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Neutron Star Kicks and Asymmetric Supernovae

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Physics of Neutron Star Interiors

Part of the book series: Lecture Notes in Physics ((LNP,volume 578))

Abstract

Observational advances over the last decade have left little doubt that neutron stars received a large kick velocity (of order a few hundred to a thousand kms?1) at birth. The physical origin of the kicks and the related supernova asymmetry is one of the central unsolved mysteries of supernova research. We review the physics of different kick mechanisms, including hydrodynamically driven, neutrino— magnetic field driven, and electromagnetically driven kicks. The viabilities of the different kick mechanisms are directly related to the other key parameters characterizing nascent neutron stars, such as the initial magnetic field and the initial spin. Recent observational constraints on kick mechanisms are also discussed.

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Author information

Authors and Affiliations

  1. Center for Radiophysics and Space Research, Department of Astronomy, Cornell University, 14853, Ithaca, NY, USA

    Dong Lai

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  1. Dong Lai
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Editor information

Editors and Affiliations

  1. Fachbereich Physik, Universität Rostock, 18051, Rostock, Deutschland

    David Blaschke

  2. Institut de Physique Nuclaire, Groupe de Physique Theorique, 15, rue Georges Clemenceau, 91406, Orsay Cedex, France

    Armen Sedrakian

  3. Institute for Nuclear and Particle Astrophysics Nuclear Science Division, Lawrence Berkeley National Lab., Berkeley, CA, 94720, USA

    Norman K. Glendenning

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Lai, D. (2001). Neutron Star Kicks and Asymmetric Supernovae. In: Blaschke, D., Sedrakian, A., Glendenning, N.K. (eds) Physics of Neutron Star Interiors. Lecture Notes in Physics, vol 578. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-44578-1_15

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  • DOI: https://doi.org/10.1007/3-540-44578-1_15

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