H I density distribution driven by supernovae: A simulation study

Hodge, Jacqueline A.; Deshpande, A.A.

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1643

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DC Field	Value	Language
dc.contributor.author	Hodge, Jacqueline A.	-
dc.contributor.author	Deshpande, A.A.	-
dc.date.accessioned	2007-01-02T11:30:32Z	-
dc.date.available	2007-01-02T11:30:32Z	-
dc.date.issued	2006-07-20	-
dc.identifier.citation	Astrophysical Journal, 2006, Vol.646, p232-239	en
dc.identifier.issn	0004-637X	-
dc.identifier.issn	1538-4357 (online)	-
dc.identifier.uri	http://hdl.handle.net/2289/1643	-
dc.description	Restricted Access till July 2009. (3 year embargo). Open access version available at arXiv.org	en
dc.description.abstract	We model the complex distribution of atomic hydrogen (H I) in the interstellar medium (ISM) assuming that it is driven entirely by supernovae (SNe). We develop and assess two different models. In the first approach, the simulated volume is randomly populated with nonoverlapping voids of a range of sizes. This may relate to a snapshot distribution of SN-remnant voids, although somewhat artificially constrained by the nonoverlap criterion. In the second approach, a simplified time evolution (considering momentum conservation as the only governing constraint during interactions) is followed as SNe populate the space with the associated input mass and energy. We describe these simulations and present our results in the form of images of the mass and velocity distributions, and the associated power spectra. The latter are compared with trends indicated by available observations. In both approaches, we find remarkable correspondence with the observed statistical description of well-studied components of the ISM, wherein the spatial spectra have been found to show significant deviations from the Kolmogorov spectrum. One of the key indications of this study, regardless of whether or not the SN-induced turbulence is the dominant process in the ISM, is that the apparent non-Kolmogorov spectral characteristics (of H I and/or electron column density across thick or thin screens) needed to explain related observations may not be in conflict at all with the underlying turbulence (i.e., the velocity structure) being of a Kolmogorov nature. We briefly discuss the limitations of our simulations and the various implications of our results.	en
dc.format.extent	264286 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	en
dc.publisher	The University of Chicago Press for the American Astronomical Society	en
dc.relation.uri	http://adsabs.harvard.edu/cgi-bin/bib_query?2006ApJ...646..232H	en
dc.relation.uri	http://arxiv.org/abs/astro-ph/0603805	en
dc.relation.uri	http://dx.doi.org/10.1086/504675	en
dc.rights	2006 American Astronomical Society	en
dc.subject	Galaxies: ISM	en
dc.subject	ISM: Kinematics and Dynamics	en
dc.subject	ISM: structure radio lines: ISM	en
dc.subject	Stars: Supernovae: General	en
dc.subject	Turbulence	en
dc.title	H I density distribution driven by supernovae: A simulation study	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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