R-mode Instability of Neutron Star with Non-Newtonian Gravity
R-mode Instability of Neutron Star with Non-Newtonian Gravity
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DOI：
10.1088/0253-6102/59/1/10
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发表时间：
2013-01
影响因子：
3.1
通讯作者：
Jielu Yan;Dehua Wen
中科院分区：
文献类型：
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作者：
Jielu Yan;Dehua Wen
利用具有超软对称能量的非对称核物质状态方程，考虑了大统一理论中提出的非牛顿引力，研究了具有刚性壳的正则中子星（1.4 M ~（12））r模的CFS不稳定性.在中子星质量和自旋频率观测的约束下，得到了正则中子星星r模不稳定性窗口的边界，结果表明，观测到的中子星都在不稳定性窗口之外，这与理论预期一致.此外，还给出了非牛顿重力参数的一个上限。
The Chandrasekhar—Friedmann—Schutz (CFS) instabilities of r-modes for canonical neutron stars (1.4 M⊙) with rigid crusts are investigated by using an equation of state of asymmetric nuclear matter with super-soft symmetry energy, where the non-Newtonian gravity proposed in the grand unification theories is also considered. Constrained by the observations of the masses and the spin frequencies for neutron stars, the boundary of the r-mode instability window for a canonical neutron star is obtained, and the results show that the observed neutron stars are all outside the instability window, which is consistent with the theoretical expectation. In addition, an upper limit of the non-Newtonian gravity parameters is also given.