Statistics – Computation
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20915006b&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #150.06; Bulletin of the American Astronomical Society,
Statistics
Computation
Scientific paper
Using three-dimensional hydrodynamics simulations, we have identified a robust instability of the stalled accretion shock in core-collapse supernovae that is able to generate a strong rotational flow in the vicinity of the accreting proto-neutron star (PNS). Sufficient angular momentum is deposited on the PNS to generate a final neutron star spin period consistent with observations of radio pulsars, even beginning with spherically symmetric, non-rotating initial conditions. This provides a new mechanism for the generation of neutron star spin and weakens, if not breaks, the assumed correlation between the rotational periods of supernova progenitor cores and pulsar spin.
This research used resources of the National Center for Computational Sciences at Oak Ridge National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC05-00OR22725.
Blondin John M.
Mezzacappa Anthony
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