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dc.contributor.authorForgan, Duncan
dc.contributor.authorPrice, Daniel J.
dc.contributor.authorBonnell, Ian
dc.date.accessioned2017-05-19T11:30:10Z
dc.date.available2017-05-19T11:30:10Z
dc.date.issued2017-04
dc.identifier250036018
dc.identifiere3a9011c-d35d-461d-8a5b-529199aa6702
dc.identifier85018365259
dc.identifier000398418600063
dc.identifier.citationForgan , D , Price , D J & Bonnell , I 2017 , ' On the fragmentation boundary in magnetized self-gravitating discs ' , Monthly Notices of the Royal Astronomical Society , vol. 466 , no. 3 , pp. 3406-3416 . https://doi.org/10.1093/mnras/stw3314en
dc.identifier.issn0035-8711
dc.identifier.urihttps://hdl.handle.net/10023/10800
dc.descriptionDHF and IAB gratefully acknowledge support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ER-2011-ADG. DJP gratefully acknowledges funding via grants DP130102078 and FT130100034 and via Future Fellowship FT130100034 from the Australian Research Council.en
dc.description.abstractWe investigate the role of magnetic fields in the fragmentation of self-gravitating discs using 3D global ideal magnetohydrodynamic simulations performed with the PHANTOM smoothed particle hydrodynamics code. For initially toroidal fields, we find two regimes. In the first, where the cooling time is greater than five times the dynamical time, magnetic fields reduce spiral density wave amplitudes, which in turn suppresses fragmentation. This is the case even if the magnetic pressure is only a 10th of the thermal pressure. The second regime occurs when the cooling time is sufficiently short that magnetic fields cannot halt fragmentation.We find that magnetized discs produce more massive fragments, due to both the additional pressure exerted by the magnetic field and the additional angular momentum transport induced by Maxwell stresses. The fragments are confined to a narrower range of initial semimajor axes than those in unmagnetized discs. The orbital eccentricity and inclination distributions of unmagnetized and magnetized disc fragments are similar. Our results suggest that the fragmentation boundary could be at cooling times a factor of 2 lower than predicted by purely hydrodynamical models.
dc.format.extent11
dc.format.extent2330985
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.subjectAccretion: accretion discsen
dc.subjectStars: formationen
dc.subjectQuasars: supermassive black holesen
dc.subjectPlanets and satellites: formationen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleOn the fragmentation boundary in magnetized self-gravitating discsen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Research Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw3314
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1612.06145en
dc.identifier.grantnumberen


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