Spatial Structure and Spectra of X-Ray Sources During the 0.8 4.5 GHz Reverse Drift Bursts Observations

Details Spatial Structure and Spectra of X-Ray Sources During the 0.8 4.5 GHz Reverse Drift Bursts Observations Spatial Structure and Spectra of X-Ray Sources During the 0.8 4.5 GHz Reverse Drift Bursts Observations

Jan 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007soph..240..121f&link_type=abstract

Solar Physics, Volume 240, Issue 1, pp.121-134

Physics

3

Sun, Radio Emission, X-Ray Emission

Scientific paper

In the years 2002 2005, 38 groups of the reverse drift bursts (RDBs) were observed in the 0.8 4.5 GHz frequency range by the Ondřejov radiospectrograph. In 21 cases, which were observed at the times of the RHESSI observations, spatial structure, positional changes, and spectra of X-ray sources during RDB observations are studied in detail. First, based on the frequency drift and the spatial structure of the associated X-ray source, the events are classified as: (a) fast drifting RDBs with a compact X-ray source, (b) fast drifting RDBs with a multiple X-ray source (FM), and slowly drifting RDBs. Then, the spectra of X-ray sources at the times of RDBs are analyzed. It is found that most fast drifting RDBs (16 of 17 cases) are associated with the spectra having a distinct power-law (non-thermal) component. In contrast, the X-ray spectra associated with the slowly drifting RDBs are predominantly purely thermal (in three out of four cases; in the 26 July 2004, case the X-ray spectrum is thermal and high temperature, with non-thermal component). Two special cases of RDBs observed during the 28 October 2003, and 23 July 2004, flares are added for comparison. The most frequent events are those with fast drifting RDBs, a compact short-lasting X-ray sources, and a power-law X-ray spectrum. The individual reverse drift bursts (˜1 s duration) do not show a clear temporal association with individual peaks of hard X-ray bursts. During slowly drifting RDBs the shape of the associated X-ray source changed or expanded. Among them the most interesting one was observed in 26 July 2004, when the very slowly drifting RDBs (+40 MHz s-1) were associated with an X-ray loop-like source continuously elongating in the southwest direction. In the most cases the model of RDBs with electron beams is compatible with the observations, but in flares on 26 July 2004, and 28 October 2003, the RDBs are probably generated by some other type of an agent; we propose here a thermal conduction front.

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