Two-fluid magnetohydrodynamic effects in the high-temperature atmosphere of the sun and their new perspectives

The magnetohydrodynamic model of the solar high-temperature atmosphere is an important plasma model, which can reproduce many important features in simulating solar coronal plasma and magnetic field processes. However, the assumption of the MHD model may fail during highly dynamic and transient events, such as magnetic reconnection, and plasma heating, and in partially ionised structures such as the chromosphere, sunspots, and coronal rain. Therefore, a two-fluid MHD model with ions and neutral components can simulate many new phenomena. This study considers the two- fluid effects of solar plasma, and investigates the modification to traditional MHD models by including neutral components. We simulated MHD waves, and loop top turbulences in partially ionised plasma in sunspots or chromospheric flows. We focus on the separation of ions and neutral components in energy transfer processes and the potential contribution of neutral components to the nascent solar wind. Our simulations show that two-fluid effects would contribute significantly to solar plasma heating by collisional friction, and lead to the leakage of neutral components across the magnetic field lines and escape to the corona, it completely revolutionised our understanding of the corona, in which the role of the neutral component was neglected.