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Gravitoturbulence in magnetized protostellar discs

dc.creatorRiols, A
dc.creatorLatter, Henrik Nils
dc.date.accessioned2016-05-09
dc.date.accessioned2018-11-24T23:18:59Z
dc.date.available2016-06-17T14:41:40Z
dc.date.available2018-11-24T23:18:59Z
dc.date.issued2016-05-11
dc.identifierhttps://www.repository.cam.ac.uk/handle/1810/256368
dc.identifier.urihttp://repository.aust.edu.ng/xmlui/handle/123456789/3383
dc.description.abstractGravitational instability (GI) features in several aspects of protostellar disc evolution, most notably in angular momentum transport, fragmentation, and the outbursts exemplified by FU Ori and EX Lupi systems. The outer regions of protostellar discs may also be coupled to magnetic fields, which could then modify the development of GI. To understand the basic elements of their interaction, we perform local 2D ideal and resistive magnetohydrodynamics simulations with an imposed toroidal field. In the regime of moderate plasma beta, we find that the system supports a hot gravitoturbulent state, characterized by considerable magnetic energy and stress and a surprisingly large Toomre parameter Q ≳ 10. This result has potential implications for disc structure, vertical thickness, ionization, etc. Our simulations also reveal the existence of long-lived and dense ‘magnetic islands’ or plasmoids. Lastly, we find that the presence of a magnetic field has little impact on the fragmentation criterion of the disc. Though our focus is on protostellar discs, some of our results may be relevant for the outer radii of AGN.
dc.languageen
dc.publisherOxford University Press
dc.publisherMonthly Notices of the Royal Astronomical Society
dc.subjectinstabilities
dc.subjectMHD
dc.subjectturbulence
dc.subjectprotoplanetary discs
dc.titleGravitoturbulence in magnetized protostellar discs
dc.typeArticle


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