Interstellar Turbulence and Star Formation

Abstract

We provide a brief overview of recent advances and outstanding issues in simulations of interstellar turbulence, including isothermal models for interior structure of molecular clouds and larger-scale multiphase models designed to simulate the formation of molecular clouds. We show how self-organization in highly compressible magnetized turbulence in the multiphase ISM can be exploited in simple numerical models to generate realistic initial conditions for star formation.

8 pages, 5 color figures; submitted to Proceedings of IAU Symposium 270 "Computational Star Formation" held in Barcelona, May 31 - June 4, 2010

References in corpus (38)

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• Simulating Star Formation and Feedback in Galactic Disk Models
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• The Power Spectrum of Supersonic Turbulence in Perseus
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• Dissipative Structures in Supersonic Turbulence
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• Density Power Spectrum in Turbulent Thermally Bi-stable Flows
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Cited by in corpus (6)

• Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations
• On the Density Distribution in Star-forming Interstellar Clouds
• Comparing Numerical Methods for Isothermal Magnetized Supersonic Turbulence
• The structure and statistics of interstellar turbulence
• The effect of diffuse background on the spatially-resolved Schmidt relation in nearby spiral galaxies
• Statistical signatures of interstellar turbulence in dust polarization maps