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dc.contributor.authorVandenbroucke, Bert
dc.contributor.authorWood, Kenneth
dc.date.accessioned2019-09-11T11:30:07Z
dc.date.available2019-09-11T11:30:07Z
dc.date.issued2019-09
dc.identifier.citationVandenbroucke , B & Wood , K 2019 , ' Radiation hydrodynamics simulations of the evolution of the diffuse ionized gas in disc galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 488 , no. 2 , pp. 1977-1986 . https://doi.org/10.1093/mnras/stz1841en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 261123079
dc.identifier.otherPURE UUID: 4ea0aebf-2a9c-4f3f-b1ea-0adcb878c6ae
dc.identifier.otherBibtex: urn:929fb738ce2fd663e8aef420bcacb99e
dc.identifier.otherORCID: /0000-0001-7241-1704/work/61622254
dc.identifier.otherWOS: 000482332500032
dc.identifier.otherScopus: 85074477176
dc.identifier.urihttp://hdl.handle.net/10023/18462
dc.descriptionBV and KW acknowledge support from STFC grant ST/M001296/1. The equipment was funded by BEIS capital funding via STFC capital grants ST/K000373/1 and ST/R002363/1 and STFC DiRAC Operations grant ST/R001014/1.en
dc.description.abstractThere is strong evidence that the diffuse ionized gas (DIG) in disc galaxies is photoionized by radiation from UV luminous O and B stars in the galactic disc, both from observations and detailed numerical models. However, it is still not clear what mechanism is responsible for providing the necessary pressure support for a diffuse gas layer at kpc-scale above the disc. In this work, we investigate if the pressure increase caused by photoionization can provide this support. We run self-consistent radiation hydrodynamics (RHD) models of a gaseous disc in an external potential. We find that photoionization feedback can drive low levels of turbulence in the dense galactic disc, and that it provides pressure support for an extended diffuse gas layer. Our results show that there is a natural fine-tuning between the total ionizing radiation budget of the sources in the galaxy and the amount of gas in the different ionization phases of the interstellar medium, and provide the first fully consistent RHD model of the DIG.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz1841en
dc.subjectMethods: numericalen
dc.subjectH ii regionsen
dc.subjectISM: structureen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleRadiation hydrodynamics simulations of the evolution of the diffuse ionized gas in disc galaxiesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.Centre for Biophotonicsen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz1841
dc.description.statusPeer revieweden


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