Podladchikova, O ; Kraaikamp, E ; Verbeeck, C

Talk presented at Solar Wind 15, Brussels, Belgium on 2018-06-19

Abstract: Coronal physics is dominated by two major problems: solar wind acceleration and coronal heating. Parker proposed that low solar corona could be heated by the dissipation at many small-scale tangential discontinuities arising spontaneously in the coronal magnetic fields braided and twisted by random photospheric footpoint motions (so-called DC mechanism). AC mechanism or wave dissipation, is obvioulsy responsible for magnetic energy transfer to heat and acceleration from 2-10 solar radii[3] in the middle solar corona. Majority of the models of coronal heating based on the dissipation of small-scale current sheets assumes energy injection at large scales by photospheric motions. However due to the turbulent nature of these motions, excitation mechanisms may occur on a wide range of scales. We present the first results of a new particle acceleration and low solar coronal heating model subject to multi-scale magnetic driving and dissipation. The model consists of two elements, the magnetic field source supposed to be associated with the small scale hydrodynamic turbulence convected from the photosphere and local dissipation of small scale currents. The dissipation is assumed to be provided by either current instabilities due to anomalous resistivity or by the magnetic reconnection which also transfer energy to accelerated particles. We study the influence of cinematic dynamo or alpha-effect, mechanism of magnetic field generation on the Sun proposed by Parker, on the properties of the heat and acceleration particle characteristics. We select the appropriated magnetic drivers and dissipation mechanisms while validating model results with SDO EUV flare database produced by Solar Demon tool.

Keyword(s): Solar Corona, Solar Orbiter
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