Spectral Approach to the Relativistic Inverse Stellar Structure Problem II
Spectral Approach to the Relativistic Inverse Stellar Structure Problem II
复制标题
相对论逆恒星结构问题II的谱法
DOI：
10.1103/physrevd.89.064003
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发表时间：
2013
影响因子：
5
通讯作者：
Nathaniel M. Indik
中科院分区：
文献类型：
--
作者：
Lee Lindblom;Nathaniel M. Indik
恒星结构逆问题是根据恒星的宏观观测量（如质量和半径）来确定恒星中物质的状态方程。这个问题在以前的论文中解决了通过构建一个光谱表示的状态方程，其恒星模型匹配一组规定的宏观观测值。本文在两个方面改进和扩展了这项工作：i）通过考虑这项工作中使用的状态方程的基于焓的表示的意外特征，使该方法更加鲁棒。在进行适当的修改后，不再需要对光谱参数进行精确的初始猜测，因此现在可以使用蒙特-卡罗技术来确保与观测值的最佳拟合。ii）该方法在这里被扩展为使用质量和潮汐形变率（将通过中子星合并的引力波观测来测量）作为宏观可观测量，而不是质量和半径。本文使用基于34种不同的高密度中子-恒星状态方程理论模型的恒星观测数据对这种扩展的、更鲁棒的谱方法的精度和可靠性进行了评估。与早期工作的定性一致，这些测试表明，中子星状态方程的高密度部分可以在百分之几的精度水平上确定，只需使用两个或三个中子星的质量和半径（或质量和潮汐形变）的高质量测量。
The inverse stellar structure problem determines the equation of state of the matter in stars from a knowledge of their macroscopic observables (e.g. their masses and radii). This problem was solved in a previous paper by constructing a spectral representation of the equation of state whose stellar models match a prescribed set of macroscopic observables. This paper improves and extends that work in two significant ways: i) The method is made more robust by accounting for an unexpected feature of the enthalpy based representations of the equations of state used in this work. After making the appropriate modifications, accurate initial guesses for the spectral parameters are no longer needed so Monte-Carlo techniques can now be used to ensure the best fit to the observables. ii) The method is extended here to use masses and tidal deformabilities (which will be measured by gravitational wave observations of neutron-star mergers) as the macroscopic observables instead of masses and radii. The accuracy and reliability of this extended and more robust spectral method is evaluated in this paper using mock data for observables from stars based on 34 different theoretical models of the high density neutron-star equation of state. In qualitative agreement with earlier work, these tests suggest the high density part of the neutron-star equation of state could be determined at the few-percent accuracy level using high quality measurements of the masses and radii (or masses and tidal deformabilities) of just two or three neutron stars.