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dc.contributor.authorWurster, James Howard
dc.contributor.authorBate, Matthew R
dc.contributor.authorBonnell, Ian Alexander
dc.date.accessioned2021-08-12T10:30:03Z
dc.date.available2021-08-12T10:30:03Z
dc.date.issued2021-08-10
dc.identifier.citationWurster , J H , Bate , M R & Bonnell , I A 2021 , ' The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation ' , Monthly Notices of the Royal Astronomical Society . https://doi.org/10.1093/mnras/stab2296en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 275421939
dc.identifier.otherPURE UUID: 3920a643-4467-4a1d-b1f0-090c0dc738f7
dc.identifier.otherORCID: /0000-0003-0688-5332/work/98488242
dc.identifier.otherScopus: 85115829562
dc.identifier.urihttp://hdl.handle.net/10023/23765
dc.descriptionFunding: JW and MRB acknowledge support from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007- 2013 grant agreement no. 339248). JW and IAB acknowledge support from the University of St Andrews.en
dc.description.abstractNon-ideal magnetohydrodynamic (MHD) processes – namely Ohmic resistivity, ambipolar diffusion and the Hall effect – modify the early stages of the star formation process and the surrounding environment. Collectively, they have been shown to promote disc formation and promote or hinder outflows. But which non-ideal process has the greatest impact? Using three-dimensional smoothed particle radiation non-ideal MHD simulations, we model the gravitational collapse of a rotating, magnetised cloud through the first hydrostatic core phase to shortly after the formation of the stellar core. We investigate the impact of each process individually and collectively. Including any non-ideal process decreases the maximum magnetic field strength by at least an order of magnitude during the first core phase compared to using ideal MHD, and promotes the formation of a magnetic wall. When the magnetic field and rotation vectors are anti-aligned and the Hall effect is included, rotationally supported discs of r ≳ 20 au form; when only the Hall effect is included and the vectors are aligned, a counter-rotating pseudo-disc forms that is not rotationally supported. Rotationally supported discs of r ≲ 4 au form if only Ohmic resistivity or ambipolar diffusion are included. The Hall effect suppresses first core outflows when the vectors are anti-aligned and suppresses stellar core outflows independent of alignment. Ohmic resistivity and ambipolar diffusion each promote first core outflows and delay the launching of stellar core outflows. Although each non-ideal process influences star formation, these results suggest that the Hall effect has the greatest influence.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2021 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/stab2296.en
dc.subjectMagnetic fieldsen
dc.subjectMHDen
dc.subjectMethods: numericalen
dc.subjectProtoplanetary discsen
dc.subjectStars: formationen
dc.subjectStars: windsen
dc.subjectOutflowsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formationen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stab2296
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2108.02787en


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