Nuclear Equation of State and Neutron Star Structure

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The hadronic equation of state for a neutron star is discussed with a particular emphasis on the symmetry energy. The results of several microscopic approaches are compared and also a new calculation in terms of the self-consistent Green function method is presented. In addition possible constraints on the symmetry energy coming from empirical information from the neutron skin of finite nuclei are considered.
Invited talk presented at the Advanced Research Workshop on "Superdense QCD Matter and Compact Stars", Yerevan, Armenia, Sep 27 2003

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Nuclear Theory

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http://salesiana.dossiersoluciones.com/handle/123456789/82140

Consulte el texto completo en el siguiente enlace:

https://arxiv.org/abs/nucl-th/0312012
 http://arxiv.org/abs/nucl-th/0312012

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arXiv