Consequences of Magnetic Field Structure for Heat Transport in Magnetohydrodynamics

Details Consequences of Magnetic Field Structure for Heat Transport in Magnetohydrodynamics Consequences of Magnetic Field Structure for Heat Transport in Magnetohydrodynamics

2011-10-04

arxiv.org/abs/1110.0817v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

41 pages, 13 figures

Scientific paper

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.

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