Black Hole Hyperaccretion Inflow-Outflow Model. I. Long and Ultra-long Gamma-Ray Bursts

Long-duration gamma-ray bursts (LGRBs) and ultra-LGRBs (ULGRBs) originate from collapsars, in the center of which a newborn rotating stellar-mass black hole (BH) surrounded by a massive accretion disk may form. In the scenario of the BH hyperaccretion inflow-outflow model and Blandford-Znajek (BZ) m...

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Bibliographic Details
Published in:The Astrophysical journal 2018-01, Vol.852 (1), p.20
Main Authors: Liu, Tong, Song, Cui-Ying, Zhang, Bing, Gu, Wei-Min, Heger, Alexander
Format: Article
Language:English
Subjects:
Accretion disks
accretion, accretion disks
Astrophysics
black hole physics
Black holes
Collapsars
Gamma ray bursts
Gamma rays
gamma-ray burst: general
Inflow
Luminosity
Magnetars
magnetic fields
Metallicity
Outflow
Population III stars
Stars
stars: massive
Stellar rotation
Time
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Summary:Long-duration gamma-ray bursts (LGRBs) and ultra-LGRBs (ULGRBs) originate from collapsars, in the center of which a newborn rotating stellar-mass black hole (BH) surrounded by a massive accretion disk may form. In the scenario of the BH hyperaccretion inflow-outflow model and Blandford-Znajek (BZ) mechanism to trigger gamma-ray bursts (GRBs), the real accretion rate to power a BZ jet is far lower than the mass supply rate from the progenitor star. The characteristics of the progenitor stars can be constrained by GRB luminosity observations, and the results exceed usual expectations. LGRBs lasting from several seconds to tens of seconds in the rest frame may originate from solar-metallicity ( , where Z and are the metallicities of progenitor stars and the Sun), massive ( , where M and are the masses of progenitor stars and the Sun) stars or some zero-metallicity ( ) stars. A fraction of low-metallicity ( ) stars, including Population III stars, can produce ULGRBs such as GRB 111209A. The fraction of LGRBs lasting less than tens of seconds in the rest frame is more than 40%, which cannot conform to the fraction of the demanded type of progenitor star. It possibly implies that the activity timescale of the central engine may be much longer than the observed timescale of prompt emission phase, as indicated by X-ray late-time activities. Alternatively, LGRBs and ULGRBs may be powered by a millisecond magnetar central engine.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/aa9e4f