Astronomy and Astrophysics – Astronomy
Scientific paper
May 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997spd....28.0159g&link_type=abstract
American Astronomical Society, SPD meeting #28, #01.59; Bulletin of the American Astronomical Society, Vol. 29, p.890
Astronomy and Astrophysics
Astronomy
Scientific paper
This analysis of a solar flare's macro thermodynamic-spatial structure is based on the RTV model of the dynamics of quiescent solar coronal forms (Rosner,Tucker and Vaiana,1978) and full disk soft X-ray measurements by the GOES two-channel soft X-ray sensor. The RTV model provides a relationship between maximum (loop top) temperature, T_m, and the semi- loop length, L. In order to reconstruct the flare's thermo- dynamic macro structure utilizing the RTV law one must know or be able to solve for T_m and the internal pressure, p (the latter assumed spatially constant at fixed times). From the GOES dual X-ray measurement one can derive the spatially averaged temperature, Tav, and the emission measure, EM, at any point during the flare. Treating these two derived parameters as measurements one can solve for the unknowns p and T_m if the loop length L can be independently specified. The constant crossection A can be deduced from L utilizing the theoretical relationship of the ratio L/A to T_m and EM (Sylwester,1988). Once the flare's L and A are specified one can numerically integrate over the full semi-length to compute density, X-ray emission, and the differentials of of volume, thermal energy and emission measure for equal increments of temperature; compare the computed Tav and EM with their observed (derived) values; and recover T_m and p by linearized iterative solutions. As noted everything depends on the availability of an independently obtained L. Fortunately L bears a robust physical relationship with the flare's rise and decay times and peak temperature. Metcalf and Fisher (1996) and predecessors (Fisher and Hawley, 1990; Hawley et al.,1995) have developed algorithms which permit the loop length to be estimated from X-ray light curves. These data are used to initiate a solution which not only yields T_m and p but collaterally determines L as well. Fourteen cases are discussed comparing thermodynamic results with Yohkoh SXT measured loop data. Fisher, G.H. & Hawley, S.L. 1990, ApJ, 357, 243 Hawley, S.L., et al. 1995, ApJ, 453, 464 Metcalf, T.R. & Fisher, G.H. 1996, ApJ, 462, 977 Rosner, R., Tucker, W.H. & Vaiana, G.S. 1978, ApJ, 220, 643 Sylwester, J. 1988, Adv. Space Res. Vol.8, No.11, 55
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