Two-fluid numerical model of chromospheric heating and plasma outflows in a quiet-Sun by K. Murawski et al. on Wednesday 23 November

\textbf{Purpose:} This paper addresses long-standing solar physics problems,

namely, the heating of the solar chromosphere and the origin of the solar wind.

Our aim is to reveal the related mechanisms behind chromospheric heating and

plasma outflows in a quiet-Sun. \textbf{Methods:} The approach is based on a

two-fluid numerical model that accounts for thermal non-equilibrium

(ionization/recombination), non-adiabatic, and non-ideal dynamics of

protons+electrons and hydrogen atoms. The model is applied to numerically

simulate the propagation and dissipation of granulation-generated waves in the

chromosphere and plasma flows inside a quiet region. \textbf{Results:} The

obtained results demonstrate that collisions between protons+electrons and

hydrogen atoms supplemented by plasma viscosity, magnetic resistivity, and

recombination lead to thermal energy release, which compensates radiative and

thermal losses in the chromosphere, and sustains the atmosphere with vertical

profiles of averaged temperature and periods of generated waves that are

consistent with recent observational data. \textbf{Conclusion:} Our model

conjectures a most robust and global physical picture of granulation-generated

wave motions, plasma flows, and subsequent heating, which form and dynamically

couple the various layers of the solar atmosphere.

arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12289v1