Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-48290
Powell, L C; Bournaud, F; Chapon, D; Devriendt, J; Slyz, A; Teyssier, R (2010). Galactic star formation in parsec-scale resolution simulations. Proceedings of the International Astronomical Union, 6(S270):487-490.
The interstellar medium (ISM) in galaxies is multiphase and cloudy, with stars forming in the very dense, cold gas found in Giant Molecular Clouds (GMCs). Simulating the evolution of an entire galaxy, however, is a computational problem which covers many orders of magnitude, so many simulations cannot reach densities high enough or temperatures low enough to resolve this multiphase nature. Therefore, the formation of GMCs is not captured and the resulting gas distribution is smooth, contrary to observations. We investigate how star formation (SF) proceeds in simulated galaxies when we obtain parsec-scale resolution and more successfully capture the multiphase ISM. Both major mergers and the accretion of cold gas via filaments are dominant contributors to a galaxy's total stellar budget and we examine SF at high resolution in both of these contexts.
|Item Type:||Journal Article, not refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute for Computational Science|
|Deposited On:||19 Feb 2012 20:19|
|Last Modified:||10 May 2014 03:57|
|Publisher:||Cambridge University Press|
|ISSN:||1743-9213 (P) 1743-9221 (E)|
|Additional Information:||Published online: 27 April 2011. - Copyright: Cambridge University Press. - Proceedings of IAU Symposium 270 (Computational Star Formation), May 31-June 4, 2010, Barcelona, Spain|
|Citations:||Web of Science®|
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