On the velocity of a hard X-ray source in the solar corona

Details On the velocity of a hard X-ray source in the solar corona On the velocity of a hard X-ray source in the solar corona

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24..543b&link_type=abstract

Astronomy Letters, Volume 24, Issue 4, July 1998, pp.543-548; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 631

Astronomy and Astrophysics

Astronomy

3

Scientific paper

We consider the velocity of a coronal hot hard X-ray source during solar flares and discuss possible mechanisms of its heating. The source is assumed to be heated by the fast MHD shock wave produced by the collision of a flow of `superhot' (T_e >= 30-40 x 10^6 K) plasma from the flare energy source - a high-temperature reconnecting current sheet - with a magnetic loop. Possible heating regimes are analyzed. We compare our theoretical estimates of the shock velocity with the observed ascent velocities of the X-ray source. A large discrepancy (by two orders of magnitude) between these quantities is shown to arise in the adiabatic approximation. The isothermal regime of the shock wave also predicts overestimated velocities. Another regime that allows for very rapid post-shock energy losses is in much better agreement with the observations.

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