Nuclear Physics of Neutron Stars Export

@article{citeulike:3991494, 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.}, archivePrefix = {arXiv}, author = {Piekarewicz, J.}, citeulike-article-id = {3991494}, citeulike-linkout-0 = {http://arxiv.org/abs/0901.4475}, citeulike-linkout-1 = {http://arxiv.org/pdf/0901.4475}, day = {28}, eprint = {0901.4475}, keywords = {neutron, star}, month = {Jan}, posted-at = {2009-02-05 15:41:54}, priority = {2}, title = {Nuclear Physics of Neutron Stars}, url = {http://arxiv.org/abs/0901.4475}, year = {2009} }

TY - JOUR ID - citeulike:3991494 L3 - citeulike-article-id:3991494 N2 - 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. TI - Nuclear Physics of Neutron Stars KW - neutron KW - star AU - Piekarewicz, J PY - 2009/Jan/28/ UR - http://arxiv.org/abs/0901.4475 ER -