Constraint on nuclear symmetry energy imposed by f-mode oscillation of neutron stars
Constraint on nuclear symmetry energy imposed by f-mode oscillation of neutron stars
复制标题
中子星f模振荡对核对称能的约束
DOI：
10.1088/1572-9494/ac1669
复制
发表时间：
2021
影响因子：
3.1
通讯作者：
Yuxi Li
中科院分区：
文献类型：
--
作者：
Jing Zhang;Dehua Wen;Yuxi Li
由于引力波探测器灵敏度的提高，对中子星基准简正模引力波的探测成为可能。未来对中子星f模引力波的探测将为我们进一步了解中子星内部核物质的性质提供一个潜在的途径。在这项工作中，我们研究了中子星的f-模振荡对核物质的对称性能量的约束，使用贝叶斯分析和参数EOS。结果表明，如果精确观测已知质量的中子星星的f模频率，核物质饱和密度2倍处的对称能（Esym（2ρ 0））可以被限制在一个较窄的范围内.例如，当以下所有参数都在给定区间内时：220 ≤ K 0 ≤ 260 MeV，28 ≤ E sym（ρ 0）≤ 36 MeV，30 ≤ L ≤ 90 MeV，−800 ≤ J 0 ≤ 400 MeV，− 400 ≤ K sym ≤ 100 MeV，−200 ≤ J sym ≤ 800 MeV，如果观测到正则中子星星（1.4 M⊙）的f模频率为1.720 kHz（相对误差为1%），则E sym（2ρ 0）将被限制在48.8 - 5.5+6.6 MeV范围内。此外，如果只有f模式频率检测可用，即没有恒星质量测量，精确检测的f模式频率也可以对对称能量施加精确的约束。例如，给定相同的参数空间和相同的假设观测到的f模频率，并假设恒星质量在1.2-2.0兆电子伏特的范围内，E sym（2ρ 0）将被限制在49.5−6.8+ 8.1兆电子伏特的范围内。此外，还表明69 ≤ L ≤ 143 MeV的较高斜率将给出E sym（2ρ 0）的较高后验分布，53.8−6.4+ 7.0 MeV。
Due to improvements in the sensitivity of gravitational wave (GW) detectors, the detection of GWs originating from the fundamental quasi-normal mode (f-mode) of neutron stars has become possible. The future detection of GWs originating from the f-mode of neutron stars will provide a potential way to improve our understanding of the nature of nuclear matter inside neutron stars. In this work, we investigate the constraint imposed by the f-mode oscillation of neutron stars on the symmetry energy of nuclear matter using Bayesian analysis and parametric EOS. It is shown that if the frequency of the f-mode of a neutron star of known mass is observed precisely, the symmetry energy at twice the saturation density (E sym(2ρ 0)) of nuclear matter can be constrained within a relatively narrow range. For example, when all the following parameters are within the given intervals: 220 ≤ K 0 ≤ 260 MeV, 28 ≤ E sym(ρ 0) ≤ 36 MeV, 30 ≤ L ≤ 90 MeV, −800 ≤ J 0 ≤ 400 MeV, − 400 ≤ K sym ≤ 100 MeV, −200 ≤ J sym ≤ 800 MeV, E sym(2ρ 0) will be constrained to within 48.8−5.5+6.6 MeV if the f-mode frequency of a canonical neutron star (1.4 M⊙) is observed to be 1.720 kHz with a 1% relative error. Furthermore, if only f-mode frequency detection is available, i.e. there is no stellar mass measurement, a precisely detected f-mode frequency can also impose an accurate constraint on the symmetry energy. For example, given the same parameter space and the same assumed observed f-mode frequency mentioned above, and assuming that the stellar mass is in the range of 1.2–2.0 M⊙, E sym(2ρ 0) will be constrained to within 49.5−6.8+8.1MeV . In addition, it is shown that a higher slope of 69 ≤ L ≤ 143 MeV will give a higher posterior distribution of E sym(2ρ 0), 53.8−6.4+7.0MeV .