1999/06/16 by K. S. Cheng, Y. Lu, Youjun Lu · 1 citation
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Angular momentum #Astrophysical Phenomena and Observations #Astrophysical jet #Astrophysics #Black hole (networking) #Classical mechanics #Dimensionless quantity #Galaxy #Gamma-ray burst #Gamma-ray bursts and supernovae #Jet (fluid) #Lorentz factor #Lorentz transformation #Magnetic field #Mechanics #Neutron star #Physics #Pulsars and Gravitational Waves Research #RADIUS #Rotating black hole #Rotational energy #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2001.03930.x
published as Mon.Not.Roy.Astron.Soc. 320 (2001) 235 · 20 pages, Latex, submitted to MNRAS
arxiv created 1999/06/16 · openalex publication_date 2001/01/11 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We suggest that an extreme Kerr black hole with a mass ∼106 M⊙, a dimensionless angular momentum A ∼ 1 and a marginally stable orbital radius rms ∼ 3rs ∼ 1012M6 cm located in a normal galaxy may produce a γ-ray burst (GRB) by capturing and disrupting a star. During the capture period, a transient accretion disc is formed and a strong transient magnetic field lasting for rms/c ∼ 30M6s, may be produced at the inner boundary of the accretion disc. A large amount of rotational energy of the black hole is extracted and released in an ultrarelativistic jet with a bulk Lorentz factor G larger than 103 via the Blandford—Znajek process. The relativistic jet energy can be converted into γ-radiation via an internal shock mechanism. The GRB duration should be the same as the lifetime of the strong transient magnetic field. The maximum number of sub-bursts is estimated to be rms/h ∼ (10 − 102) because the disc material is likely to break into pieces with a size about the thickness of the disc h at the cusp (2rs ≤ r ≤ 3rs). The shortest risetime of the burst estimated from this model is The model GRB density rate is also estimated.