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能通过大质量中子星转动惯量来限定超子参数吗?

喻孜 丁文波 许妍 张贵清

喻孜, 丁文波, 许妍, 张贵清. 能通过大质量中子星转动惯量来限定超子参数吗?[J]. 原子核物理评论, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
引用本文: 喻孜, 丁文波, 许妍, 张贵清. 能通过大质量中子星转动惯量来限定超子参数吗?[J]. 原子核物理评论, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
YU Zi, DING Wenbo, XU Yan, ZHANG Guiqing. Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?[J]. Nuclear Physics Review, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
Citation: YU Zi, DING Wenbo, XU Yan, ZHANG Guiqing. Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?[J]. Nuclear Physics Review, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127

能通过大质量中子星转动惯量来限定超子参数吗?

doi: 10.11804/NuclPhysRev.35.02.127
基金项目: 国家自然科学基金资助项目(11265009,11175077,11271055);江苏省自然基金青年基金项目(Bk20140982)
详细信息
    作者简介:

    喻孜(1981-),男,湖北武汉人,博士,副教授,从事核天体物理研究;E-mail:ziyunjfu@163.com

    通讯作者: 丁文波,E-mail:dingwenbo1980@163.com
  • 中图分类号: O572.24

Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?

Funds: Natural Science Fundamental Research Project of Jiangsu Colleges and Universities (Bk20140982); National Natural Science Foundation of China (11265009, 11175077, 11271055)
  • 摘要: 在相对论平均场理论(RMFT)框架内,使用GL91参数组结合超核数据和大质量中子星的观测数据限定超子标量耦合参数Xσ=0.59~1.0,用慢转近似计算了大质量中子星和前中子星的转动惯量。当Xσ从0.59增加到1.0,中子星(前中子星)的最大转动惯量增幅达89%(60%)。在同样的变化范围内,用Crab的观测数据,计算得到中子星(前中子星)的最大能量损失(dE/dt)的增幅为44%(25%),最大磁场增幅为48%(38%)。相比于前中子星,中子星的性质对超子参数更为敏感。当Xσ从0.59增加到1.0,PSR J0348+0432的转动惯量和dE/dt的增幅均为14%,而磁场减幅为10%。如果天文观测能够给出中子星转动惯量的上限,或者同时精确测量中子星的质量和转动惯量,能帮助人们进一步限定超子参数。


    In the framework of the relativistic mean field theory(RMFT) with GL91 cets, the momentum of inertia (I) of slowly rotating neutron stars is studied by perturbative approach. The scalar hyperon coupling should lie in the range of Xσ=0.59~1.0 to be compatible with massive neutron stars. As Xσ increases from 0.59 to 1.0, the maximum momentum of inertia(Imax) of neutron (protoneutron) stars increases by 89% (60%). According to the data of Crab, the maximum energy loss(dE/dt) of neutron (protoneutron) stars will increase by 44%(25%)and the maximum magnetic field (B) will increase by 48%(38%). I and dE/dt of PSR J0348+0432 both increase by 14%, while B decreases by 10% as Xσ increases from 0.59 to 1.0. So if the upper bound of I, or the accurate values of both the mass and I of neutron stars could be provided by the astronomical observations, the hyperon couplings should be further constrained in the future.
  • [1] BETHE H A. Rev Mod Phys, 1990, 62:801.
    [2] GLENDENNING N K. Compact stars:Nuclear Physics, Particle Ph and General Relativity[M]. New York:Springer:1997:206.
    [3] DEMOREST P B, PENNUCCI T, RANSOM S M, et al. Nature, 2010, 467:1081.
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    [9] FATTOYEV F J, PIEKAREWICZ J. Phys Rev C, 2010, 82:025810.
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    [14] ZHAO Xianfeng, WANG Shunjing, ZHANG Hua, et al. Journal of Southwest University(Natural Science Edition), 2010, 32(7):46. (in Chinese) (赵先锋, 王顺金, 张华, 等. 西南大学学报(自然科学版), 2010, 32(7):46.)
    [15] ZHAO Xianfeng. Acta Astronomic Sinica, 2011, 52(2):126. (in Chinese) (赵先锋. 天文学报, 2011, 52(2):126.)
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出版历程
  • 收稿日期:  2018-04-20
  • 修回日期:  2018-05-26
  • 刊出日期:  2018-06-20

能通过大质量中子星转动惯量来限定超子参数吗?

doi: 10.11804/NuclPhysRev.35.02.127
    基金项目:  国家自然科学基金资助项目(11265009,11175077,11271055);江苏省自然基金青年基金项目(Bk20140982)
    作者简介:

    喻孜(1981-),男,湖北武汉人,博士,副教授,从事核天体物理研究;E-mail:ziyunjfu@163.com

    通讯作者: 丁文波,E-mail:dingwenbo1980@163.com
  • 中图分类号: O572.24

摘要: 在相对论平均场理论(RMFT)框架内,使用GL91参数组结合超核数据和大质量中子星的观测数据限定超子标量耦合参数Xσ=0.59~1.0,用慢转近似计算了大质量中子星和前中子星的转动惯量。当Xσ从0.59增加到1.0,中子星(前中子星)的最大转动惯量增幅达89%(60%)。在同样的变化范围内,用Crab的观测数据,计算得到中子星(前中子星)的最大能量损失(dE/dt)的增幅为44%(25%),最大磁场增幅为48%(38%)。相比于前中子星,中子星的性质对超子参数更为敏感。当Xσ从0.59增加到1.0,PSR J0348+0432的转动惯量和dE/dt的增幅均为14%,而磁场减幅为10%。如果天文观测能够给出中子星转动惯量的上限,或者同时精确测量中子星的质量和转动惯量,能帮助人们进一步限定超子参数。


In the framework of the relativistic mean field theory(RMFT) with GL91 cets, the momentum of inertia (I) of slowly rotating neutron stars is studied by perturbative approach. The scalar hyperon coupling should lie in the range of Xσ=0.59~1.0 to be compatible with massive neutron stars. As Xσ increases from 0.59 to 1.0, the maximum momentum of inertia(Imax) of neutron (protoneutron) stars increases by 89% (60%). According to the data of Crab, the maximum energy loss(dE/dt) of neutron (protoneutron) stars will increase by 44%(25%)and the maximum magnetic field (B) will increase by 48%(38%). I and dE/dt of PSR J0348+0432 both increase by 14%, while B decreases by 10% as Xσ increases from 0.59 to 1.0. So if the upper bound of I, or the accurate values of both the mass and I of neutron stars could be provided by the astronomical observations, the hyperon couplings should be further constrained in the future.

English Abstract

喻孜, 丁文波, 许妍, 张贵清. 能通过大质量中子星转动惯量来限定超子参数吗?[J]. 原子核物理评论, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
引用本文: 喻孜, 丁文波, 许妍, 张贵清. 能通过大质量中子星转动惯量来限定超子参数吗?[J]. 原子核物理评论, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
YU Zi, DING Wenbo, XU Yan, ZHANG Guiqing. Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?[J]. Nuclear Physics Review, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
Citation: YU Zi, DING Wenbo, XU Yan, ZHANG Guiqing. Can the Moment of Inertia of Massive Neutron Stars be Used to Constrain the Hyperon Couplings?[J]. Nuclear Physics Review, 2018, 35(2): 127-132. doi: 10.11804/NuclPhysRev.35.02.127
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