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dc.contributor.authorVandenbroucke, Bert
dc.contributor.authorSartorio, Nina S
dc.contributor.authorWood, Kenneth
dc.contributor.authorLund, Kristin
dc.contributor.authorFalceta-gonçalves, Diego
dc.contributor.authorHaworth, Thomas J
dc.contributor.authorBonnell, Ian
dc.contributor.authorKeto, Eric
dc.contributor.authorTootill, Daniel
dc.date.accessioned2019-12-09T12:30:09Z
dc.date.available2019-12-09T12:30:09Z
dc.date.issued2019-05-21
dc.identifier.citationVandenbroucke , B , Sartorio , N S , Wood , K , Lund , K , Falceta-gonçalves , D , Haworth , T J , Bonnell , I , Keto , E & Tootill , D 2019 , ' Testing the stability of supersonic ionized Bondi accretion flows with radiation hydrodynamics ' , Monthly Notices of the Royal Astronomical Society , vol. 485 , no. 3 , pp. 3771-3782 . https://doi.org/10.1093/mnras/stz357en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 264191642
dc.identifier.otherPURE UUID: b80ccd07-4239-4548-8a29-baa1e82d568c
dc.identifier.othercrossref: 10.1093/mnras/stz357
dc.identifier.otherScopus: 85074517736
dc.identifier.otherORCID: /0000-0001-7241-1704/work/66070368
dc.identifier.otherWOS: 000474902000060
dc.identifier.urihttp://hdl.handle.net/10023/19100
dc.descriptionBV and KW acknowledge support from STFC grant ST/M001296/1. NSS would like to thank CAPES for graduate research funding. KL acknowledges support from the Carnegie Trust. DFG thanks the Brazilian agencies FAPESP (no. 2013/10559-3) and CNPq (no. 311128/2017-3) for financial support. TJH is funded by an Imperial College London Junior Research Fellowship.en
dc.description.abstractWe investigate the general stability of 1D spherically symmetric ionized Bondi accretion on to a massive object in the specific context of accretion on to a young stellar object. We first derive a new analytic expression for a steady-state two-temperature solution that predicts the existence of compact and hypercompact H ii regions. We then show that this solution is only marginally stable if ionization is treated self-consistently. This leads to a recurring collapse of the H ii region over time. We derive a semi-analytic model to explain this instability, and test it using spatially converged 1D radiation hydrodynamical simulations. We discuss the implications of the 1D instability on 3D radiation hydrodynamics simulations of supersonic accreting flows.
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 author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stz357en
dc.subjectHydrodynamicsen
dc.subjectInstabilitiesen
dc.subjectMethods: numericalen
dc.subjectHII regionsen
dc.subjectQB Astronomyen
dc.subjectDASen
dc.subject.lccQBen
dc.titleTesting the stability of supersonic ionized Bondi accretion flows with radiation hydrodynamicsen
dc.typeJournal articleen
dc.description.versionPostprinten
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/stz357
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1903.00479en


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