Nuclear Physics of Neutron Stars
Nuclear Theory
2009-06-12 v1 Solar and Stellar Astrophysics
General Relativity and Quantum Cosmology
Nuclear Experiment
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.
Cite
@article{arxiv.0901.4475,
title = {Nuclear Physics of Neutron Stars},
author = {J. Piekarewicz},
journal= {arXiv preprint arXiv:0901.4475},
year = {2009}
}
Comments
10 pages, 5 figures, Proceedings of the 5th FRIB Workshop on Bulk Nuclear Properties