Benchmarking Hall-Induced Magnetoacoustic to Alfvén Mode Conversion in the Solar Chromosphere

Abstract

A 2.5D numerical model of magnetoacoustic-Alfvén linear mode conversions in the partially ionised low solar atmosphere induced by the Hall effect is surveyed, varying magnetic field strength and inclination, and wave frequency and horizontal wave number. It is found that only the magnetic component of wave energy is subject to Hall-mediated conversions to Alfvén wave-energy via a process of polarisation rotation. This strongly boosts direct mode conversion between slow magnetoacoustic and Alfvén waves in the quiet low chromosphere, even at mHz frequencies. However, fast waves there, which are predominantly acoustic in nature, are only subject to Hall-induced conversion via an indirect two-step process: (i) a geometry-induced fast-slow transformation near the Alfvén-acoustic equipartition height 𝑧 eq ; and (ii) Hall-rotation of the fast wave in 𝑧 > 𝑧 eq . Thus, for the two-stage process to yield upgoing Alfvén waves, 𝑧 eq must lie below or within the Hall-effective window 0 𝑧 700 km. Magnetic field strengths over 100 G are required to achieve this. Since the potency of this Hall effect varies inversely with the field strength but directly with the wave frequency, only frequencies above about 100 mHz are significantly affected by the two-stage process. Increasing magnetic field inclination 𝜃 generally strengthens the Hall convertibility, but the horizontal wavenumber 𝑘 𝑥 has little effect. The direct and indirect Hall mechanisms both have implications for the ability of MHD waves excited at the photosphere to reach the upper chromosphere, and by implication the corona.

The non-ideal finite Larmor radius effect in the solar atmosphere

“…2009Soler at al. , 2015Cally & Khomenko 2015;Shelyag et al 2016;Khomenko 2017;Martínez-Gómez et al 2017;Martínez-Sykora et al 2017;Ballester et al 2018;Cally & Khomenko 2018;Raboonik & Cally 2019;Muthsam et al 2021;Khomenko et al 2021;Raboonik & Cally 2021). Thus the canonical picture that emerges from the recent research suggests that with increasing altitude the solar atmosphere changes from weakly ionized and weakly magnetized Ohm dominated photosphere to moderately ionized and highly magnetized ambipolar dominated chromosphere with the overlapping Ohm-Hall and Hall-ambipolar regions sandwiched in the middle (Pandey & Wardle 2012, 2013.…”