Abstract
The physics of the solar chromosphere is complex from both theoretical and modeling perspectives. The plasma temperature from the photosphere to corona increases from ∼5, 000 K to ∼1 million K over a distance of only ∼10, 000 km from the chromosphere and the transition region. Certain regions of the solar atmosphere have sufficiently low temperature and ionization rates to be considered as weakly-ionized. In particular, this is true at the lower chromosphere. In this paper, we present an overview of our data-driven magnetohydrodynamics model for the weakly-ionized chromosphere and show a benchmark result. It utilizes the Cowling resistivity which is orders of magnitude greater than the Coulomb resistivity. Ohm’s law therefore includes anisotropic dissipation. We investigate the effects of the Cowling resistivity on heating and magnetic reconnection in the chromosphere as the flare-producing active region (AR) 11166 evolves. In particular, we analyze a C2.0 flare emerging from AR11166 and find a normalized reconnection rate of 0.12.
Highlights
Chromosphere is a difficult region to model in the solar atmosphere
We presented an overview of this model and a benchmark case result which validated the local simulation setup
The partial ionization effects in our model equations are introduced by the Cowling resistivity which poses numerical challenges such as the restriction on the stability condition and the convergence speed that we needed to address
Summary
Chromosphere is a difficult region to model in the solar atmosphere. Together with the transition region, it can be considered as a transition layer from the photosphere to the corona where the plasma temperature increases from ∼5,000 K to ∼1 million K over a distance of only ∼10,000 km. In the latter category (e.g., [5, 6, 7]), there are flux emergence models that extend through the upper convection zone, photosphere, chromosphere, and transition region into the corona These are local models that include the physical processes to model the weakly-ionized plasma in the chromosphere. We present a data-driven magnetohydrodynamics (MHD) model for the weakly-ionized chromosphere It is driven by photospheric vector magnetogram data from the Helioseismic and Magnetic Imager (HMI) [8] onboard the Solar Dynamics Observatory (SDO) [9], we do not consider the upper convection zone unlike the flux emergence models.
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