften the HXR spectrum. In the decay phase after 07:20:00 UT, thermal emission is the dominating component for the radio burst.
Huang Jing
Yan Yihua
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