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We study the non-thermal emissions in a solar flare occurring on 2003 May 29by using RHESSI hard X-ray (HXR) and Nobeyama microwave observations. Thisflare shows several typical behaviors of the HXR and microwave emissions: timedelay of microwave peaks relative to HXR peaks, loop-top microwave andfootpoint HXR sources, and a harder electron energy distribution inferred fromthe microwave spectrum than from the HXR spectrum. In addition, we found thatthe 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 thelower-energy ($\lsim 100$ keV) HXRs. We interpret these observations in termsof an electron transport model called {\TPP}. We numerically solved thespatially-homogeneous {\FP} equation to determine electron evolution in energyand pitch-angle space. By comparing the behaviors of the HXR and microwaveemissions predicted by the model with the observations, we discuss thepitch-angle distribution of the electrons injected into the flare site. Wefound that the observed spectral variations can qualitatively be explained ifthe injected electrons have a pitch-angle distribution concentratedperpendicular to the magnetic field lines rather than isotropic distribution.

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