Version 1
: Received: 27 February 2023 / Approved: 28 February 2023 / Online: 28 February 2023 (02:23:20 CET)
How to cite:
Podgorny, A.; Podgorny, I.; Borisenko, A. MHD Simulation in the Solar Corona to Obtain Conditions for the Acceleration of Cosmic Rays during Solar Flares. Preprints2023, 2023020486. https://doi.org/10.20944/preprints202302.0486.v1.
Podgorny, A.; Podgorny, I.; Borisenko, A. MHD Simulation in the Solar Corona to Obtain Conditions for the Acceleration of Cosmic Rays during Solar Flares. Preprints 2023, 2023020486. https://doi.org/10.20944/preprints202302.0486.v1.
Cite as:
Podgorny, A.; Podgorny, I.; Borisenko, A. MHD Simulation in the Solar Corona to Obtain Conditions for the Acceleration of Cosmic Rays during Solar Flares. Preprints2023, 2023020486. https://doi.org/10.20944/preprints202302.0486.v1.
Podgorny, A.; Podgorny, I.; Borisenko, A. MHD Simulation in the Solar Corona to Obtain Conditions for the Acceleration of Cosmic Rays during Solar Flares. Preprints 2023, 2023020486. https://doi.org/10.20944/preprints202302.0486.v1.
Abstract
Solar cosmic rays (SCR) are generated during the primordial energy release in solar flares. This explosive process takes place in the solar corona above the active region. It represents fast release of the magnetic field energy of the current sheet, which is formed near a singular magnetic field line. Solar cosmic rays appear as a result of acceleration of charged particles, mainly protons, by an inductive electric field in the current sheet, equal to the field E=V´B/c near the current sheet. To study the mechanism of solar flares and obtain conditions for stydy SCR acceleration it is necessary to carry out magnetohydrodynamic (MHD) simulation of a flare situation in the solar corona above a real active region. The methods of stabilization were developed which made it possible to solve partially the problem of numerical instabilities. MHD simulations showed complicated configuration near the singular line. Comparison of the results of MHD simulations with observations showed a general agreement of the positions of the current sheets with regions of intense flare radiation. However, there are some problems with the details of such coincidences. The results show the possibility of improving the methods of MHD simulation in order to solve the arisen problems.
Keywords
solar flare; solar cosmic rays; current sheet; magnetohydrodynamic simulation; active region
Subject
PHYSICAL SCIENCES, Astronomy & Astrophysics
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
