Shock-triggered formation of magnetically-dominated clouds. II. Weak shock-cloud interaction in three dimensions

Abstract

To understand the formation of a magnetically dominated molecular cloud from an atomic cloud, we study the interaction of a weak, radiative shock with a magnetised cloud. The thermally stable warm atomic cloud is initially in static equilibrium with the surrounding hot ionised gas. A shock propagating through the hot medium then interacts with the cloud. We follow the dynamical evolution of the shocked cloud with a time-dependent ideal magnetohydrodynamic code. By performing the simulations in 3D, we investigate the effect of different magnetic field orientations including parallel, perpendicular and oblique to the shock normal. We find that the angle between the shock normal and the magnetic field must be small to produce clouds with properties similar to observed molecular clouds.

10 pages, 12 figures, accepted for publication in MNRAS

References in corpus (8)

• From the warm magnetized atomic medium to molecular clouds
• The Magnetohydrodynamics of Shock-Cloud Interaction in Three Dimensions
• Two-Fluid MHD Simulations of Converging Hi Flows in the Interstellar Medium. II: Are Molecular Clouds Generated Directly from Warm Neutral Medium?
• The star-forming content of the W3 giant molecular cloud
• Shock-triggered formation of magnetically-dominated clouds
• Local Star formation triggered by SN shocks in magnetized diffuse neutral clouds
• The effect of ambipolar resistivity on the formation of dense cores
• Generation of density inhomogeneities by magnetohydrodynamic waves in two dimensions

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• Formation of HI Clouds in Shock-compressed Interstellar Medium: Physical Origin of Angular Correlation Between Filamentary Structure and Magnetic Field
• The turbulent destruction of clouds - III. Three dimensional adiabatic shock-cloud simulations
• GMC Collisions as Triggers of Star Formation. I. Parameter Space Exploration with 2D Simulations
• Kiloparsec-Scale Simulations of Star Formation in Disk Galaxies. I. The unmagnetized and zero-feedback limit
• MHD simulation of the formation of clumps and filaments in quiescent diffuse medium by thermal instability
• The Early Stage of Molecular Cloud Formation by Compression of Two-phase Atomic Gases
• MHD Shock-Clump Evolution with Self-Contained Magnetic Fields
• Thermal instability revisited
• The interaction of a magnetohydrodynamical shock with a filament
• Bimodal Behavior and Convergence Requirement in Macroscopic Properties of the Multiphase Interstellar Medium Formed by Atomic Converging Flows
• Magnetic Fields and Galactic Star Formation Rates
• 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