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Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores
Item metadata
dc.contributor.author | Wurster, J. | |
dc.contributor.author | Bate, Matthew R. | |
dc.contributor.author | Price, Daniel J. | |
dc.date.accessioned | 2019-10-25T09:30:05Z | |
dc.date.available | 2019-10-25T09:30:05Z | |
dc.date.issued | 2018-11 | |
dc.identifier.citation | Wurster , J , Bate , M R & Price , D J 2018 , ' Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores ' , Monthly Notices of the Royal Astronomical Society , vol. 480 , no. 4 , pp. 4434-4442 . https://doi.org/10.1093/mnras/sty2212 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | PURE: 262150176 | |
dc.identifier.other | PURE UUID: 38408421-e633-4c42-af68-4bad83c46e10 | |
dc.identifier.other | Bibtex: WursterBatePrice2018hd | |
dc.identifier.other | Scopus: 85055184462 | |
dc.identifier.other | ORCID: /0000-0003-0688-5332/work/63716939 | |
dc.identifier.uri | https://hdl.handle.net/10023/18765 | |
dc.description.abstract | We demonstrate the formation of gravitationally unstable discs in magnetized molecular cloud cores with initial mass-to-flux ratios of five times the critical value, effectively solving the magnetic braking catastrophe. We model the gravitational collapse through to the formation of the stellar core, using Ohmic resistivity, ambipolar diffusion and the Hall effect, and using the canonical cosmic ray ionization rate of ζcr = 10−17 s−1. When the magnetic field and rotation axis are initially aligned, a ≲ 1 au disc forms after the first core phase, whereas when they are anti-aligned, a gravitationally unstable 25 au disc forms during the first core phase. The aligned model launches a 3 km s−1 first core outflow, while the anti-aligned model launches only a weak ≲ 0.3 km s−1 first core outflow. Qualitatively, we find that models with ζcr = 10−17 s−1 are similar to purely hydrodynamical models if the rotation axis and magnetic field are initially anti-aligned, whereas they are qualitatively similar to ideal magnetohydrodynamical models if initially aligned. | |
dc.format.extent | 9 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
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/sty2212 | en |
dc.subject | Accretion disc | en |
dc.subject | Magnetic fields | en |
dc.subject | MHD | en |
dc.subject | Methods: numerical | en |
dc.subject | Stars: formation | en |
dc.subject | QA75 Electronic computers. Computer science | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | DAS | en |
dc.subject.lcc | QA75 | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores | en |
dc.type | Journal article | en |
dc.description.version | Publisher PDF | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.1093/mnras/sty2212 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/1808.04376 | en |
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