Magnetohydrostatic flux tube model in the solar atmosphere

TL;DR

This paper develops two classes of magnetohydrostatic flux tube models in the solar atmosphere, incorporating twisted magnetic fields and stratification, aligning well with observations of magnetic bright points.

Contribution

It introduces new axisymmetric flux tube models with twisted fields using the Grad-Shafranov equation and self-similar formulation, covering both closed and open magnetic structures.

Findings

Models are consistent with observed magnetic bright points.

Parameter space analysis aligns with solar atmospheric conditions.

Provides a framework for understanding magnetic flux tube structures.

Abstract

We construct two classes of the magnetohydrostatic equilibria of the axisymmetric flux tubes with twisted magnetic fields in the stratified solar atmosphere that span from the photosphere to the transition region. We built the models by incorporating specific forms of the gas pressure and poloidal current in the Grad-Shafranov equation. This model gives both closed and open field structure of the flux tube. The other open field model we construct is based on the self-similar formulation, where we have incorporated specific forms of the gas pressure, poloidal current and two different shape functions. We study the homology of the parameter space that is consistent with the solar atmosphere and find that the estimation of the magnetic structure inside the flux tubes is consistent with the observation and simulation results of the magnetic bright points.