Accounting for the Albedo Flux in RHESSI Image Reconstructions

Details Accounting for the Albedo Flux in RHESSI Image Reconstructions Accounting for the Albedo Flux in RHESSI Image Reconstructions

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1504s&link_type=abstract

American Astronomical Society, SPD meeting #42, #15.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Solar flare hard x-ray emission over the disk of the Sun must be accompanied by a high percentage of back-scattered x-rays from the photosphere. This albedo flux is an inevitable result of the high ratio of Compton scattering to photoelectric absorption. While we know that a substantial fraction of the emission should be albedo we have been unable to separate this flux in images made with RHESSI because the albedo may be more diffuse or very closely aligned with the direct flux.
In this study we will take a fresh approach where we include the contribution of the albedo flux for a point source where we have assumed the height of the source above the photosphere as well as its up/down directivity. For this we use a Green's function approach to modify the expected count rates of the point source or alternatively determine the true visibilities from the measured x-ray visibilities. We will examine how this affects images obtained for two solar flares, one on 20 Feb. 2002 at 11:06 UT and the other on 20 Aug. 2002 at 8:24 UT. Both flares are observed in energies above 100 keV with footpoints above the visible solar disk. We will make images assuming several different combinations of the height and directivity to see how the spectrum and image have changed.
This activity has been supported by NASA and the European Community FrameworkProgramme 7, 'High Energy Solar Physics Data in Europe (HESPE).'

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