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Optimal Electron Energies for Driving Chromospheric Evaporation in Solar Flares View all abstracts by submitter

Jeffrey Reep   Submitted: 2015-07-06 07:38

In the standard model of solar flares, energy deposition by a beam of electrons drives strong chromospheric evaporation leading to a significantly denser corona and much brighter emission across the spectrum. Chromospheric evaporation was examined in great detail by Fisher, Canfield, & McClymont (1985a,b,c), who described a distinction between two different regimes, termed explosive and gentle evaporation. In this work, we examine the importance of electron energy and stopping depths on the two regimes and on the atmospheric response. We find that with explosive evaporation, the atmospheric response does not depend strongly on electron energy. In the case of gentle evaporation, lower energy electrons are significantly more efficient at heating the atmosphere and driving up-flows sooner than higher energy electrons. We also find that the threshold between explosive and gentle evaporation is not fixed at a given beam energy flux, but also depends strongly on the electron energy and duration of heating. Further, at low electron energies, a much weaker beam flux is required to drive explosive evaporation.

Authors: Reep, J.W., Bradshaw, S.J., & Alexander, D.
Projects: None

Publication Status: Accepted to ApJ
Last Modified: 2015-07-06 13:04
Go to main E-Print page  Formation of Magnetic Flux Ropes during Confined Flaring Well Before the Onset of a Pair of Major Coronal Mass Ejections  Confined Flares in Solar Active Region 12192 from 2014 October 18 to 29  Edit Entry  Download Preprint  Delete Entry 

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