Mass and spin co-evolution during the alignment of a black hole in a warped accretion disc
dc.contributor.author | Perego, A. | en_US |
dc.contributor.author | Dotti, Massimo | en_US |
dc.contributor.author | Colpi, M. | en_US |
dc.contributor.author | Volonteri, Marta | en_US |
dc.date.accessioned | 2010-06-01T21:43:08Z | |
dc.date.available | 2010-06-01T21:43:08Z | |
dc.date.issued | 2009-11-11 | en_US |
dc.identifier.citation | Perego, A.; Dotti, M.; Colpi, M.; Volonteri, M. (2009). "Mass and spin co-evolution during the alignment of a black hole in a warped accretion disc." Monthly Notices of the Royal Astronomical Society 399(4): 2249-2263. <http://hdl.handle.net/2027.42/74763> | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.issn | 1365-2966 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/74763 | |
dc.description.abstract | In this paper, we explore the gravitomagnetic interaction of a black hole (BH) with a misaligned accretion disc to study BH spin precession and alignment jointly with BH mass M BH and spin parameter a evolution, under the assumption that the disc is continually fed, in its outer region, by matter with angular momentum fixed on a given direction . We develop an iterative scheme based on the adiabatic approximation to study the BH–disc co-evolution: in this approach, the accretion disc transits through a sequence of quasi-steady warped states (Bardeen–Petterson effect) and interacts with the BH until the spin J BH aligns with . For a BH aligning with a corotating disc, the fractional increase in mass is typically less than a few per cent, while the spin modulus can increase up to a few tens of per cent. The alignment time-scale is of ∼10 5 –10 6 yr for a maximally rotating BH accreting at the Eddington rate. BH–disc alignment from an initially counter-rotating disc tends to be more efficient compared to the specular corotating case due to the asymmetry seeded in the Kerr metric: counter-rotating matter carries a larger and opposite angular momentum when crossing the innermost stable orbit, so that the spin modulus decreases faster and so the relative inclination angle. | en_US |
dc.format.extent | 18663982 bytes | |
dc.format.extent | 3109 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Blackwell Publishing Ltd | en_US |
dc.rights | Journal compilation © 2009 RAS | en_US |
dc.subject.other | Accretion, Accretion Discs | en_US |
dc.subject.other | Black Hole Physics | en_US |
dc.subject.other | Galaxies: Active | en_US |
dc.subject.other | Galaxies: Evolution | en_US |
dc.subject.other | Quasars: General | en_US |
dc.title | Mass and spin co-evolution during the alignment of a black hole in a warped accretion disc | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Astronomy | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA | en_US |
dc.contributor.affiliationother | Department of Physics, University of Basel, Klingelbergstr. 82, 4056 Basel, Switzerland | en_US |
dc.contributor.affiliationother | Dipartimento di Fisica, UniversitÀ degli Studi di Milano-Bicocca, Piazza Della Scienza 3, 20126 Milano, Italy | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/74763/1/j.1365-2966.2009.15427.x.pdf | |
dc.identifier.doi | 10.1111/j.1365-2966.2009.15427.x | en_US |
dc.identifier.source | Monthly Notices of the Royal Astronomical Society | en_US |
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