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Simulating the chemistry and dynamics of molecular clouds

Published online by Cambridge University Press:  21 October 2010

S. C. O. Glover ,
C. Federrath ,
M.-M. Mac Low  and
R. S. Klessen
S. C. O. Glover
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Strasse 2, 69120 Heidelberg, Germany email: [email protected]
C. Federrath
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Strasse 2, 69120 Heidelberg, Germany email: [email protected]
M.-M. Mac Low
Affiliation:
Department of Astronomy, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, USA
R. S. Klessen
Affiliation:
Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle-Strasse 2, 69120 Heidelberg, Germany email: [email protected]
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Abstract

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We have performed high-resolution three-dimensional simulations of turbulent interstellar gas that for the first time self-consistently follow its coupled thermal, chemical and dynamical evolution. Our simulations have allowed us to quantify the formation timescales for the most important molecules found in giant molecular clouds (H2, CO), as well as their spatial distribution within the clouds. Our results are consistent with models in which molecular clouds form quickly, within 1–2 turbulent crossing times, and emphasize the crucial role of density inhomogeneities in determining the chemical structure of the clouds.

Keywords

astrochemistry – molecular processes – methods: numerical – ISM: clouds – ISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 405
Copyright
Copyright © International Astronomical Union 2010

References

Glover, S. C. O., Federrath, C., Mac Low, M.-M., & Klessen, R. S. 2009, MNRAS, in press; arXiv:0907.4081Google Scholar