The interaction of a magnetohydrodynamical shock with a filament

Abstract

We present 3D magnetohydrodynamic numerical simulations of the adiabatic interaction of a shock with a dense, filamentary cloud. We investigate the effects of various filament lengths and orientations on the interaction using different orientations of the magnetic field, and vary the Mach number of the shock, the density contrast of the filament, and the plasma beta, in order to determine their effect on the evolution and lifetime of the filament. We find that in a parallel magnetic field filaments have longer lifetimes if they are orientated more 'broadside' to the shock front, and that an increase in the density contrast hastens the destruction of the cloud, in terms of the modified cloud-crushing time-scale, tcs. The combination of a mild shock and a perpendicular or oblique field provides the best condition for extending the life of the filament, with some filaments able to survive almost indefinitely since they are cocooned by the magnetic field. A high value for the density contrast does not initiate large turbulent instabilities in either the perpendicular or oblique field cases but rather draws the filament out into long tendrils which may eventually fragment. In addition, flux ropes are only formed in parallel magnetic fields. The length of the filament is, however, not as important for the evolution and destruction of a filament.

30 pages, 42 figures, accepted by MNRAS

References in corpus (10)

• Theory of Star Formation
• Magnetized Gas Clouds can Survive Acceleration by a Hot Wind
• The Launching of Cold Clouds by Galaxy Outflows I: Hydrodynamic Interactions with Radiative Cooling
• The identification of filaments on far infrared and submillimiter images. Morphology, physical conditions and relation with star formation of filamentary structure
• The importance of magnetic-field-oriented thermal conduction in the interaction of SNR shocks with interstellar clouds
• The Magnetohydrodynamics of Shock-Cloud Interaction in Three Dimensions
• The turbulent destruction of clouds - I. A k-epsilon treatment of turbulence in 2D models of adiabatic shock-cloud interactions
• Numerical simulations of shocks encountering clumpy regions
• Numerical Simulations of a Shock Interacting with Multiple Magnetized Clouds
• Discovery of a pre-existing molecular filament associated with supernova remnant G127.1+0.5

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• Magnetized High Velocity Clouds in the Galactic Halo: A New Distance Constraint
• Exploring Hydrodynamic Instabilities along the Infalling High-Velocity Cloud Complex A
• Evolving Supernova Remnants in Multiphase Interstellar Media
• Interactions of a shock with a molecular cloud at various stages of its evolution due to thermal instability and gravity
• The isothermal evolution of a shock-filament interaction
• Momentum and energy injection by a wind-blown bubble into an inhomogeneous interstellar medium
• Star-forming galaxies in the cosmic web in the last 11 Gyr