Rotation-powered radio pulsars are born with inferred initial rotation periods1 of order 300 ms (some as short as 20 ms) in core-collapse supernovae. In the traditional picture, this fast rotation is the result of conservation of angular momentum during the collapse of a rotating stellar core. This leads to the inevitable conclusion that pulsar spin is directly correlated with the rotation of the progenitor star2. So far, however, stellar theory has not been able to explain the distribution of pulsar spins, suggesting that the birth rotation is either too slow3 or too fast2,4. Here we report 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. Sufficient angular momentum is deposited on the proto-neutron star to generate a final spin period consistent with observations, even beginning with spherically symmetrical 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.
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This work was supported by a SciDAC grant from the US Department of Energy High Energy, Nuclear Physics, and Advanced Scientific Computing Research Programs. A.M. is supported at the Oak Ridge National Laboratory, managed by UT-Battelle, LLC, for the US Department of Energy. The simulations presented here were performed at the Leadership Computing Facility at ORNL. We thank the National Center for Computational Sciences at ORNL for their resources and support.
Reprints and permissions information is available at www.nature.com/reprints. The authors declare no competing financial interests.
This file contains Supplementary Methods which describe the hydrodynamic model used to study the dynamics of the stalled supernova shock and the numerical method employed to evolve this model. (PDF 355 kb)
This file contains Supplementary Image which is a volume rendering of the gas entropy during an epoch dominated by the spiral SASI mode. The angular momentum axis is oriented vertically in this view, and the SASI wave is approaching the viewer on the right-hand side of the image. (JPG 1881 kb)
This file contains Supplementary Movie showing the evolution of the unstable accretion shock in the case of a non-rotating progenitor, illustrating the transition from the sloshing mode of the SASI to the spiral mode. The flow is depicted with a set of transparent surfaces of constant entropy, with the outermost surface representing the accretion shock. (MOV 23769 kb)
This file contains Supplementary Movie showing the flow in the equatorial plane (as defined by the SASI rotation) for one rotational period of the spiral SASI mode. The color scale corresponds to gas entropy. (MOV 7632 kb)
This file contains Supplementary Movie showing the rapid development of the spiral mode of the SASI in the case of a rotating progenitor star. The solid surface represents the accretion shock, colored by the gas density at the shock. (MOV 9770 kb)
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Blondin, J., Mezzacappa, A. Pulsar spins from an instability in the accretion shock of supernovae. Nature 445, 58–60 (2007). https://doi.org/10.1038/nature05428
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