Effects of Gravitational Correction on Neutrino Emission from Neutron Stars

Considering the gravitational correction through introduction of weakly interacting light vector U bosons, not only the equation of state （EoS） of the neutron star matter, but also the cooling properties of neutron stars may be changed. In this work, effects of gravitational correction on neutrino e...

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Bibliographic Details
Published inChinese physics letters Vol. 32; no. 5; pp. 178 - 182
Main Author 丁文波 鄂姗姗 喻孜 张齐 戚湛强
Format Journal Article
LanguageEnglish
Published Chinese Physical Society and IOP Publishing 01.05.2015
Subjects
Bosons
Cooling
Cooling effects
Gravitation
Gravitational effects
Neutrinos
Neutron stars
Stars
中子星物质
中微子
冷却性能
冷却速度
发射率
引力
排放
相对论平均场理论
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ISSN0256-307X
1741-3540
DOI10.1088/0256-307X/32/5/059701

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Summary:Considering the gravitational correction through introduction of weakly interacting light vector U bosons, not only the equation of state （EoS） of the neutron star matter, but also the cooling properties of neutron stars may be changed. In this work, effects of gravitational correction on neutrino emission and cooling of neutron stars in the matter with neutrons, protons, electrons, muons, △- and △0 are studied by the relativistic mean field theory and the related cooling theory. The results show that the effects are sensitive to the ratio of coupling strength to mass squared of U bosons, defined as gu. With increasing gu, the radial region where direct Urca process of nucleons can be allowed in a neutron star with the fixed mass becomes narrower, while the neutrino emissivity is somewhat higher. Moreover, the gravitational correction suppresses the effects of △- on neutrino emission. The gravitational correction leads the star to cool faster, and the higher the gu is, the faster the star cools.
Bibliography:11-1959/O4
DING Wen-Bo, E Shan-Shan, YU Zi,ZHANG Qi, QI Zhan-Qiang（ 1School of Mathematics and Physics, Bohai University, dinzhou 121000 2College of Science, Nanjing Forestry University, Nanjing 210037）
Considering the gravitational correction through introduction of weakly interacting light vector U bosons, not only the equation of state （EoS） of the neutron star matter, but also the cooling properties of neutron stars may be changed. In this work, effects of gravitational correction on neutrino emission and cooling of neutron stars in the matter with neutrons, protons, electrons, muons, △- and △0 are studied by the relativistic mean field theory and the related cooling theory. The results show that the effects are sensitive to the ratio of coupling strength to mass squared of U bosons, defined as gu. With increasing gu, the radial region where direct Urca process of nucleons can be allowed in a neutron star with the fixed mass becomes narrower, while the neutrino emissivity is somewhat higher. Moreover, the gravitational correction suppresses the effects of △- on neutrino emission. The gravitational correction leads the star to cool faster, and the higher the gu is, the faster the star cools.
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ISSN:0256-307X
1741-3540
DOI:10.1088/0256-307X/32/5/059701