5:15 PM - 7:15 PM
[PEM11-P10] A robust MHD relaxation method for reconstructing the solar atmospheric magnetic field
Keywords:MHD relaxation method, magnetohydrostatic equilibrium, coronal magnetic field, chromospheric magnetic field
Explosive phenomena in the solar atmosphere such as solar flares are processes in which free magnetic energy in the solar atmosphere is suddenly released. Therefore, understanding and predicting these phenomena require information on the three-dimensional distribution of the solar atmospheric magnetic field. Various methods have been developed to reconstruct the solar atmospheric magnetic field from directly measured vector magnetic fields on the photosphere. In particular, we proposed an MHD relaxation method for reconstructing magnetohydrostatic fields that include the effects of pressure and gravity [Miyoshi, et al., 2020]. However, numerical schemes for the MHD relaxation method have not been thoroughly investigated.
In this study, we develop a new scheme for the MHD relaxation method for robustly reconstructing the solar atmospheric magnetic field without the need for empirical parameter tuning. The proposed algorithm decouples the temporal evolution of the magnetic field and pressure and solves them alternately. The evolution of the magnetic field is computed using the HLLD Riemann solver in conjunction with the constrained transport (CT). Meanwhile, the evolution of the pressure is solved using the Lax-Friedrichs solver with a well-balanced treatment applied to the gravitational term. We validate and confirm the accuracy and robustness of the proposed method using benchmark models. Furthermore, we attempt to reconstruct the solar atmospheric magnetic field using observational data.
In this study, we develop a new scheme for the MHD relaxation method for robustly reconstructing the solar atmospheric magnetic field without the need for empirical parameter tuning. The proposed algorithm decouples the temporal evolution of the magnetic field and pressure and solves them alternately. The evolution of the magnetic field is computed using the HLLD Riemann solver in conjunction with the constrained transport (CT). Meanwhile, the evolution of the pressure is solved using the Lax-Friedrichs solver with a well-balanced treatment applied to the gravitational term. We validate and confirm the accuracy and robustness of the proposed method using benchmark models. Furthermore, we attempt to reconstruct the solar atmospheric magnetic field using observational data.