Parker, RJ and Dale, JE (2015) On the spatial distributions of stars and gas in numerical simulations of molecular clouds. Monthly Notices of the Royal Astronomical Society, 451 (4). pp. 3664-3670. ISSN 1365-2966

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Abstract

We compare the spatial distribution of stars which form in hydrodynamical simulations to the spatial distribution of the gas, using the $\mathcal{Q}$-parameter. The $\mathcal{Q}$-parameter enables a self-consistent comparison between the stars and gas because it uses a pixelated image of the gas as a distribution of points, in the same way that the stars (sink particles in the simulations) are a distribution of points. We find that, whereas the stars have a substructured, or hierarchical spatial distribution ($\mathcal{Q} \sim 0.4 - 0.7$), the gas is dominated by a smooth, concentrated component and typically has $\mathcal{Q} \sim 0.9$. We also find no statistical difference between the structure of the gas in simulations that form with feedback, and those that form without, despite these two processes producing visually different distributions. These results suggest that the link between the spatial distributions of gas, and the stars which form from them, is non-trivial.

Item Type:	Article
Additional Information:	This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly notices of the Royal Astronomical Society following peer review. The version of record MNRAS (August 21, 2015) 451 (4): 3664-3670 is available online at http://dx.doi.org/10.1093/mnras/stv1223
Uncontrolled Keywords:	astro-ph.GA; astro-ph.GA
Subjects:	Q Science > QB Astronomy
Divisions:	Astrophysics Research Institute
Publisher:	Oxford University Press
Related URLs:	http://arxiv.org/abs/1506.00646v1
Date Deposited:	12 Jun 2015 12:39
Last Modified:	04 Sep 2021 14:18
URI:	https://researchonline.ljmu.ac.uk/id/eprint/1391

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