Ionization front-driven turbulence in the clumpy interstellar medium

Abstract

We present 3D radiation-gasdynamical simulations of an ionization front running into a dense clump. In our setup, a B0 star irradiates an overdensity which is at a distance of 10 pc and modelled as a supercritical 100 M_sol Bonnor-Ebert sphere. The radiation from the star heats up the gas and creates a shock front that expands into the interstellar medium. The shock compresses the clump material while the ionizing radiation heats it up. The outcome of this "cloud-crushing" process is a fully turbulent gas in the wake of the clump. In the end, the clump entirely dissolves. We propose that this mechanism is very efficient in creating short-living supersonic turbulence in the vicinity of massive stars.

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Cited by in corpus (7)

• The link between molecular cloud structure and turbulence
• The SILCC project --- IV. Impact of dissociating and ionising radiation on the interstellar medium and Halpha emission as a tracer of the star formation rate
• Smoothed Particle Hydrodynamics simulations of expanding HII regions. I. Numerical methods and tests
• Radiation hydrodynamics of triggered star formation: the effect of the diffuse radiation field
• Synthetic observations of star formation and the interstellar medium
• Star Formation in Molecular Clouds
• The SATIN project I: Turbulent multi-phase ISM in Milky Way simulations with SNe feedback from stellar clusters