2007/07/31 by N. Bucciantini, Eliot Quataert, E. Quataert +5 · 4 citations
Physics and Astronomy · #Astronomy #Astrophysical jet #Astrophysics #Astrophysics and Cosmic Phenomena #Classical mechanics #Galaxy #Gamma-ray burst #Gamma-ray bursts and supernovae #Jet (fluid) #Lorentz factor #Lorentz transformation #Magnetar #Magnetic field #Mechanics #Neutron star #Physics #Pulsars and Gravitational Waves Research #Supernova #astro-ph
paper · pdf · doi:10.1111/j.1745-3933.2007.00403.x
5 pages, 3 figures, accepted in MNRAS letter, presented at the conference "Astrophysics of Compact Objects", 1-7 July, Huangshan, China
arxiv created 2007/09/26 · openalex publication_date 2007/11/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We present time-dependent axisymmetric magnetohydrodynamic simulations of the interaction of a relativistic magnetized wind produced by a proto-magnetar with a surrounding stellar envelope, in the first ∼10 s after core collapse. We inject a super-magnetosonic wind with into a cavity created by an outgoing supernova shock. A strong toroidal magnetic field builds up in the bubble of plasma and magnetic field that is at first inertially confined by the progenitor star. This drives a jet out along the polar axis of the star, even though the star and the magnetar wind are each spherically symmetric. The jet has the properties needed to produce a long-duration gamma-ray burst (GRB). At ∼5 s after core bounce, the jet has escaped the host star and the Lorentz factor of the material in the jet at large radii ∼1011 cm is similar to that in the magnetar wind near the source. Most of the spindown power of the central magnetar escapes via the relativistic jet. There are fluctuations in the Lorentz factor and energy flux in the jet on a ∼ 0.01–0.1 s time-scale. These may contribute to variability in GRB emission (e.g. via internal shocks).