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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| Published in | Chinese physics letters Vol. 32; no. 5; pp. 178 - 182 |
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| Main Author | |
| Format | Journal Article |
| Language | English |
| Published |
Chinese Physical Society and IOP Publishing
01.05.2015
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| Subjects | |
| Online Access | Get full text |
| ISSN | 0256-307X 1741-3540 |
| DOI | 10.1088/0256-307X/32/5/059701 |
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| Abstract | 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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| AbstractList | 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, [Delta]- and [Delta] super(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 g sub(U). With increasing g sub(U), 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 [Delta]- on neutrino emission. The gravitational correction leads the star to cool faster, and the higher the g sub(U) is, the faster the star cools. 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. 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, Δ− and Δ0 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 Δ− on neutrino emission. The gravitational correction leads the star to cool faster, and the higher the gU is, the faster the star cools. |
| Author | 丁文波 鄂姗姗 喻孜 张齐 戚湛强 |
| AuthorAffiliation | School of Mathematics and Physics, Bohai University, Jinzhou 121000 College of Science, Nanjing Forestry University, Nanjing 210037 |
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| Cites_doi | 10.1103/PhysRevLett.105.231103 10.1111/j.1365-2966.2005.09214.x 10.1088/0256-307X/25/2/029 10.1103/PhysRevLett.103.211102 10.1038/nature09466 10.1103/PhysRevA.83.035801 10.1038/nature04858 10.1103/PhysRevLett.66.2701 10.1103/PhysRevLett.105.101101 10.1038/421899a |
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| Copyright | 2015 Chinese Physical Society and IOP Publishing Ltd |
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| DocumentTitleAlternate | Effects of Gravitational Correction on Neutrino Emission from Neutron Stars |
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| Notes | 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. ObjectType-Article-1 SourceType-Scholarly Journals-1 ObjectType-Feature-2 content type line 23 |
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| References | 11 Fujii Y (14) 1971; 234 15 16 17 Fayet P (1) 2010; 81 Zhu S H (2) 2007; 75 Krivoruchenko M I (8) 2009; 79 Zheng H (10) 2012; 85 Ding W B (12) 2008; 25 3 Ding W B (13) 2012; 29 5 6 7 9 DeDeo S (4) 2008; 78 |
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| Snippet | Considering the gravitational correction through introduction of weakly interacting light vector U bosons, not only the equation of state （EoS） of the... Considering the gravitational correction through introduction of weakly interacting light vector U bosons, not only the equation of state (EoS) of the neutron... |
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| SubjectTerms | 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 |
| Title | Effects of Gravitational Correction on Neutrino Emission from Neutron Stars |
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