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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.identifier275421939
dc.identifier3920a643-4467-4a1d-b1f0-090c0dc738f7
dc.identifier85115829562
dc.identifier000697380800052
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.otherORCID: /0000-0003-0688-5332/work/98488242
dc.identifier.urihttps://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.format.extent6230635
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
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.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.1093/mnras/stab2296
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2108.02787en


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