The formation of stellar black holes

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It is believed that stellar black holes (BHs) can be formed in two different ways: Either a massive star collapses directly into a BH without a supernova (SN) explosion, or an explosion occurs in a proto-neutron star, but the energy is too low to completely unbind the stellar envelope, and a large f...

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Autor principal: Mirabel, F.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: Elsevier B.V. 2017
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Mirabel, F. 
245 1 4 |a The formation of stellar black holes 
260 |b Elsevier B.V.  |c 2017 
506 |2 openaire  |e Política editorial 
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520 3 |a It is believed that stellar black holes (BHs) can be formed in two different ways: Either a massive star collapses directly into a BH without a supernova (SN) explosion, or an explosion occurs in a proto-neutron star, but the energy is too low to completely unbind the stellar envelope, and a large fraction of it falls back onto the short-lived neutron star (NS), leading to the delayed formation of a BH. Theoretical models set progenitor masses for BH formation by implosion, namely, by complete or almost complete collapse, but observational evidences have been elusive. Here are reviewed the observational insights on BHs formed by implosion without large natal kicks from: (1) the kinematics in three dimensions of space of five Galactic BH X-ray binaries (BH-XRBs), (2) the diversity of optical and infrared observations of massive stars that collapse in the dark, with no luminous SN explosions, possibly leading to the formation of BHs, and (3) the sources of gravitational waves (GWs) produced by mergers of stellar BHs so far detected with LIGO. Multiple indications of BH formation without ejection of a significant amount of matter and with no natal kicks obtained from these different areas of observational astrophysics, and the recent observational confirmation of the expected dependence of BH formation on metallicity and redshift, are qualitatively consistent with the high merger rates of binary black holes (BBHs) inferred from the first detections with LIGO. © 2017 Elsevier B.V.  |l eng 
593 |a Institute of Astronomy and Space Physics, CONICET-Universidad de Buenos Aires, Ciudad Universitaria, Buenos Aires, 1428, Argentina 
593 |a Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu−CNRS, CEA-Saclay, pt courrier 131, Gif-sur-Yvette, 91191, France 
690 1 0 |a BINARY BACK HOLES 
690 1 0 |a BLACK HOLES 
690 1 0 |a GRAVITATIONAL WAVES 
690 1 0 |a X-RAY BINARIES 
773 0 |d Elsevier B.V., 2017  |g v. 78  |h pp. 1-15  |p New Astron. Rev.  |x 13876473  |w (AR-BaUEN)CENRE-6280  |t New Astronomy Reviews 
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856 4 0 |u https://doi.org/10.1016/j.newar.2017.04.002  |y DOI 
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999 |c 86393 

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