2003/01/17 by S. E. Woosley, Alexander Heger, Woosley, S. E. +2
Physics and Astronomy · #Angular momentum #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics (astro-ph) #Compact star #Ejecta #FOS: Physical sciences #Gamma-ray burst #Gamma-ray bursts and supernovae #Neutrino #Neutron star #Nuclear physics #Physics #Pulsar #Pulsars and Gravitational Waves Research #Rotation (mathematics) #Rotation period #Stars #Stellar rotation #Supernova #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0301373
published in arXiv (Cornell University) (Cornell University) · 12 pages, 2 figures, to appear in Proc. IAU 215 "Stellar Rotation"
arxiv created 2003/01/17 · openalex publication_date 2003/01/17 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/08
One of the most dramatic possible consequences of stellar rotation is its influence on stellar death, particularly of massive stars. If the angular momentum of the iron core when it collapses is such as to produce a neutron star with a period of 5 ms or less, rotation will have important consequences for the supernova explosion mechanism. Still shorter periods, corresponding to a neutron star rotating at break up, are required for the progenitors of gamma-ray bursts (GRBs). Current stellar models, while providing an excess of angular momentum to pulsars, still fall short of what is needed to make GRBs. The possibility of slowing young neutron stars in ordinary supernovae by a combination of neutrino-powered winds and the propeller mechanism is discussed. The fall back of slowly moving ejecta during the first day of the supernova may be critical. GRBs, on the other hand, probably require stellar mergers for their production and perhaps less efficient mass loss and magnetic torques than estimated thus far.