| Title | Black Hole Hyperaccretion Inflow-Outflow Model. I. Long and Ultra-long Gamma-Ray Bursts |
| Authors | Liu, Tong Song, Cui-Ying Zhang, Bing Gu, Wei-Min Heger, Alexander |
| Affiliation | Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China. Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. Monash Univ, Monash Ctr Astrophys, Clayton, Vic 3800, Australia. Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Shanghai Jiao Tong Univ, Dept Phys & Astron, Shanghai 200240, Peoples R China. |
| Keywords | accretion, accretion disks black hole physics gamma-ray burst: general magnetic fields stars: massive BLANDFORD-ZNAJEK PROCESS ROTATING MASSIVE STARS COOLED ACCRETION DISKS NEUTRON-STARS MILLISECOND PULSARS CENTRAL ENGINE ENERGY INJECTION MAGNETIC-FIELDS SWIFT DATA EVOLUTION |
| Issue Date | 2018 |
| Publisher | ASTROPHYSICAL JOURNAL |
| Citation | ASTROPHYSICAL JOURNAL. 2018, 852(1). |
| Abstract | 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 (Z similar to 1Z(circle dot), where Z and Z(circle dot) are the metallicities of progenitor stars and the Sun), massive (M greater than or similar to 34 M-circle dot, where M and M-circle dot are the masses of progenitor stars and the Sun) stars or some zero-metallicity (Z similar to 0) stars. A fraction of low-metallicity (Z less than or similar to 10(-2) Z(circle dot)) 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. |
| URI | http://hdl.handle.net/20.500.11897/500161 |
| ISSN | 0004-637X |
| DOI | 10.3847/1538-4357/aa9e4f |
| Indexed | SCI(E) |
| Appears in Collections: | 物理学院 科维理天文与天体物理研究所 |
