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A 2.5D numerical model of magnetoacoustic-Alfvén linear mode conversions in the partially ionized low solar atmosphere induced by the Hall effect is surveyed, varying magnetic field strength and inclination, and wave frequency and horizontal wavenumber. 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 polarization 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 zeq; and (ii) Hall-rotation of the fast wave in z &amp;gt; zeq. Thus, for the two-stage process to yield upgoing Alfvén waves, zeq 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 kx 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.

Benchmarking hall-induced magnetoacoustic to Alfvén mode conversion in the solar chromosphere