1999/11/30 by M. Á. Aloy, Miguel A. Aloy, Ewald Mueller +6 · 307 citations
Physics and Astronomy · #Active galactic nucleus #Astrophysical jet #Astrophysics #Astrophysics and Cosmic Phenomena #Classical mechanics #Collimated light #Flow (mathematics) #Galaxy #Gamma-ray bursts and supernovae #Geometry #Jet (fluid) #Lorentz factor #Lorentz transformation #Mechanics #Optics #Physics #Pulsars and Gravitational Waves Research #Rotation (mathematics) #astro-ph
paper · pdf · doi:10.1086/312537
published in The Astrophysical Journal 531(2), L119-L122 (IOP Publishing) · 7 pages, 4 figures, ApJL accepted
arxiv created 2000/01/17 · openalex publication_date 2000/03/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Using a collapsar progenitor model of MacFadyen & Woosley, we have simulated the propagation of an axisymmetric jet through a collapsing rotating massive star with the GENESIS multidimensional relativistic hydrodynamic code. The jet forms as a consequence of an assumed (constant or variable) energy deposition in the range of 1050-1051 ergs s-1 within a 30 degrees cone around the rotation axis. The jet flow is strongly beamed (approximately less than a few degrees), spatially inhomogeneous, and time dependent. The jet reaches the surface of the stellar progenitor (R*=2.98x1010 cm) intact. At breakout, the maximum Lorentz factor of the jet flow is 33. After breakout, the jet accelerates into the circumstellar medium, whose density is assumed to decrease exponentially and then become constant, rhoext=10-5 g cm-3. Outside the star, the flow begins to expand laterally also (v approximately c), but the beam remains very well collimated. At a distance of 2.54 R*, where the simulation ends, the Lorentz factor has increased to 44.