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Article: Constraints on the symmetry energy and neutron skins from experiments and theory

TitleConstraints on the symmetry energy and neutron skins from experiments and theory
Authors
Issue Date2012
Citation
Physical Review C - Nuclear Physics, 2012, v. 86, n. 1 How to Cite?
AbstractThe symmetry energy contribution to the nuclear equation of state impacts various phenomena in nuclear astrophysics, nuclear structure, and nuclear reactions. Its determination is a key objective of contemporary nuclear physics, with consequences for the understanding of dense matter within neutron stars. We examine the results of laboratory experiments that have provided initial constraints on the nuclear symmetry energy and on its density dependence at and somewhat below normal nuclear matter density. Even though some of these constraints have been derived from properties of nuclei while others have been derived from the nuclear response to electroweak and hadronic probes, within experimental uncertainties-they are consistent with each other. We also examine the most frequently used theoretical models that predict the symmetry energy and its slope parameter. By comparing existing constraints on the symmetry pressure to theories, we demonstrate how contributions of three-body forces, which are essential ingredients in neutron matter models, can be determined. © 2012 American Physical Society.
Persistent Identifierhttp://hdl.handle.net/10722/200105
ISSN
2014 Impact Factor: 3.733
2015 SCImago Journal Rankings: 1.601
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorTsang, Betty-
dc.contributor.authorStone, Jiřina Říkovská-
dc.contributor.authorCamera, Franco-
dc.contributor.authorDanielewicz, Paweł-
dc.contributor.authorGandolfi, Stefano-
dc.contributor.authorHebeler, Kai-
dc.contributor.authorHorowitz, Charles J.-
dc.contributor.authorLee, Jenny-
dc.contributor.authorLynch, William G.-
dc.contributor.authorKohley, Zach-
dc.contributor.authorLemmon, Roy C.-
dc.contributor.authorMöller, P.-
dc.contributor.authorMurakami, Tetsuya-
dc.contributor.authorRiordan, S.-
dc.contributor.authorRoca-Maza, Xavier-
dc.contributor.authorSammarruca, Francesca-
dc.contributor.authorSteiner, Andrew W.-
dc.contributor.authorVidaña, Isaac-
dc.contributor.authorYennello, Sherry J.-
dc.date.accessioned2014-07-26T23:11:08Z-
dc.date.available2014-07-26T23:11:08Z-
dc.date.issued2012-
dc.identifier.citationPhysical Review C - Nuclear Physics, 2012, v. 86, n. 1-
dc.identifier.issn0556-2813-
dc.identifier.urihttp://hdl.handle.net/10722/200105-
dc.description.abstractThe symmetry energy contribution to the nuclear equation of state impacts various phenomena in nuclear astrophysics, nuclear structure, and nuclear reactions. Its determination is a key objective of contemporary nuclear physics, with consequences for the understanding of dense matter within neutron stars. We examine the results of laboratory experiments that have provided initial constraints on the nuclear symmetry energy and on its density dependence at and somewhat below normal nuclear matter density. Even though some of these constraints have been derived from properties of nuclei while others have been derived from the nuclear response to electroweak and hadronic probes, within experimental uncertainties-they are consistent with each other. We also examine the most frequently used theoretical models that predict the symmetry energy and its slope parameter. By comparing existing constraints on the symmetry pressure to theories, we demonstrate how contributions of three-body forces, which are essential ingredients in neutron matter models, can be determined. © 2012 American Physical Society.-
dc.languageeng-
dc.relation.ispartofPhysical Review C - Nuclear Physics-
dc.titleConstraints on the symmetry energy and neutron skins from experiments and theory-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1103/PhysRevC.86.015803-
dc.identifier.scopuseid_2-s2.0-84864407347-
dc.identifier.volume86-
dc.identifier.issue1-
dc.identifier.eissn1089-490X-
dc.identifier.isiWOS:000306190600007-

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