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dc.contributor.authorBarnes, J.E.
dc.contributor.authorWood, K.
dc.contributor.authorHill, A.S.
dc.contributor.authorMatthew Haffner, L.
dc.date.accessioned2015-03-03T11:31:02Z
dc.date.available2015-03-03T11:31:02Z
dc.date.issued2015-02-11
dc.identifier.citationBarnes , J E , Wood , K , Hill , A S & Matthew Haffner , L 2015 , ' Models of diffuse Hα in the interstellar medium : the relative contributions from in situ ionization and dust scattering ' , Monthly Notices of the Royal Astronomical Society , vol. 447 , no. 1 , pp. 559-566 . https://doi.org/10.1093/mnras/stu2454en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 172275153
dc.identifier.otherPURE UUID: a11722e7-b88d-463c-b019-fec38bb0987f
dc.identifier.otherScopus: 84922469399
dc.identifier.otherWOS: 000350272700045
dc.identifier.urihttps://hdl.handle.net/10023/6156
dc.descriptionJB acknowledges the support of an STFC studentship. LMH acknowledges support from the US National Science Foundation through award AST-1108911.en
dc.description.abstractUsing three-dimensional Monte Carlo radiation transfer models of photoionization and dust scattering, we explore different components of the widespread diffuse Hα emission observed in the interstellar medium of the Milky Way and other galaxies. We investigate the relative contributions of Hα from recombination emission in ionized gas and Hα that originates in HII regions near the Galactic mid-plane and scatters off high-altitude dust in the diffuse interstellar medium. For the radiation transfer simulations, we consider two geometries for the interstellar medium: a three-dimensional fractal geometry that reproduces the average density structure inferred for hydrogen in the Milky Way, and a density structure from a magnetohydrodynamic simulation of a supernova-driven turbulent interstellar medium. Although some sight lines that are close to HII regions can be dominated by scattered light, overall we find that less than ~20 per cent of the total Hα intensity in our simulations can be attributed to dust scattering. Our findings on the relative contribution of scattered Hα are consistent with previous observational and theoretical analyses. We also investigate the relative contributions of dust scattering and in situ ionization of high-density dust clouds in the diffuse gas. Dust scattering in these partially ionized clouds contribute ~40 per cent to the total intensity of Hα.
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectISM: generalen
dc.subjectGalaxies: ISMen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleModels of diffuse Hα in the interstellar medium : the relative contributions from in situ ionization and dust scatteringen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stu2454
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/J001651/1en


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