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Magnetohydrodynamical simulations of a deep tidal disruption in general relativity
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC). Universidad Nacional Autónoma de México, Mexico.
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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Number of Authors: 5
2016 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 458, no 4, 4250-4268 p.Article in journal (Refereed) Published
Abstract [en]

We perform hydro- and magnetohydrodynamical general-relativistic simulations of a tidal disruption of a 0.1 M-circle dot red dwarf approaching a 10(5) M-circle dot non-rotating massive black hole on a close (impact parameter beta = 10) elliptical (eccentricity e = 0.97) orbit. We track the debris self-interaction, circularization and the accompanying accretion through the black hole horizon. We find that the relativistic precession leads to the formation of a self-crossing shock. The dissipated kinetic energy heats up the incoming debris and efficiently generates a quasi-spherical outflow. The self-interaction is modulated because of the feedback exerted by the flow on itself. The debris quickly forms a thick, almost marginally bound disc that remains turbulent for many orbital periods. Initially, the accretion through the black hole horizon results from the self-interaction, while in the later stages it is dominated by the debris originally ejected in the shocked region, as it gradually falls back towards the hole. The effective viscosity in the debris disc stems from the original hydrodynamical turbulence, which dominates over the magnetic component. The radiative efficiency is very low because of low energetics of the gas crossing the horizon and large optical depth that results in photon trapping. Although the parameters of the simulated tidal disruption are probably not representative of most observed events, it is possible to extrapolate some of its properties towards more common configurations.

Place, publisher, year, edition, pages
2016. Vol. 458, no 4, 4250-4268 p.
Keyword [en]
accretion, accretion discs, black hole physics, relativistic processes, methods: numerical
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-132058DOI: 10.1093/mnras/stw589ISI: 000375799500068OAI: oai:DiVA.org:su-132058DiVA: diva2:948906
Available from: 2016-07-14 Created: 2016-07-06 Last updated: 2016-07-14Bibliographically approved

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Gafton, EmanuelRosswog, Stephan
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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