DC pole | Wartość | Język |
dc.contributor.author | Bednarek, Ilona | - |
dc.contributor.author | Sładkowski, Jan | - |
dc.contributor.author | Syska, Jacek | - |
dc.date.accessioned | 2020-06-02T09:49:26Z | - |
dc.date.available | 2020-06-02T09:49:26Z | - |
dc.date.issued | 2020 | - |
dc.identifier.citation | "Symmetry" Vol. 12, iss. 6, art. 898 (2020), s. 1-22 | pl_PL |
dc.identifier.issn | 2073-8994 | - |
dc.identifier.uri | http://hdl.handle.net/20.500.12128/14359 | - |
dc.description.abstract | The symmetry energy is an invaluable tool for studying dense nuclearmatter. Unfortunately,
its definition is somewhat implicit, and therefore, phenomenologicalmethods are necessary to describe
experimental facts. This paper discusses the differences arising from the use of Taylor series
expansion and Padé approximation to determine theoretically the symmetry energy and the possible
consequences for neutron stars. For this purpose, a form of the nuclear matter equation of state that
explicitly depends on the symmetry energy is used. The obtained results point out that the applied
approximations lead to modifications of the equilibrium proton fractions and equation of state,
especially in their high-density limit. However, this effect is small near the saturation density n0. | 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 | symmetry energy | pl_PL |
dc.subject | neutron star | pl_PL |
dc.subject | dense nuclear matter | pl_PL |
dc.subject | Padé approximation | pl_PL |
dc.title | Forms of the symmetry energy relevant to neutron stars | pl_PL |
dc.type | info:eu-repo/semantics/article | pl_PL |
dc.identifier.doi | 10.3390/sym12060898 | - |
Pojawia się w kolekcji: | Artykuły (WNŚiT)
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