paper

Structure and dynamics of the internetwork solar chromosphere: results of a small-scale dynamo simulation

arXiv:2508.19809 · doi:10.1051/0004-6361/202554656

Abstract

The heating and structure of the solar chromosphere depends on the underlying magnetic field, among other parameters. The lowest magnetic flux of the solar atmosphere is found in the quiet Sun internetwork and is thought to be provided by the small-scale dynamo (SSD) process. We aim to understand the chromospheric structure and dynamics in a simulation with purely SSD generated magnetic fields. We perform a 3D radiation-magnetohydrodynamic (rMHD) simulation of the solar atmosphere, including the necessary physics to simulate the solar chromosphere. No magnetic field is imposed beyond that generated by an SSD process. We analyse the magnetic field in the chromosphere, and the resulting energy balance. Plasma at chromospheric temperatures reaches high into the atmosphere, with small, transient regions reaching coronal temperatures. An average Poynting flux of \;s is found at the base of the chromosphere. The magnetic field in the chromosphere falls off more slowly with height than predicted by a potential field extrapolation from the radial component of the photospheric field. Starting in the middle chromosphere, the magnetic energy density is an order of magnitude larger than the kinetic energy density and, in the upper chromosphere, also larger than the thermal energy density. Nonetheless, even in the high chromosphere, the plasma beta in shock fronts and low-field regions can locally reach values above unity. The interactions between shocks and the magnetic field are essential to understanding the dynamics of the internetwork chromosphere. The SSD generated magnetic fields are strong enough to dominate the energy balance in the mid-to-upper chromosphere. The energy flux into the chromosphere is , larger than the canonical values required to heat the quiet sun chromosphere and corona.

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