dc.contributor.author | Wurster, J | |
dc.contributor.author | Bate, MR | |
dc.contributor.author | Bonnell, IA | |
dc.date.accessioned | 2021-08-09T09:46:41Z | |
dc.date.issued | 2021-08-10 | |
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. | en_GB |
dc.description.sponsorship | European Union FP7 | en_GB |
dc.description.sponsorship | University of St Andrews | en_GB |
dc.identifier.citation | Published online 10 August 2021 | en_GB |
dc.identifier.doi | 10.1093/mnras/stab2296 | |
dc.identifier.grantnumber | 339248 | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/126714 | |
dc.language.iso | en | en_GB |
dc.publisher | Oxford University Press (OUP) / Royal Astronomical Society | en_GB |
dc.relation.url | https://doi.org/10.24378/exe.607 | en_GB |
dc.rights | © 2021 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society | |
dc.subject | magnetic fields | en_GB |
dc.subject | MHD | en_GB |
dc.subject | methods: numerical | en_GB |
dc.subject | protoplanetary discs | en_GB |
dc.subject | stars: formation | en_GB |
dc.subject | stars: winds, outflows | en_GB |
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_GB |
dc.type | Article | en_GB |
dc.date.available | 2021-08-09T09:46:41Z | |
dc.identifier.issn | 0035-8711 | |
dc.description | This is the author accepted manuscript. The final version is available from the Royal Astronomical Society via the DOI in this record | en_GB |
dc.description | Data availability: The data for models iMHD and ohaMHD± are openly available from the University of Exeters institutional repository at
https://doi.org/10.24378/exe.607. The data for the remaining models will be available upon reasonable request. | en_GB |
dc.identifier.journal | Monthly Notices of the Royal Astronomical Society | en_GB |
dc.rights.uri | http://www.rioxx.net/licenses/all-rights-reserved | en_GB |
dcterms.dateAccepted | 2021-08-04 | |
exeter.funder | ::European Commission | en_GB |
rioxxterms.version | AM | en_GB |
rioxxterms.licenseref.startdate | 2021-08-04 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2021-08-07T17:58:02Z | |
refterms.versionFCD | AM | |
refterms.dateFOA | 2021-08-20T15:02:24Z | |
refterms.panel | B | en_GB |