Other
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e...4p&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Other
Scientific paper
Fast electrons moving along a magnetic field line in the solar atmosphere undergo collisions with the particles of the background plasma. In doing so, they deposit some of their energy into the background plasma, increasing its temperature. In addition to this temperature increase, the plasma also undergoes radiative and conductive cooling, which alters the temperature distribution along the field line. Using stochastic simulations, we can model the movement of fast electrons along a field line and calculate changes in their energy as they undergo collisions. We use this data to map the temperature distribution along the field line, including radiative and conductive cooling, for injected electron beams of various initial distributions and injection parameters. Temperature maps, and the radiation maps that arise from them, can be compared with observations from RHESSI and other satellites.
Fletcher Lauren
Pollock Jennifer A.
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