Particle Acceleration and Plasma Heating in the Chromosphere

• DOI: 10.1007/s11207-015-0731-y
• Publication Date: 2015-07-15T12:05:25Z
• Authors: V. V. Zaitsev; A. V. Stepanov
• Keywords: Chromosphere; Solar flare; Nanoflares; Photosphere; Corona (planetary geology); Coronal radiative losses; Coronal loop; Electric current

We propose a new mechanism of electron acceleration and plasma heating in the solar chromosphere, based on the magnetic Rayleigh–Taylor instability. The instability develops at the chromospheric footpoints of a flare loop and deforms the local magnetic field. As a result, the electric current in the loop varies, and a resulting inductive electric field appears. A pulse of the induced electric field, together with the pulse of the electric current, propagates along the loop with the Alfven velocity and begins to accelerate electrons up to an energy of about 1 MeV. Accelerated particles are thermalized in the dense layers of the chromosphere with the plasma density $n \approx10^{14}\,\mbox{--}\,10^{15}~\mbox{cm}^{-3}$ , heating them to a temperature of about several million degrees. Joule dissipation of the electric current pulse heats the chromosphere at heights that correspond to densities $n \le10^{11}\,\mbox{--}\,10^{13}~\mbox{cm}^{-3}$ . Observations with the New Solar Telescope at Big Bear Solar Observatory indicate that chromospheric footpoints of coronal loops might be heated to coronal temperatures and that hot plasma might be injected upwards, which brightens ultra-fine loops from the photosphere to the base of the corona. Thereby, recent observations of the Sun and the model we propose stimulate a deja vu – they are reminiscent of the concept of the chromospheric flare.