Consequences of Magnetic Field Structure for Heat Transport in Magnetohydrodynamics

TL;DR

This paper investigates how magnetic field structure influences heat transfer across hot-cold plasma interfaces in astrophysical environments, deriving a mathematical relation for heat conduction based on magnetic topology.

Contribution

It introduces a simple mathematical model linking magnetic field topology to heat transfer rates at plasma interfaces, with potential astrophysical applications.

Findings

Derived a relation between magnetic field structure and heat conduction rate.

Showed how magnetic topology affects temperature evolution in plasma interfaces.

Discussed implications for astrophysical phenomena like wind-blown bubbles.

Abstract

Interfaces between hot and cold magnetized plasmas exist in various astrophysical contexts, for example where hot outflows impinge on an ambient interstellar medium (ISM). It is of interest to understand how the structure of the magnetic field spanning the interface affects the temporal evolution of the temperature gradient. Here we explore the relation between the magnetic field topology and the heat transfer rate by adding various fractions of tangled vs. ordered field across a hot-cold interface allow the system to evolve to a steady state. We find a simple mathematical relation for the rate of heat conduction as a function of the initial ratio of ordered to tangled field across the interface. We discuss potential implications for the astrophysical context of magnetized wind blown bubbles (WBB) around evolved stars.