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dc.contributor.authorMacLachlan, J. M.
dc.contributor.authorBonnell, I. A.
dc.contributor.authorWood, K.
dc.contributor.authorDale, J. E.
dc.date.accessioned2015-04-20T10:31:23Z
dc.date.available2015-04-20T10:31:23Z
dc.date.issued2015-01
dc.identifier.citationMacLachlan , J M , Bonnell , I A , Wood , K & Dale , J E 2015 , ' Photoionising feedback and the star formation rates in galaxies ' , Astronomy & Astrophysics , vol. 573 , A112 . https://doi.org/10.1051/0004-6361/201322250en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 182355985
dc.identifier.otherPURE UUID: 2bc4cf61-199c-4feb-82d9-7b1c15a2b888
dc.identifier.otherWOS: 000350806000002
dc.identifier.otherScopus: 84921303773
dc.identifier.otherWOS: 000350806000002
dc.identifier.urihttp://hdl.handle.net/10023/6520
dc.descriptionI.A.B. acknowledges funding from the European Research Council for the FP7 ERC advanced grant project ECOGAL. This research was also supported by the DFG cluster of excellence “Origin and Structure of the Universe” (JED).en
dc.description.abstractAims. We investigate the effects of ionising photons on accretion and stellar mass growth in a young star forming region, using a Monte Carlo radiation transfer code coupled to a smoothed particle hydrodynamics (SPH) simulation. Methods. We introduce the framework with which we correct stellar cluster masses for the effects of photoionising (PI) feedback and compare to the results of a full ionisation hydrodynamics code. Results. We present results of our simulations of star formation in the spiral arm of a disk galaxy, including the effects of photoionising radiation from high mass stars. We find that PI feedback reduces the total mass accreted onto stellar clusters by ≈23% over the course of the simulation and reduces the number of high mass clusters, as well as the maximum mass attained by a stellar cluster. Mean star formation rates (SFRs) drop from SFRcontrol = 4.2 × 10-2 M⊙ yr-1 to SFRMCPI = 3.2 × 10-2 M⊙ yr-1 after the inclusion of PI feedback with a final instantaneous SFR reduction of 62%. The overall cluster mass distribution appears to be affected little by PI feedback. Conclusions. We compare our results to the observed extra-galactic Schmidt-Kennicutt relation and the observed properties of local star forming regions in the Milky Way and find that internal photoionising (PI) feedback is unlikely to reduce SFRs by more than a factor of approximate to 2 and thus may play only a minor role in regulating star formation.
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© ESO, 2015. Reproduced with permission from Astronomy & Astrophysics, © ESO.en
dc.subjectHII regionsen
dc.subjectRadiative transferen
dc.subjectStars: massiveen
dc.subjectH-II REGIONSen
dc.subjectSmoothed particle hydrodynamicsen
dc.subjectRadiation-driven implosionen
dc.subjectMolecular cloudsen
dc.subjectMassive starsen
dc.subjectIonizing-radiationen
dc.subjectCluster formationen
dc.subjectGas expulsionen
dc.subjectSchmidt lawen
dc.subjectMilky-wayen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectNDASen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titlePhotoionising feedback and the star formation rates in galaxiesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201322250
dc.description.statusPeer revieweden


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