Influence of electrons on granulation-generated solar chromosphere heating and plasma outflows

Context: It is known that the solar atmosphere exhibits a varying degree of ionization through its different layers. The ionization degree directly depends on plasma temperature, i.e., the lower the temperature, the lower the ionization degree. As a result, the plasma in the lower atmospheric layers (the photosphere and the chromosphere) is only partially ionized, which motivates the use of a three-fluid model. Aims: The paper aims to consider for the first time the influence of electrons on granulation-generated solar chromosphere heating and plasma outflows. We attempt to detect variations in the ion temperature and plasma up- and down-flows. Methods: We perform $2.5$-D numerical simulations of the generation and evolution of granulation-generated waves, flows, and other granulation-associated phenomena with the adaptation of the JOANNA code. This code solves the simplified three-fluid equations for ions (protons), electrons and neutrals (hydrogen atoms) which are coupled by collision forces. Results: Electron-neutral and electron-ion collisions provide extra heat in the low chromosphere and enhance plasma outflows in this region. However, this effect is small and can be neglected. Conclusions: Electrons do not play a major role in solar chromosphere heating and generation of plasma outflows.