Turbulent molecular clouds

Abstract

Stars form within molecular clouds but our understanding of this fundamental process remains hampered by the complexity of the physics that drives their evolution. We review our observational and theoretical knowledge of molecular clouds trying to confront the two approaches wherever possible. After a broad presentation of the cold interstellar medium and molecular clouds, we emphasize the dynamical processes with special focus to turbulence and its impact on cloud evolution. We then review our knowledge of the velocity, density and magnetic fields. We end by openings towards new chemistry models and the links between molecular cloud structure and star--formation rates.

To be published in AARv, 58 pages, 13 figures (higher resolution figures will be available on line)

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• On the universality of interstellar filaments: theory meets simulations and observations
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• On the effective turbulence driving mode of molecular clouds formed in disc galaxies
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• Thermal and turbulent properties of the Warm Neutral Medium in the solar neighborhood
• Turbulent Magnetic Field Amplification by the Interaction of Shock Wave and Inhomogeneous Medium
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• The core and stellar mass functions in massive collapsing filaments
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• Principal Component Analysis of Molecular Clouds: Can CO reveal the dynamics?
• WISDOM Project XII. Clump properties and turbulence regulated by clump-clump collisions in the dwarf galaxy NGC404
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• Density distribution function of a self-gravitating isothermal compressible turbulent fluid in the context of Molecular Clouds ensembles II: the contribution of the turbulent term and the potential of the outer shells
• Cloud properties across spatial scales in simulations of the interstellar medium
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• 25 years of XMM-Newton observations of the Sgr A complex: 3D distribution and internal structure of the clouds
• Multiline observations of hydrogen, helium, and carbon radio-recombination lines toward Orion A: A detailed dynamical study and direct determination of physical conditions
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• Characteristic scale of star formation. I. Clump formation efficiency on local scales
• Mapping and characterizing magnetic fields in the Rho Ophiuchus-A molecular cloud with SOFIA/HAWC$+$
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• On the Flux-Intensity Relation of Molecular Clouds
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• The role of environment on the evolution of disc galaxies density profiles New insights from simulations and comparison to Euclid data
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• The Drag Instability in a 2D Isothermal C-shock
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• Do tides play a role in the determination of the pre-stellar core mass function?
• The signature of large scale turbulence driving on the structure of the interstellar medium
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• Why most molecular clouds are gravitationally dominated
• Density profile of a self-gravitating polytropic turbulent fluid in the context of ensembles of molecular clouds
• Multi-tracer analysis of straight depolarisation canals in the surroundings of the 3C 196 field
• Monte Carlo simulation of molecular dynamics for amino acid production from carboxylic acid via C-14 beta-decay
• Revealing the drag instability in one-fluid nonideal MHD simulations of a 1D isothermal C-shock
• Influence of protostellar jets and HII regions on the formation and evolution of stellar clusters