MHS sunspot model from deep sub-photospheric to chromospheric layers

TL;DR

This paper presents a method to construct magnetohydrostatic equilibrium models of the sun's atmosphere, spanning from deep sub-photospheric to chromospheric layers, for use in helioseismology wave simulations.

Contribution

It introduces a novel approach combining self-similar solutions and current-distributed models to create comprehensive equilibrium models for solar wave propagation studies.

Findings

Developed a set of magnetohydrostatic models through numerical integration.

Models cover a wide range of parameters from sub-photospheric to chromospheric layers.

Facilitates more accurate forward modeling of helioseismic wave propagation.

Abstract

In order to understand the influence of magnetic fields on the propagation properties of waves, as derived from different local helioseismology techniques, forward modeling of waves is required. Such calculations need a model in magnetohydrostatic equilibrium as initial atmosphere to propagate oscillations through it. We provide a method to construct such a model in equilibrium for a wide range of parameters to be used for simulations of artificial helioseismologic data. The method combine the advantages of self-similar solutions and current-distributed models. A set of models is developed by numerical integration of magnetohydrostatic equations from the sub-photospheric to chromospheric layers.