Comparative Analysis of Non-thermal Emissions and Study of Electron Transport in a Solar Flare

Details Comparative Analysis of Non-thermal Emissions and Study of Electron Transport in a Solar Flare Comparative Analysis of Non-thermal Emissions and Study of Electron Transport in a Solar Flare

2007-10-02

arxiv.org/abs/0710.0441v1

Astronomy and Astrophysics

Astrophysics

32 pages, 12 figures, accepted for publication in The Astronomical Journal

Scientific paper

10.1086/523884

We study the non-thermal emissions in a solar flare occurring on 2003 May 29 by using RHESSI hard X-ray (HXR) and Nobeyama microwave observations. This flare shows several typical behaviors of the HXR and microwave emissions: time delay of microwave peaks relative to HXR peaks, loop-top microwave and footpoint HXR sources, and a harder electron energy distribution inferred from the microwave spectrum than from the HXR spectrum. In addition, we found that the time profile of the spectral index of the higher-energy ($\gsim 100$ keV) HXRs is similar to that of the microwaves, and is delayed from that of the lower-energy ($\lsim 100$ keV) HXRs. We interpret these observations in terms of an electron transport model called {\TPP}. We numerically solved the spatially-homogeneous {\FP} equation to determine electron evolution in energy and pitch-angle space. By comparing the behaviors of the HXR and microwave emissions predicted by the model with the observations, we discuss the pitch-angle distribution of the electrons injected into the flare site. We found that the observed spectral variations can qualitatively be explained if the injected electrons have a pitch-angle distribution concentrated perpendicular to the magnetic field lines rather than isotropic distribution.

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