Emergence of magnetic flux in a partially ionized solar atmosphere
Abstract
We perform 3-D MHD simulations for a magnetic flux emergence experiment to investigate whether the inclusion of ionization-recombination in the equation of state affects the magnetic flux ascend to the solar atmosphere. We modify the single-fluid MHD equations to include the presence of neutrals on our environment configuration. We used the Lare3D code to numerically solve this 3D time-dependent compressible, resistive MHD equations in cartesian coordinates. Two different models have been considered, the FIP which assumes a fully ionized plasma and the PIP which assumes partially ionized plasma. We performed two different runs with the same beta plasma to be able to observe the differences in the behaviour of the ascend of each flux tube. The axis of the PIP flux tube reaches lower altitudes in the convection zone compared to the axis of the FIP due to the inclusion of the ionization-recombination to the equation of state. The presence of neutrals in the high convection zone affects the structure of the rising magnetic field on the small scale. This different ascended magnetic field on the photosphere has an impact on the evolution of the bipolar region leading to polarities with more spherical and compact shapes than the FIP model and shorter polarity inversion line. Overall our magnetic flux emergence experiment revealed further the role of partial ionization to the magnetic flux emergence into the dynamic solar atmosphere.
- Publication:
-
44th COSPAR Scientific Assembly. Held 16-24 July
- Pub Date:
- July 2022
- Bibcode:
- 2022cosp...44.2552C