Thermodynamics of partly occulted limb flares

Details Thermodynamics of partly occulted limb flares Thermodynamics of partly occulted limb flares

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.477..171s&link_type=abstract

In: Proceedings of the Second Solar Cycle and Space Weather Euroconference, 24 - 29 September 2001, Vico Equense, Italy. Editor:

Computer Science

X-Ray Flares, Thermodynamic Parameters

Scientific paper

We have studied time variations of the thermodynamic parameters for several flares which have been partly occulted by solar disc. The data consist mainly of deconvolved Yohkoh Soft X-ray Telescope (SXT) images coaligned to sub-arcsec accuracy using specially designed method. At first in our analysis we have followed the maximum brightness location for pronounced flare kernels emission seen on deconvolved images. The analysis of the data reveals systematic variations of the brightest kernel position. Spatial resolution achieved on the deconvolved images allows to derive the maps of temperature and emission measure within unocculated portion of the flaring structures (kernels) with the resolution below ~1 arcsec. It is possible to estimate the electron density of plasma confined within individual kernels based on their spatial dimensions. Our analysis indicates that the hottest regions within the flaring kernels are these with the smaller density. As a rule the cooler regions are related with the denser plasma. It is typical that some amount of plasma with temperatures T >= 20 MK is present within the flaring region during the rise phase. Derived patterns of maximum brightness location as observed on A101, A112 and Be119 filter images have been cross-compared with the location of hard X-ray emission centers as seen on the MEM-reconstructed Hard X-ray Telescope (HXT) images.

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