Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010pasj...62..755y&link_type=abstract
Publications of the Astronomical Society of Japan, Vol.62, No.3, pp.755--767
Astronomy and Astrophysics
Astronomy
Sun: Flares, Sun: Magnetic Fields, Sun: Photosphere, Sun: X-Rays, Gamma Rays
Scientific paper
The purpose of this study is to reproduce the GOES X-ray (1-8 Å) light curves of the impulsive phase of 20 solar flares and to estimate the thermal and magnetic parameters in flare loops. The expected X-ray light curves are calculated from the values of the coronal field strength and inflow velocity under some assumptions. We used the magnetic reconnection heating model of Shibata and Yokoyama (2002, ApJ, 577, 422), photospheric vector magnetic field data, and a simple 1-D flare loop model. It is found the maximum inflow velocities are ˜ 107cm s-1, and that the maximum magnetic reconnection rates are 0.006-0.9, and further that the characteristic coronal field strengths are 6-100 G. Using the thermal and magnetic parameters derived, we found that geometrically our calculated flare loops are higher than the potential fields that model the postflare loops, and are also higher than the preflare loops containing magnetic free energy that is large enough to provide the thermal energy of a flare. Hence, we conclude that the plasma β value would be near unity in the flare loops we studied, and the magnetic field lines shrunk during the decay phase. The downward velocities of the field-line shrinkage are estimated to be 106-107cm s-1 except one event. The height of the reconnection point was roughly estimated to be from 1010cm to 4 × 1010cm. We propose a new interpretation of the Neupert effect, and also discuss a temporal relationship between the X-ray flux and the flare loop heating.
Sakurai Takashi
Yamamoto Tetsuya T.
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