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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/4763
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dc.contributor.authorChattopadhyay, Indranil-
dc.contributor.authorSharma, Mahavir-
dc.contributor.authorNath, Biman B.-
dc.contributor.authorRyu, Dongsu-
dc.date.accessioned2012-06-26T06:59:25Z-
dc.date.available2012-06-26T06:59:25Z-
dc.date.issued2012-07-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2012, Vol. 423, p. 2153-2161en
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/4763-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe present 2-D hydrodynamic simulation of rotating galactic winds driven by radiation. We study the structure and dynamics of the cool and/or warm component($T \simeq 10^4$ K) which is mixed with dust. We have taken into account the total gravity of a galactic system that consists of a disc, a bulge and a dark matter halo. We find that the combined effect of gravity and radiation pressure from a realistic disc drives the gas away to a distance of $\sim 5$ kpc in $\sim 37$ Myr for typical galactic parameters. The outflow speed increases rapidly with the disc Eddington parameter $\Gamma_0(=\kappa I/(2 c G \Sigma)$) for $\Gamma_0 \ge 1.5$. We find that the rotation speed of the outflowing gas is $\lesssim 100$ km s$^{-1}$. The wind is confined in a cone which mostly consist of low angular momentum gas lifted from the central region.en
dc.language.isoenen
dc.publisherWiley Interscience for the RASen
dc.relation.urihttp://adsabs.harvard.edu/abs/2012MNRAS.tmp.3046Cen
dc.relation.urihttp://arxiv.org/abs/1204.1133en
dc.relation.urihttp://dx.doi.org/10.1111/j.1365-2966.2012.21027.xen
dc.rights2012 The authors & the Royal Astronomical Society.en
dc.subjectgalaxies: formationen
dc.subjectintergalactic mediumen
dc.subjectgalaxies: starbursten
dc.titleSimulation of radiation-driven winds from disc galaxiesen
dc.typeArticleen
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