Nuclear Physics of Neutron Stars

Details Nuclear Physics of Neutron Stars Nuclear Physics of Neutron Stars

2009-01-28

arxiv.org/abs/0901.4475v1

AIP Conf.Proc.1128:144-153,2009

Physics

Nuclear Physics

Nuclear Theory

10 pages, 5 figures, Proceedings of the 5th FRIB Workshop on Bulk Nuclear Properties

Scientific paper

10.1063/1.3146209

Understanding the equation of state (EOS) of cold nuclear matter, namely, the relation between the pressure and energy density, is a central goal of nuclear physics that cuts across a variety of disciplines. Indeed, the limits of nuclear existence, the collision of heavy ions, the structure of neutron stars, and the dynamics of core-collapse supernova, all depend critically on the equation of state of hadronic matter. In this contribution I will concentrate on the special role that nuclear physics plays in constraining the EOS of cold baryonic matter and its impact on the properties of neutron stars.

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