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dc.contributor.authorWurster, J.
dc.contributor.authorPrice, D. J.
dc.contributor.authorBate, M. R.
dc.date.accessioned2019-10-22T12:30:05Z
dc.date.available2019-10-22T12:30:05Z
dc.date.issued2017-04
dc.identifier.citationWurster , J , Price , D J & Bate , M R 2017 , ' The impact of non-ideal magnetohydrodynamics on binary star formation ' , Monthly Notices of the Royal Astronomical Society , vol. 466 , no. 2 , pp. 1788-1804 . https://doi.org/10.1093/mnras/stw3181en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 262150395
dc.identifier.otherPURE UUID: e437b621-a368-4668-8446-3b2a879de749
dc.identifier.otherBibtex: WursterPriceBate2017
dc.identifier.otherORCID: /0000-0003-0688-5332/work/63716935
dc.identifier.otherScopus: 85023767578
dc.identifier.urihttp://hdl.handle.net/10023/18743
dc.description.abstractWe investigate the effect of non-ideal magnetohydrodynamics (MHD) on the formation of binary stars using a suite of three-dimensional smoothed particle magnetohydrodynamics simulations of the gravitational collapse of 1 M⊙, rotating, perturbed molecular-cloud cores. Alongside the role of Ohmic resistivity, ambipolar diffusion and the Hall effect, we also examine the effects of magnetic field strength, orientation and amplitude of the density perturbation. When modelling sub-critical cores, ideal MHD models do not collapse whereas non-ideal MHD models collapse to form single protostars. In supercritical ideal MHD models, increasing the magnetic field strength or decreasing the initial-density perturbation amplitude decreases the initial binary separation. Strong magnetic fields initially perpendicular to the rotation axis suppress the formation of binaries and yield discs with magnetic fields ∼10 times stronger than if the magnetic field was initially aligned with the rotation axis. When non-ideal MHD is included, the resulting discs are larger and more massive, and the binary forms on a wider orbit. Small differences in the supercritical cores caused by non-ideal MHD effects are amplified by the binary interaction near periastron. Overall, the non-ideal effects have only a small impact on binary formation and early evolution, with the initial conditions playing the dominant role.
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016 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/stw3181en
dc.subjectMagnetic fieldsen
dc.subjectMHDen
dc.subjectMethods: numericalen
dc.subjectBinaries: generalen
dc.subjectStars: formationen
dc.subjectQA75 Electronic computers. Computer scienceen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQA75en
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe impact of non-ideal magnetohydrodynamics on binary star formationen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw3181
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1612.02016en


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