TL;DR
This paper explores the nuclear equation of state for neutron-rich matter, emphasizing its significance in understanding neutron stars and supernovae, and discusses how laboratory experiments inform this understanding.
Contribution
It highlights the role of laboratory measurements of neutron skins and nuclear resonances in constraining the neutron star equation of state.
Findings
Laboratory experiments provide insights into neutron star structure.
Neutron skins and nuclear resonances are key to understanding dense matter.
EOS impacts neutron star composition and dynamics.
Abstract
Understanding the equation of state (EOS) of neutron-rich matter is a central goal of nuclear physics that cuts across a variety of disciplines. Indeed, the limits of nuclear existence, the collision of energetic heavy ions, the structure of neutron stars, and the dynamics of core-collapse supernova all depend critically on the nuclear-matter EOS. In this contribution I focus on the EOS of cold baryonic matter with special emphasis on its impact on the structure, dynamics, and composition of neutron stars. In particular, I discuss how laboratory experiments on neutron skins as well as on Pygmy and Giant resonances can help us elucidate the structure of these fascinating objects.
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