Nuclear Equation of State and Neutron Star Structure

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dc.creatorDieperink, A. E. L.
dc.creatorVan Neck, D.
dc.creatorDewulf, Y.
dc.creatorRodin, V.
dc.date2003-12-03
dc.date.accessioned2026-07-07T05:40:02Z
dc.date.available2026-07-07T05:40:02Z
dc.descriptionThe 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.
dc.descriptionInvited talk presented at the Advanced Research Workshop on "Superdense QCD Matter and Compact Stars", Yerevan, Armenia, Sep 27 2003
dc.identifierhttps://arxiv.org/abs/nucl-th/0312012
dc.identifierhttp://arxiv.org/abs/nucl-th/0312012
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/82140
dc.subjectNuclear Theory
dc.titleNuclear Equation of State and Neutron Star Structure
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