A Fixed-point Scheme for the Numerical Construction of Magnetohydrostatic Atmospheres in Three Dimensions
arXiv:1609.00733 · doi:10.1007/s11207-016-0992-0
Abstract
Magnetohydrostatic models of the solar atmosphere are often based on idealized analytic solutions because the underlying equations are too difficult to solve in full generality. Numerical approaches, too, are often limited in scope and have tended to focus on the two-dimensional problem. In this article we develop a numerical method for solving the nonlinear magnetohydrostatic equations in three dimensions. Our method is a fixed-point iteration scheme that extends the method of Grad and Rubin (Proc. 2nd Int. Conf. on Peaceful Uses of Atomic Energy 31, 190, 1958) to include a finite gravity force. We apply the method to a test case to demonstrate the method in general and our implementation in code in particular.
Accepted for publication in Solar Physics
References in corpus (6)
- Non-linear numerical simulations of magneto-acoustic wave propagation in small-scale flux tubes
- A self-consistent nonlinear force-free solution for a solar active region magnetic field
- Magnetic modelling and tomography: First steps towards a consistent reconstruction of the solar corona
- Optimization approach for the computation of magnetohydrostatic coronal equilibria in spherical geometry
- First nonlinear force-free field extrapolations of SOLIS/VSM data
- Numerical Models of Travel-Time Inhomogeneities in Sunspots