Numerical Simulations of a Shock-Filament Interaction

Abstract

We present 3D hydrodynamic adiabatic simulations of a shock interacting with a dense, elongated cloud. We compare how the nature of the interaction changes with the filament's length and its orientation to the shock, and with the shock Mach number and the density contrast of the filament. We then examine the differences with respect to 3D spherical-cloud calculations. We find significant differences in the morphology of the interaction when M=10 and chi=100: in many cases 3 parallel rolls are formed, and spread further apart with time, and periodic vortex shedding can occur off the ends of oblique filaments. Sideways-on filaments are accelerated more quickly, and initially lose mass more quickly than spherical clouds due to their greater surface area to volume ratio. However, at late stages they lose mass more slowly, due to the reduced relative speed between the filament and the postshock flow. The acceleration and mixing timescales can vary by a factor of 2 as the filament orientation changes. Oblique filaments can achieve transverse velocities up to 10% of the shock speed. Some aspects of our simulations are compared against experimental and numerical work on rigid cylinders.

29 pages, 46 figures, accepted by MNRAS

References in corpus (18)

• The COS-Halos Survey: Physical Conditions and Baryonic Mass in the Low-Redshift Circumgalactic Medium
• Draping of Cluster Magnetic Fields over Bullets and Bubbles -- Morphology and Dynamic Effects
• Magnetized Gas Clouds can Survive Acceleration by a Hot Wind
• The Launching of Cold Clouds by Galaxy Outflows I: Hydrodynamic Interactions with Radiative Cooling
• On the nature of star-forming filaments: I. Filament morphologies
• Extended Mid-Infrared Aromatic Feature Emission in M 82
• The Bones of the Milky Way
• Rapid Molecular Cloud and Star Formation: Mechanisms and Movies
• The dynamical properties of dense filaments in the infrared dark cloud G035.39-00.33
• CARMA Large Area Star Formation Survey: Observational Analysis of Filaments in the Serpens South Molecular Cloud
• The turbulent destruction of clouds - I. A k-epsilon treatment of turbulence in 2D models of adiabatic shock-cloud interactions
• The Origin and Kinematics of Cold Gas in Galactic Winds: Insight from Numerical Simulations
• The Role of Turbulence and Magnetic Fields in Simulated Filamentary Structure
• The turbulent destruction of clouds - III. Three dimensional adiabatic shock-cloud simulations
• Can We Trust the Dust? Evidence of Dust Segregation in Molecular Clouds
• A large-scale CO survey of the Rosette Molecular Cloud: assessing the effects of O stars on surrounding molecular gas
• The formation of filamentary structures in radiative cluster winds
• IRAS 18511+0146: a proto Herbig Ae/Be cluster?

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