Collisional Dark Matter and the Origin of Massive Black Holes

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dc.creatorOstriker, Jeremiah P.
dc.date1999-12-29
dc.date2000-04-17
dc.date.accessioned2026-07-07T12:01:12Z
dc.date.available2026-07-07T12:01:12Z
dc.descriptionIf the cosmological dark matter is primarily in the form of an elementary particle which has cross section and mass for self-interaction having a ratio similar to that of ordinary nuclear matter, then seed black holes (formed in stellar collapse) will grow in a Hubble time, due to accretion of the dark matter, to a mass range 10^6 - 10^9 solar masses. Furthermore, the dependence of the final black hole mass on the galaxy velocity dispersion will be approximately as observed and the growth rate will show a time dependence consistent with observations. Other astrophysical consequences of collisional dark matter and tests of the idea are noted.
dc.description7 pages, no figures, LaTeX2e, Accepted for publication in Phys. Rev. Lett. Changed content
dc.identifierhttps://arxiv.org/abs/astro-ph/9912548
dc.identifierhttp://arxiv.org/abs/astro-ph/9912548
dc.identifierPhys.Rev.Lett.84:5258-5260,2000
dc.identifierdoi:10.1103/PhysRevLett.84.5258
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/207022
dc.subjectAstrophysics
dc.titleCollisional Dark Matter and the Origin of Massive Black Holes
dc.typetext

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