Hard X-ray Footpoint Source Sizes

Details Hard X-ray Footpoint Source Sizes Hard X-ray Footpoint Source Sizes

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640405d&link_type=abstract

American Astronomical Society, AAS Meeting #216, #404.05; Bulletin of the American Astronomical Society, Vol. 41, p.900

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Scientific paper

RHESSI has detected compact hard (25 - 100 keV) X-ray sources that are ɜ arcseconds (FWHM) in extent for certain flares (Dennis and Pernak (2009). These sources are believed to be at magnetic loop footpoints that are known from observations at other wavelengths to be very small. Flare ribbons seen in the UV with TRACE, for example, are 1 arcsecond in width, and white light flares show structure at the 1 arcsecond level. However, Kontar and Jeffrey (2010) have shown that the measured extent should be >6 arcseconds, even if the X-ray emitting thick-target source is point-like. This is because of the strong albedo contribution in the measured energy range for a source located at the expected altitude of 1 Mm near the top of the chromosphere. This discrepancy between observations and model predictions may indicate that the source altitude is significantly lower than assumed or that the RHESSI image reconstruction procedures are not sensitive to the more diffuse albedo patch in the presence of a strong compact source. Results will be presented exploring the latter possibility using the Pixon image reconstruction procedure and other methods based on visibilities.
Dennis, B. R. and Pernak, R. L., 2009, ApJ, 698, 2131-2143.
Kontar, E. P. and Jeffrey, N. L. S., 2010, A&A, in press.

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