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Analytic I-Love-C relations for realistic neutron stars

机译:现实中子星的解析I-Love-C关系

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Recent observations of neutron stars with radio, x rays, and gravitational waves have begun to constrain the equation of state for nuclear matter beyond the nuclear saturation density. To one's surprise, there exist approximate universal relations connecting certain bulk properties of neutron stars that are insensitive to the underlying equation of state and having important applications on probing fundamental physics including nuclear and gravitational physics. To date, analytic works on universal relations for realistic neutron stars are lacking, which may lead to a better understanding of the origin of the universality. Here, we focus on the universal relations between the compactness (C), the moment of inertia (I), and the tidal deformability (related to the Love number) and derive analytic, approximate I-Love-C relations. To achieve this, we construct slowly rotating and tidally deformed neutron star solutions analytically starting from an extended Tolman VII model that accurately describes nonrotating realistic neutron stars, which allows us to extract the moment of inertia and the tidal deformability on top of the compactness. We solve the field equations analytically by expanding them about the Newtonian limit and keeping up to sixth order in the stellar compactness. Based on these analytic solutions, we can mathematically demonstrate the O(10) equationof- state variation in the I-C and Love-C relations and the O(1) variation in the I-Love relation that have previously been found numerically. Our new analytic relations agree more accurately with numerical results for realistic neutron stars (especially the I-C and Love-C ones) than the analytic relations for constant-density stars derived in previous work. Based on these analytic findings, we attribute a possible origin of the universality for the I-C and Love-C relations to the fact that the energy density of realistic neutron stars can be approximated as a quadratic function, as is the case for the Tolma
机译:最近用无线电、X射线和引力波对中子星的观测已经开始限制核物质超出核饱和密度的状态方程。令人惊讶的是,存在着近似的普遍关系,将中子星的某些体性联系起来,这些中子星对潜在的状态方程不敏感,并且在探测基础物理学(包括核物理学和引力物理学)方面具有重要应用。迄今为止,缺乏关于现实中子星普遍关系的分析工作,这可能会导致对普遍性起源的更好理解。在这里,我们关注紧致性(C)、转动惯量(I)和潮汐变形率(与Love数有关)之间的普遍关系,并推导出解析的近似I-Love-C关系。为了实现这一点,我们从扩展的Tolman VII模型开始,分析构建了缓慢旋转和潮汐变形的中子星解决方案,该模型准确地描述了非旋转的现实中子星,这使我们能够在致密性的基础上提取转动惯量和潮汐变形性。我们通过将场方程扩展为牛顿极限并保持恒星致密度的六阶来解析求解场方程。基于这些解析解,我们可以用数学方法证明 I-C 和 Love-C 关系中的 O(10%) 状态方程变化以及 I-Love 关系中的 O(1%) 变化,这些变化之前已经通过数值方式发现。我们的新解析关系与现实中子星(尤其是I-C和Love-C中子星)的数值结果比之前工作中推导的恒定密度恒星的解析关系更精确。基于这些分析结果,我们将I-C和Love-C关系的普遍性的可能起源归因于这样一个事实,即现实中子星的能量密度可以近似为二次函数,就像托尔马的情况一样

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