Quasiperiodic Electron Acceleration in the 15 June 2003 Solar Flare

Details Quasiperiodic Electron Acceleration in the 15 June 2003 Solar Flare Quasiperiodic Electron Acceleration in the 15 June 2003 Solar Flare

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp41c..04f&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP41C-04

Physics

7519 Flares, 7524 Magnetic Fields, 7534 Radio Emissions

Scientific paper

We report a comprehensive analysis of strong quasiperiodic radio- and X-ray pulsations observed from the X1.3-class flare which occurred at S06E78 on 23:42-23:50 UT, 15 June 2003. Because of the favorable time of the flare, it was jointly observed by the Owens Valley Solar Array (OVSA) and the Nobeyama Solar Radio Observatory, which allowed us the advantage of combining high spectral, temporal, and spatial resolution radio observations. In addition, the part of this event displaying the strongest pulsations was also observed in hard X-rays with RHESSI. We study the frequency dependence of quantitative measures of the pulsations, including Fourier spectra, phase differences, modulation depth, as well as the degree of (radio) polarization. We compare these measures with the expectations of competing radio pulsation models, i.e., MHD loop oscillations and quasiperiodic electron injection. Although the Fourier spectra display a few significant peaks at each observing frequency, we found that none of them can be explained by the MHD-oscillations. In contrast, the model of quasiperiodic particle acceleration/injection is capable of explaining all quantitative measures observed for this event in a natural way. We discuss implications of these findings for electron acceleration and transport in solar flares.

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