Interaction of a collisionless conduction front with the chromosphere and solar hard X-ray bursts
The interaction of a collisionless conduction front with the transition region and chromosphere is investigated in a one-dimensional fluid approach as an explanation of elementary flare bursts in hard X-rays. It is shown that, for finite energy injection times, material boiled off of the chromosphere rises into the corona and eventually quenches the X-ray emission. This provides an acceptable explanation of elementary flare bursts with many testable predictions. Softer (10--20 keV) X-rays should come primarily from near the chromosphere, while harder (90--100 keV) X-rays should come primarily from higher in the corona. Ion heating to 10/sup 8/ K and upward mass motions to 1000 km s/sup -1/ should be observed. Limitations of the analysis resulting from its fluid character and implications for testable predictions are discussed. It is emphasized that, although the efficiency of this thermal model is only slightly larger than a nonthermal model for an initial density of 2.6 x 10/sup 10/ cm/sup -3/, it is much easier from the point of view of plasma physics to heat a plasma than to accelerate a significant fraction of its electrons.
- Research Organization:
- Department of Astro-Geophysics, University of Colorado
- OSTI ID:
- 5577321
- Journal Information:
- Astrophys. J.; (United States), Vol. 252:2
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
GENERAL PHYSICS
CHROMOSPHERE
STAR MODELS
SOLAR X-RAY BURSTS
HYDRODYNAMICS
IONIZATION
MATHEMATICAL MODELS
PLASMA
SAHA EQUATION
SOLAR ATMOSPHERE
SOLAR CORONA
SOLAR FLARES
ATMOSPHERES
EQUATIONS
FLUID MECHANICS
MECHANICS
SOLAR ACTIVITY
640104* - Astrophysics & Cosmology- Solar Phenomena