Neutron star cooling in various sets of nucleon coupling constants

The influences of nucleon coupling constants on the neutrino scatting and cooling properties of neutron stars are investigated. The results in the GM1, GPS250 and NL-SH parameter sets show that the magnitude of the neutrino emissivity and density ranges where the dUrca process of nucleons is allowed...

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Bibliographic Details
Published inChinese physics C Vol. 37; no. 5; pp. 35 - 40
Main Author 丁文波 喻孜 密更 王春艳
Format Journal Article
LanguageEnglish
Published 01.05.2013
Subjects
Constants
Cooling
Density
Emissivity
Joining
Neutrinos
Neutron stars
Nucleons
中子星
中微子
冷却性能
冷却速度
密度范围
核子
状态方程
耦合常数
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Summary:The influences of nucleon coupling constants on the neutrino scatting and cooling properties of neutron stars are investigated. The results in the GM1, GPS250 and NL-SH parameter sets show that the magnitude of the neutrino emissivity and density ranges where the dUrca process of nucleons is allowed differ obviously between the three parameter sets in nucleon-only and hyperonic matter. Furthermore, the neutron stars in the CPS250 set cool very quickly, whereas those in the NL-SH set cool slowly. The cooling rate of the former can be almost three times more that of the latter. It can be concluded that the stiffer the equation of state, the slower the corresponding neutron stars cool. The hyperon A makes neutrino emissivity due to the direct Urca process of nucleons lower compared with nucleon-only matter, and postpones the dUrca process with muons. However, these A effects are relatively weaker in the GPS250 set than in the GM1 set.
Bibliography:The influences of nucleon coupling constants on the neutrino scatting and cooling properties of neutron stars are investigated. The results in the GM1, GPS250 and NL-SH parameter sets show that the magnitude of the neutrino emissivity and density ranges where the dUrca process of nucleons is allowed differ obviously between the three parameter sets in nucleon-only and hyperonic matter. Furthermore, the neutron stars in the CPS250 set cool very quickly, whereas those in the NL-SH set cool slowly. The cooling rate of the former can be almost three times more that of the latter. It can be concluded that the stiffer the equation of state, the slower the corresponding neutron stars cool. The hyperon A makes neutrino emissivity due to the direct Urca process of nucleons lower compared with nucleon-only matter, and postpones the dUrca process with muons. However, these A effects are relatively weaker in the GPS250 set than in the GM1 set.
nucleon coupling constants, cooling, neutron stars
11-5641/O4
ObjectType-Article-2
SourceType-Scholarly Journals-1
ObjectType-Feature-1
content type line 23
ISSN:1674-1137
0254-3052
DOI:10.1088/1674-1137/37/5/055101