Modeling of X-Ray Source Occultation by the Solar Disk

Details Modeling of X-Ray Source Occultation by the Solar Disk Modeling of X-Ray Source Occultation by the Solar Disk

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..409s&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

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It is known, that the application of filter ratio (Al12/Be119) technique into the analysis of SXT images requires a precise image coalignment. The coalignment problems are even more serious in the case of analysis of deconvolved images with oversampling. In order to achieve the necessary alignment accuracy in this case, we have used the occulting solar limb position as a reference. The limb's position, as seen on images taken using individual SXT filters, may depend on the source temperature and the filter transmission. We have investigated this dependence using VAL model of the photosphere/chromosphere transition region. We have found a difference of 0.3 arcsec (200 km) of the limb location as seen on images taken with Be119 and the other SXT filters. The difference is even larger for individual HXT channels. Results of the analysis allow us to coalign the Al12 and Be119 deconvolved images to the required accuracy. In parallel, we also discuss implications of the occultation phenomenon on the shape of X-ray lightcurves for kernels evanescent from behind the limb. By applying filter ratio (Al12/Be119) technique to deconvolved images we have studied the evolution of temperature and emission measure of flaring kernels with 1 arcsec resolution for behind the limb sources. Obtained high resolution temperature and emission measure maps we have compared with the maps of hard X-ray brightness (HXT). We discuss physical implications of the results obtained.

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