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dc.contributor.authorDobbs, C L
dc.contributor.authorWurster, J
dc.date.accessioned2021-02-09T10:30:07Z
dc.date.available2021-02-09T10:30:07Z
dc.date.issued2021-01-23
dc.identifier.citationDobbs , C L & Wurster , J 2021 , ' The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds ' , Monthly Notices of the Royal Astronomical Society . https://doi.org/10.1093/mnras/stab150en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 272795388
dc.identifier.otherPURE UUID: 6ae7a6e5-cefb-43d1-84dc-9471dbf64981
dc.identifier.otherJisc: b2d7a5e4f55647bd927d9cc349bcdc26
dc.identifier.otherORCID: /0000-0003-0688-5332/work/88731481
dc.identifier.otherWOS: 000648997200053
dc.identifier.otherScopus: 85117444372
dc.identifier.urihttps://hdl.handle.net/10023/21391
dc.descriptionFunding: LD acknowledges funding from the European Research Council for the Horizon 2020 ERC consolida-tor grant project ICYBOB, grant number 818940.en
dc.description.abstractWe have performed Smoothed Particle Magneto-Hydrodynamics (SPMHD) calculations of colliding clouds to investigate the formation of massive stellar clusters, adopting a timestep criterion to prevent large divergence errors. We find that magnetic fields do not impede the formation of young massive clusters (YMCs), and the development of high star formation rates, although we do see a strong dependence of our results on the direction of the magnetic field. If the field is initially perpendicular to the collision, and sufficiently strong, we find that star formation is delayed, and the morphology of the resulting clusters is significantly altered. We relate this to the large amplification of the field with this initial orientation. We also see that filaments formed with this configuration are less dense. When the field is parallel to the collision, there is much less amplification of the field, dense filaments form, and the formation of clusters is similar to the purely hydrodynamical case. Our simulations reproduce the observed tendency for magnetic fields to be aligned perpendicularly to dense filaments, and parallel to low density filaments. Overall our results are in broad agreement with past work in this area using grid codes.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2021 The Author(s). Published by Oxford University Press on behalf of 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 author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stab150.en
dc.subjectGeneral, ISM: cloudsen
dc.subjectStars: formationen
dc.subjectGalaxies: star clusters: generalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding cloudsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stab150
dc.description.statusPeer revieweden


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