Microquasars and ULXS: Fossils of GRB sources

Gamma-ray bursts (GRBs) of long duration probably result from the core-collapse of massive stars in binary systems. After the collapse of the primary star the binary system may remain bound leaving a microquasar or ULX source as remnant. In this context, microquasars and ULXs are fossils of GRB sour...

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Guardado en:
Detalles Bibliográficos
Publicado: 2004
Materias:
Accretion
Accretion discs
X-rays:Binaries
X-rays:Stars
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_14052059_v20_n_p14_Mirabel
http://hdl.handle.net/20.500.12110/paper_14052059_v20_n_p14_Mirabel
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_14052059_v20_n_p14_Mirabel
record_format dspace
spelling paper:paper_14052059_v20_n_p14_Mirabel2023-06-08T16:13:17Z Microquasars and ULXS: Fossils of GRB sources Accretion Accretion discs X-rays:Binaries X-rays:Stars Gamma-ray bursts (GRBs) of long duration probably result from the core-collapse of massive stars in binary systems. After the collapse of the primary star the binary system may remain bound leaving a microquasar or ULX source as remnant. In this context, microquasars and ULXs are fossils of GRB sources and should contain physical and astrophysical clues on their GRB-source progenitors. Here I show that the identification of the birth place of microquasars can provide constrains on the progenitor stars of compact objects, and that the runaway velocity can be used to constrain the energy in the explosion of massive stars that leave neutron stars and black holes. The observations show that the neutron star binaries LS 5039, LSI +61°303 and the low-mass black hole GRO J1655-40 formed in energetic supernova explosions, whereas the black holes of larger masses (M ≥ 10 M) in Cygnus X-1 and GRS 1915+105 formed promptly, in the dark or in underluminous supernovae. The association with clusters of massive stars of the microquasar LSI +61°303 and the magnetars SGR 1806-20 and SGR 1900+14, suggest that very massive stars (M≥ 50 M) may -in some cases- leave neutron stars rather than black holes. The models of GRB sources of long duration have the same basic ingredients as microquasars and ULXs: compact objects with accretion disks and relativistic jets in binary systems. Therefore, the analogies between microquasars and AGN may be extended to the sources of GRBs. © Copyright 2004: IA, UNAM). 2004 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_14052059_v20_n_p14_Mirabel http://hdl.handle.net/20.500.12110/paper_14052059_v20_n_p14_Mirabel
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Accretion
Accretion discs
X-rays:Binaries
X-rays:Stars
spellingShingle Accretion
Accretion discs
X-rays:Binaries
X-rays:Stars
Microquasars and ULXS: Fossils of GRB sources
topic_facet Accretion
Accretion discs
X-rays:Binaries
X-rays:Stars
description Gamma-ray bursts (GRBs) of long duration probably result from the core-collapse of massive stars in binary systems. After the collapse of the primary star the binary system may remain bound leaving a microquasar or ULX source as remnant. In this context, microquasars and ULXs are fossils of GRB sources and should contain physical and astrophysical clues on their GRB-source progenitors. Here I show that the identification of the birth place of microquasars can provide constrains on the progenitor stars of compact objects, and that the runaway velocity can be used to constrain the energy in the explosion of massive stars that leave neutron stars and black holes. The observations show that the neutron star binaries LS 5039, LSI +61°303 and the low-mass black hole GRO J1655-40 formed in energetic supernova explosions, whereas the black holes of larger masses (M ≥ 10 M) in Cygnus X-1 and GRS 1915+105 formed promptly, in the dark or in underluminous supernovae. The association with clusters of massive stars of the microquasar LSI +61°303 and the magnetars SGR 1806-20 and SGR 1900+14, suggest that very massive stars (M≥ 50 M) may -in some cases- leave neutron stars rather than black holes. The models of GRB sources of long duration have the same basic ingredients as microquasars and ULXs: compact objects with accretion disks and relativistic jets in binary systems. Therefore, the analogies between microquasars and AGN may be extended to the sources of GRBs. © Copyright 2004: IA, UNAM).
title Microquasars and ULXS: Fossils of GRB sources
title_short Microquasars and ULXS: Fossils of GRB sources
title_full Microquasars and ULXS: Fossils of GRB sources
title_fullStr Microquasars and ULXS: Fossils of GRB sources
title_full_unstemmed Microquasars and ULXS: Fossils of GRB sources
title_sort microquasars and ulxs: fossils of grb sources
publishDate 2004
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_14052059_v20_n_p14_Mirabel
http://hdl.handle.net/20.500.12110/paper_14052059_v20_n_p14_Mirabel
_version_ 1768546175304073216

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