The Magnetohydrodynamics of Shock-Cloud Interaction in Three Dimensions

TL;DR

This study models the magnetohydrodynamic interactions between a shock wave and a dense cloud in space, revealing how magnetic fields influence cloud stability, fragmentation, and emissions during shock encounters.

Contribution

It provides a detailed analysis of how magnetic field strength and orientation affect shock-cloud interactions in three dimensions, highlighting effects on cloud stability and emission properties.

Findings

Weak magnetic fields significantly alter cloud evolution compared to hydrodynamic cases.

Strong magnetic fields suppress cloud fragmentation and mixing.

Magnetic energy density distribution varies with field geometry, affecting emissions.

Abstract

The magnetohydrodynamic evolution of a dense spherical cloud as it interacts with a strong planar shock is studied, as a model for shock interactions with density inhomogeneities in the interstellar medium. The cloud is assumed to be small enough that radiative cooling, thermal conduction, and self-gravity can be ignored. A variety of initial orientations (including parallel, perpendicular, and oblique to the incident shock normal) and strengths for the magnetic field are investigated. During the early stages of the interaction (less than twice the time taken for the transmitted shock to cross the interior of the cloud) the structure and dynamics of the shocked cloud is fairly insensitive to the magnetic field strength and orientation. However, at late times strong fields substantially alter the dynamics of the cloud, suppressing fragmentation and mixing by stabilizing the interface at the cloud surface. Even weak magnetic fields can drastically alter the evolution of the cloud compared to the hydrodynamic case. Weak fields of different geometries result in different distributions and amplifications of the magnetic energy density, which may affect the thermal and non-thermal x-ray emission expected from shocked clouds associated with, for example, supernovae remnants.