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dc.contributor.authorWurster, J.
dc.contributor.authorBate, Matthew R.
dc.contributor.authorPrice, Daniel J.
dc.date.accessioned2019-10-22T15:30:03Z
dc.date.available2019-10-22T15:30:03Z
dc.date.issued2018-04
dc.identifier.citationWurster , J , Bate , M R & Price , D J 2018 , ' The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics ' , Monthly Notices of the Royal Astronomical Society , vol. 475 , no. 2 , pp. 1859-1880 . https://doi.org/10.1093/mnras/stx3339en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 262150330
dc.identifier.otherPURE UUID: 7b93fde2-c400-4dab-bc40-3551e8bd475c
dc.identifier.otherBibtex: WursterBatePrice2018sd
dc.identifier.otherScopus: 85045957136
dc.identifier.otherORCID: /0000-0003-0688-5332/work/63716932
dc.identifier.urihttps://hdl.handle.net/10023/18746
dc.description.abstractWe present results from radiation non-ideal magnetohydrodynamics (MHD) calculations that follow the collapse of rotating, magnetized, molecular cloud cores to stellar densities. These are the first such calculations to include all three non-ideal effects: ambipolar diffusion, Ohmic resistivity, and the Hall effect. We employ an ionization model in which cosmic ray ionization dominates at low temperatures and thermal ionization takes over at high temperatures. We explore the effects of varying the cosmic ray ionization rate from ζcr = 10−10 to 10−16 s−1. Models with ionization rates ≳10−12 s−1 produce results that are indistinguishable from ideal MHD. Decreasing the cosmic ray ionization rate extends the lifetime of the first hydrostatic core up to a factor of 2, but the lifetimes are still substantially shorter than those obtained without magnetic fields. Outflows from the first hydrostatic core phase are launched in all models, but the outflows become broader and slower as the ionization rate is reduced. The outflow morphology following stellar core formation is complex and strongly dependent on the cosmic ray ionization rate. Calculations with high ionization rates quickly produce a fast (≈14 km s−1) bipolar outflow that is distinct from the first core outflow, but with the lowest ionization rate, a slower (≈3−4 km s−1) conical outflow develops gradually and seamlessly merges into the first core outflow.
dc.format.extent22
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2018 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/stx3339en
dc.subjectMagnetic fieldsen
dc.subjectMHDen
dc.subjectRadiative transferen
dc.subjectMethods: numericalen
dc.subjectStars: formationen
dc.subjectStars: windsen
dc.subjectOutflowsen
dc.subjectQA75 Electronic computers. Computer scienceen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-DASen
dc.subject.lccQA75en
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamicsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stx3339
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1801.01126en


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