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Radiative Turbulent Flares in Magnetically-dominated Plasmas by Nättilä, J.; Beloborodov, A. M. is a scholarly article available to read on EtoBox.

What is Radiative Turbulent Flares in Magnetically-dominated Plasmas about?

We perform 2D and 3D kinetic simulations of reconnection-mediated turbulent flares in a magnetized electron-positron plasma, with weak and strong radiative cooling. Such flares can be generated around neutron stars and accreting black holes. We focus on the magnetically-dominated regime where tension of the background magnetic field lines exceeds the plasma rest mass by a factor $\sigma_0 > 1$. In the simulations, turbulence is excited on a macroscopic scale $l_0$, and we observe that it develops by forming thin, dynamic current sheets on various scales. The deposited macroscopic energy dissipates by energizing thermal and nonthermal particles. The particle energy distribution is shaped by impulsive acceleration in reconnecting current sheets, gradual stochastic acceleration, and radiative losses. We parameterize radiative cooling by the ratio $A$ of light-crossing time $l_0/c$ to a cooling timescale, and study the effect of increasing $A$ on the flare. When radiative losses are sufficiently weak, $A<\sigma_0^{-1}$, the produced emission is dominated by stochastically accelerated particles, and the radiative power depends logarithmically on $A$. The resulting flare radiation spectr

Author

Nättilä, J.; Beloborodov, A. M.

Published

2020

Language

EN