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arXiv · 0901.4475

Nuclear Physics of Neutron Stars

J. Piekarewicz
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Abstract

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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J. Piekarewicz. 2009-01-28. Nuclear Physics of Neutron Stars. https://doi.org/10.1063/1.3146209

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