Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..209s&link_type=abstract
Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc
Astronomy and Astrophysics
Astronomy
Scientific paper
The most suitable data set available for investigation of flares has been accumulated by the Yohkoh instruments. The SXT collected a wealth of solar X-ray images including thousands of flare sequences. Over several past years, our team in Space Research Center (SRC) of Polish Academy of Sciences in Wroclaw has been interested in developing the numerical image enhancement techniques with the aim of increasing the resolution on SXT flare images. The algorithm has been worked out which allows for the image deblurring with oversampling. The code (ANDRIL) is available in the public domain (SolarSoft). The application of this algorithm allows to increase the resolution on the SXT images to the level of 1 arc sec. We performed the deconvolution of large number of flare sequences using ANDRIL algorithm. The analysis of these data allowed to study the morphology of million degree flaring plasma with the resolution comparable to TRACE. The main results will be presented in the review. In order to infer the thermodynamic parameters of the plasma from the analysis of deconvolved images their precise coalignment is required. Techniques which have been developed at SRC to achieve high accuracy of image coalignment will be presented. The application of filter ratio (Al12/Be119) technique to the deconvolved and coaligned images allows to study temperature and emission measure distributions in great details. These maps better resolve flare kernels located both at the summits and foot points of flaring loop structures. We have studied the thermodynamic properties of kernels and related them with the corresponding characteristics derived from the analysis of BCS and HXT data. Performed analysis improved considerably our understanding of solar flares. Many of the results and theoretical ideas presented in this review have been obtained in cooperation with the team from the Astronomical Institute of Wroclaw University.
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