Monochromatic Two-Fluid Alfvén Waves in the Partially Ionised Solar Chromosphere

Abstract We present new results towards the explanation of chromospheric-heating problem and solar-wind origin, using a two-fluid model that takes into account collisional interaction between ions (protons) neutrals (hydrogen atoms). Our aim is to further reveal mechanism behind chromospheric heating plasma outflows. simulate analyse propagation evolution Alfvén waves in partially ionised solar chromosphere, consisting + electrons neutral fluids. The simplified chromosphere permeated by vertical, uniform magnetic field. perform numerical simulations framework quasi-1.5-dimensional (1.5D), which are excited harmonic driver transverse component ion velocities, operating chromosphere. In case small-amplitude driver, weakly damped, for chosen wave periods few seconds, manage propagate through enter corona. Non-linear large-amplitude cause significant thus conclude with larger amplitudes can contribute outflows, may result higher up origin.