SMuK 2021 – scientific programme
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EP: Fachverband Extraterrestrische Physik
EP 2: Sun and Heliosphere II
EP 2.6: Talk
Monday, August 30, 2021, 18:00–18:15, H7
Non-thermal electron velocity distribution functions generated by kinetic magnetic reconnection in the solar atmosphere — •Xin Yao1,2, Patricio Muñoz2, and Jörg Büchner2,1 — 1Max Planck Institute for Solar System Research, 37077 Göttingen, Germany — 2Centre for Astronomy and Astrophysics, Technical University of Berlin, 10623 Berlin, Germany
Magnetic reconnection in solar flares can generate non-thermal electron beams. Those accelerated electrons can, in turn, emit radio waves via kinetic instabilities. We aim at investigating the properties of those electrons beams that are relevant for those instabilities (sources of free energy) and their resulting radio emission. For this sake we utilize fully kinetic Particle-In-Cell simulations. Our results show that: (1) Parallel sources of free energy due to magnetized electrons are mainly generated in the diffusion region below/above the X point and separatrices, which can cause bump-on-tail instabilities and generate harmonics of electrostatic Langmuir waves. (2) Perpendicular sources of free energy due to unmagnetized electrons are formed in the diffusion and outflow region near the midplane of the reconnection, which can cause electron cyclotron maser instabilities and generate electrostatic Bernstein waves. In particular, a crescent-shaped EVDF in the velocity space perpendicular to local magnetic field is found. (3) The strength of external field has a negative influence on the formation of perpendicular sources of free energy. Our results allows us to remote diagnose some local plasma properties at the source regions of coronal magnetic reconnection via its radio emission.