Volume 620, December 2018
|Number of page(s)||4|
|Section||Letters to the Editor|
|Published online||30 November 2018|
Letter to the Editor
Non-thermal electrons from solar nanoflares
In a 3D radiative MHD simulation
1 Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway
2 Rosseland Centre for Solar physics (RoCS), University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway
Accepted: 14 November 2018
Context. We introduce a model for including accelerated particles in pure magnetohydrodynamics (MHD) simulations of the solar atmosphere.
Aims. We show that the method is viable and produces results that enhance the realism of MHD simulations of the solar atmosphere.
Methods. The acceleration of high-energy electrons in solar flares is an accepted fact, but is not included in the most advanced 3D simulations of the solar atmosphere. The effect of the acceleration is not known, and here we introduce a simple method to account for the ability of the accelerated electrons to move energy from the reconnection sites and into the dense transition zone and chromosphere.
Results. The method was only run for a short time and with low reconnection energies, but this showed that the reconnection process itself changes, and that there is a clear effect on the observables at the impact sites of the accelerated electrons. Further work will investigate the effect on the reconnection sites and the impact sites in detail.
Key words: Sun: corona / Sun: general / acceleration of particles / magnetohydrodynamics (MHD) / magnetic reconnection
© ESO 2018
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.