Forms of the Symmetry Energy Relevant to Neutron Stars

Forms of the Symmetry Energy Relevant to Neutron Stars

The symmetry energy is an invaluable tool for studying dense nuclear matter. Unfortunately, its definition is somewhat implicit, and therefore, phenomenological methods are necessary to describe experimental facts. This paper discusses the differences arising from the use of Taylor series expansion...

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Main Authors: Ilona Bednarek, Jan Sładkowski, Jacek Syska
Format: Article
Language:English
Published: MDPI AG 2020-06-01
Series:Symmetry
Subjects:
symmetry energy
neutron star
dense nuclear matter
Padé approximation
Online Access:https://www.mdpi.com/2073-8994/12/6/898
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spelling doaj-5c532acfdb594d84b64ee3677727528d2020-11-25T02:51:54ZengMDPI AGSymmetry2073-89942020-06-011289889810.3390/sym12060898Forms of the Symmetry Energy Relevant to Neutron StarsIlona Bednarek0Jan Sładkowski1Jacek Syska2Institute of Physics, University of Silesia, 75 Pułku Piechoty 1, Pl 41-500 Chorzów, PolandInstitute of Physics, University of Silesia, 75 Pułku Piechoty 1, Pl 41-500 Chorzów, PolandInstitute of Physics, University of Silesia, 75 Pułku Piechoty 1, Pl 41-500 Chorzów, PolandThe symmetry energy is an invaluable tool for studying dense nuclear matter. Unfortunately, its definition is somewhat implicit, and therefore, phenomenological methods 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 <inline-formula> <math display="inline"> <semantics> <msub> <mi>n</mi> <mn>0</mn> </msub> </semantics> </math> </inline-formula>.https://www.mdpi.com/2073-8994/12/6/898symmetry energyneutron stardense nuclear matterPadé approximation
collection DOAJ
language English
format Article
sources DOAJ
author Ilona Bednarek
Jan Sładkowski
Jacek Syska
spellingShingle Ilona Bednarek
Jan Sładkowski
Jacek Syska
Forms of the Symmetry Energy Relevant to Neutron Stars
Symmetry
symmetry energy
neutron star
dense nuclear matter
Padé approximation
author_facet Ilona Bednarek
Jan Sładkowski
Jacek Syska
author_sort Ilona Bednarek
title Forms of the Symmetry Energy Relevant to Neutron Stars
title_short Forms of the Symmetry Energy Relevant to Neutron Stars
title_full Forms of the Symmetry Energy Relevant to Neutron Stars
title_fullStr Forms of the Symmetry Energy Relevant to Neutron Stars
title_full_unstemmed Forms of the Symmetry Energy Relevant to Neutron Stars
title_sort forms of the symmetry energy relevant to neutron stars
publisher MDPI AG
series Symmetry
issn 2073-8994
publishDate 2020-06-01
description The symmetry energy is an invaluable tool for studying dense nuclear matter. Unfortunately, its definition is somewhat implicit, and therefore, phenomenological methods 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 <inline-formula> <math display="inline"> <semantics> <msub> <mi>n</mi> <mn>0</mn> </msub> </semantics> </math> </inline-formula>.
topic symmetry energy
neutron star
dense nuclear matter
Padé approximation
url https://www.mdpi.com/2073-8994/12/6/898
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AT jansładkowski formsofthesymmetryenergyrelevanttoneutronstars
AT jaceksyska formsofthesymmetryenergyrelevanttoneutronstars
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