Evaporation from Reconnection-driven Heat Fronts

Details Evaporation from Reconnection-driven Heat Fronts Evaporation from Reconnection-driven Heat Fronts

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640509b&link_type=abstract

American Astronomical Society, AAS Meeting #216, #405.09; Bulletin of the American Astronomical Society, Vol. 41, p.890

Astronomy and Astrophysics

Astronomy

Scientific paper

During the post-reconnection retraction of a flaring loop, material confined by the magnetic field is rapidly compressed, forming a shock wave that propagates down the loop. This shock wave, which is similar to a one-dimensional piston shock, eventually encounters the higher-density chromosphere at the footpoints of the loop. Due to the large field-aligned thermal conductivity, a heat front progresses ahead of the shock, reaching the chromosphere first and driving evaporative backflow. This research presented here investigates the effects of this backflow on the main shock, and under what conditions the shock front is significantly affected by the evaporation.
This work is supported by the NSF and DOE.

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