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Galaxy formation hydrodynamics: From cosmic flows to star-forming clouds

Published online by Cambridge University Press:  27 April 2011

Frédéric Bournaud
Frédéric Bournaud*
Affiliation:
CEA, IRFU, SAp. CEA-Saclay, F-91191 Gif-sur-Yvette, France email: frederic.bournaud@cea.fr
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Abstract

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Major progress has been made over the last few years in understanding hydrodynamical processes on cosmological scales, in particular how galaxies get their baryons. There is increasing recognition that a large part of the baryons accrete smoothly onto galaxies, and that internal evolution processes play a major role in shaping galaxies – mergers are not necessarily the dominant process. However, predictions from the various assembly mechanisms are still in large disagreement with the observed properties of galaxies in the nearby Universe. Small-scale processes have a major impact on the global evolution of galaxies over a Hubble time and the usual sub-grid models account for them in a far too uncertain way. Understanding when, where and at which rate galaxies formed their stars becomes crucial to understand the formation of galaxy populations. I discuss recent improvements and current limitations in “resolved” modeling of star formation, aiming at explicitly capturing star-forming instabilities, in cosmological and galaxy-sized simulations. Such models need to develop three-dimensional turbulence in the ISM, which requires parsec-scale resolution at redshift zero.

Keywords

galaxies: formationgalaxies: ISMgalaxies: structuregalaxies: high-redshift
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 491 - 498
Copyright
Copyright © International Astronomical Union 2011

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