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The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation
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dc.contributor.author | Wurster, James Howard | |
dc.contributor.author | Bate, Matthew R | |
dc.contributor.author | Bonnell, Ian Alexander | |
dc.date.accessioned | 2021-08-12T10:30:03Z | |
dc.date.available | 2021-08-12T10:30:03Z | |
dc.date.issued | 2021-08-10 | |
dc.identifier | 275421939 | |
dc.identifier | 3920a643-4467-4a1d-b1f0-090c0dc738f7 | |
dc.identifier | 85115829562 | |
dc.identifier | 000697380800052 | |
dc.identifier.citation | Wurster , 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/stab2296 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | ORCID: /0000-0003-0688-5332/work/98488242 | |
dc.identifier.uri | https://hdl.handle.net/10023/23765 | |
dc.description | Funding: 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.abstract | Non-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.extent | 6230635 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Magnetic fields | en |
dc.subject | MHD | en |
dc.subject | Methods: numerical | en |
dc.subject | Protoplanetary discs | en |
dc.subject | Stars: formation | en |
dc.subject | Stars: winds | en |
dc.subject | Outflows | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation | en |
dc.type | Journal article | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.1093/mnras/stab2296 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/2108.02787 | en |
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