DC pole | Wartość | Język |
dc.contributor.author | Bednarek, Ilona | - |
dc.contributor.author | Pieńkos, Monika | - |
dc.date.accessioned | 2018-11-20T07:34:12Z | - |
dc.date.available | 2018-11-20T07:34:12Z | - |
dc.date.issued | 2011 | - |
dc.identifier.citation | Acta Physica Polonica B, Vol. 42, no. 11 (2011), s. 2211-2219 | pl_PL |
dc.identifier.issn | 0587-4254 | - |
dc.identifier.uri | http://hdl.handle.net/20.500.12128/7120 | - |
dc.description.abstract | Information about many aspects of both nuclear physics and a neutron star structure are encoded in the density dependence of the symmetry energy. Despite the fact that considerable progress has been made in constraining
the density dependence of the symmetry energy, it is still the most uncertain part of the asymmetric nuclear matter equation of state (EOS). The analysis of neutron star parameters which are most sensitive to the
form of the symmetry energy in the case of nucleon and strangeness-rich matter has been done with the use of the relativistic mean field (RMF) approximation. The mixed vector meson interactions have been introduced
to modify the density dependence of the symmetry energy. | pl_PL |
dc.language.iso | en | pl_PL |
dc.rights | Uznanie autorstwa 3.0 Polska | * |
dc.rights.uri | http://creativecommons.org/licenses/by/3.0/pl/ | * |
dc.subject | gwiazdy neutronowe | pl_PL |
dc.subject | astofizyka jądrowa | pl_PL |
dc.title | Symmetry Energy and Neutron Star Equation of State | pl_PL |
dc.type | info:eu-repo/semantics/article | pl_PL |
dc.identifier.doi | 10.5506/APhysPolB.42.2211 | - |
Pojawia się w kolekcji: | Artykuły (WNŚiT)
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