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X-ray Source Heights in a Solar Flare: Thick-target versus Thermal Conduction Front Heating View all abstracts by submitter

Jeffrey Reep   Submitted: 2016-01-04 07:31

Observations of solar flares with RHESSI have shown X-ray sources traveling along flaring loops, from the corona down to the chromosphere and back up. The 28 November 2002 C1.1 flare, first observed with RHESSI by Sui et al. 2006 and quantitatively analyzed by O'Flannagain et al. 2013, very clearly shows this behavior. By employing numerical experiments, we use these observations of X-ray source height motions as a constraint to distinguish between heating due to a non-thermal electron beam and in situ energy deposition in the corona. We find that both heating scenarios can reproduce the observed light curves, but our results favor non-thermal heating. In situ heating is inconsistent with the observed X-ray source morphology and always gives a height dispersion with photon energy opposite to what is observed.

Authors: Reep, J.W., Bradshaw, S.J., Holman, G.D.
Projects: RHESSI

Publication Status: Accepted to ApJ
Last Modified: 2016-01-06 10:49
Go to main E-Print page  Injection of solar energetic particles into both loop legs of a magnetic cloud   The Hinode /XRT Full-Sun Image Corrections and the Improved Synoptic Composite Image Archive  Edit Entry  Download Preprint  Delete Entry 

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