TL;DR
This paper reviews how nuclear physics constrains the equation of state of cold nuclear matter, which is crucial for understanding neutron star properties and related astrophysical phenomena.
Contribution
It highlights the role of nuclear physics in constraining the EOS of cold baryonic matter and its implications for neutron star characteristics.
Findings
Nuclear physics provides key constraints on the EOS of cold nuclear matter.
The EOS influences neutron star structure and behavior.
Understanding the EOS aids in interpreting astrophysical observations.
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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