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Evolution of the M•-σ relation

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dc.contributor.author Bhattacharyya, D
dc.contributor.author Mangalam, A
dc.date.accessioned 2020-11-27T12:55:21Z
dc.date.available 2020-11-27T12:55:21Z
dc.date.issued 2018-05
dc.identifier.citation Proceedings of the International Astronomical Union, Vol. 342, pp. 254-256 en_US
dc.identifier.issn 1743-9213
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7507
dc.description Restricted Access © International Astronomical Union https://doi.org/10.1017/S1743921318007251 en_US
dc.description.abstract Black holes at the centers of the galaxies grow mainly by the processes of accretion, mergers, and consumption of stars. In the case of gas accretion with cooling sources, the flow is momentum driven, after which the black hole reaches a saturated mass, and subsequently, it grows only by consumption of stars. In addition, we include the effect of mergers on the growth of black hole spin and mass and study its evolution as a function of redshift in a ΛCDM cosmology using an initial seed mass and spin distribution functions that we have derived. For the stellar ingestion, we have assumed a power-law density profile for the galaxy in our framework of a new relativistic loss cone theory that includes the effect of the black hole spin. We predict the impact of the evolution on the M•−σ relation and compare it with available observations. en_US
dc.language.iso en en_US
dc.publisher Cambridge University Press en_US
dc.relation.ispartofseries IAU Symposium No. 342;
dc.subject spin, mass of black hole en_US
dc.subject M• en_US
dc.subject σ relation en_US
dc.subject redshift en_US
dc.subject evolution en_US
dc.title Evolution of the M•-σ relation en_US
dc.type Article en_US

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