Fast magnetic wave could heat the solar low-beta chromosphere
arXiv:2107.13722 · doi:10.3847/2041-8213/ac10c7
Abstract
Magnetohydrodynamic (MHD) waves are candidates for heating the solar chromosphere, although it is still unclear which mode of the wave is dominant in heating. We perform two-dimensional radiative MHD simulation to investigate the propagation of MHD waves in the quiet region of the solar chromosphere. We identify the mode of the shock waves by using the relationship between gas pressure and magnetic pressure across the shock front and calculate their corresponding heating rate through the entropy jump to obtain a quantitative understanding of the wave heating process in the chromosphere. Our result shows that the fast magnetic wave is significant in heating the low-beta chromosphere. The low-beta fast magnetic waves are generated from high-beta fast acoustic waves via mode conversion crossing the equipartition layer. Efficient mode conversion is achieved by large attacking angles between the propagation direction of the shock waves and the chromospheric magnetic field.
Accepted by ApJL
References in corpus (8)
- Multiwavelength studies of MHD waves in the solar chromosphere: An overview of recent results
- On the generation of solar spicules and Alfvénic waves
- Non-equilibrium hydrogen ionization in 2D simulations of the solar atmosphere
- Dynamics of the Solar Magnetic Network. II. Heating the Magnetized Chromosphere
- Three-dimensional Magnetohydrodynamic Simulation of the Formation of Solar Chromospheric Jets with Twisted Magnetic Field Lines
- Ion-neutral interactions and non-equilibrium ionization in the solar chromosphere
- Heating of the magnetic chromosphere: observational constraints from Ca II 8542 spectra
- Chromospheric polarimetry through multi-line observations of the 850 nm spectral region III: Chromospheric jets driven by twisted magnetic fields