Relation between cool and hot post-flare loops of 26 June 1992 derived from optical and X-ray (SXT-Yohkoh) observations

Details Relation between cool and hot post-flare loops of 26 June 1992 derived from optical and X-ray (SXT-Yohkoh) observations Relation between cool and hot post-flare loops of 26 June 1992 derived from optical and X-ray (SXT-Yohkoh) observations

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..156..337s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 156, no. 2, p. 337-361

Physics

49

Plasmas (Physics), Solar Flares, Solar Physics, Sun, Astronomical Models, Doppler Effect, Electron Density (Concentration), H Alpha Line, Solar X-Rays, Time Dependence

Scientific paper

We have analyzed the physical conditions of the plasma in post-flare loops with special emphasis on dynamics and energy transport using SXT-data (hot plasma) and optical ground-based data from Pic du Midi, Wroclaw, and Ondrejov (cool plasma). By combining the H alpha observations with the SXT images we can understand the relationship between cool and hot plasmas, the process of cooling post-flare loops and the mechanism which maintains the long duration of these loops. Using recent results of non-local thermodynamic equilibrium (NLTE) modeling of prominence-like plasmas, we derive the emission measure od cool H alpha loops and this gives us a realistic estimate of the electron density (2.2 x 1010 cm-3). Then, by comparing this emission measure with that of hot loops derived from SXT data, we are able to estimate the radio between electron densities in hot and cool loops taking into account the effect of geometrical filling factors. This leads to the electron density in hot loops 7 x 109 cm-3. We also derive the temperature of hot X-ray loops (approximately equal to 5.5 x 106 K), which, together with the electron density, provides the initial values for solving the time-dependent energy balance equation. We obtaine the cooling times which are compared to a typical growth-time of the whole loop system (approximately 2000 s). In the legs of cool H alpha loops, we observed an excess of the emission measure which we attribute to the effect of Doppler brightening (due to large downflow velocities).

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