Stellar-Mass Black Holes and Their Progenitors

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dc.creatorMiller, J. M.
dc.creatorUttley, P.
dc.creatorNandra, K.
dc.creatorBarret, D.
dc.creatorMatt, G.
dc.creatorPaerels, F.
dc.creatorMendez, M.
dc.creatorTrigo, M. Diaz
dc.creatorCappi, M.
dc.creatorKitamoto, S.
dc.creatorNowak, M.
dc.creatorWilms, J.
dc.creatorRothschild, R.
dc.creatorSmith, R.
dc.creatorWeisskopf, M.
dc.creatorTerashima, Y.
dc.creatorUeda, Y.
dc.date2009-02-26
dc.date.accessioned2026-07-07T12:47:12Z
dc.date.available2026-07-07T12:47:12Z
dc.descriptionIf a black hole has a low spin value, it must double its mass to reach a high spin parameter. Although this is easily accomplished through mergers or accretion in the case of supermassive black holes in galactic centers, it is impossible for stellar-mass black holes in X-ray binaries. Thus, the spin distribution of stellar-mass black holes is almost pristine, largely reflective of the angular momentum imparted at the time of their creation. This fact can help provide insights on two fundamental questions: What is the nature of the central engine in supernovae and gamma-ray bursts? and What was the spin distribution of the first black holes in the universe?
dc.descriptionAstro 2010 Science White Paper
dc.identifierhttps://arxiv.org/abs/0902.4677
dc.identifierhttp://arxiv.org/abs/0902.4677
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/221637
dc.subjectHigh Energy Astrophysical Phenomena
dc.subjectSolar and Stellar Astrophysics
dc.titleStellar-Mass Black Holes and Their Progenitors
dc.typetext

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