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Effects of the equation of state on the bulk properties of maximally rotating neutron stars

机译：状态方程对最大旋转中子恒星散装性能的影响

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摘要

Neutron stars are among the densest known objects in the universe and an ideal laboratory for the strange physics of supercondensed matter. While the simultaneous measurements of mass and radius of nonrotating neutron stars may impose constraints on the properties of the dense nuclear matter, the observation and study of maximally rotating ones, close to the mass-shedding limit, may lead to significantly further constraints. Theoretical predictions allow neutron stars to rotate extremely fast (even more than 2000 Hz). However, until this moment, the fastest observed rotating pulsar has a frequency of 716 Hz, much lower compared to the theoretical predictions. There are many suggestions for the mechanism which lead to this situation. In any case, the theoretical study of uniformly rotating neutron stars, along with accurate measurements, may offer rich information concerning the high-density part of the equation of state. In addition, neutron stars through their evolution may provide us with a criterion to determine the final fate of a rotating compact star. Sensitivity of bulk neutron stars properties on the equation of state at the mass-shedding limit are the main subject of the present study.
机译：中子恒星是宇宙中最密集的已知物体之一，是一个理想的实验室，适用于超级致密物质的奇怪物理学。虽然非调节中子恒星的质量和半径的同时测量可能对致密核物质的性质进行限制，但最大旋转的物质的性质，接近质量脱落限制可能导致显着进一步的约束。理论预测允许中子恒星旋转极快（甚至超过2000 Hz）。然而，直到这一刻，与理论预测相比，最快观察到的旋转脉冲条件具有716Hz的频率，远低得多。导致这种情况的机制有很多建议。在任何情况下，均匀旋转中子恒星以及精确测量的理论研究可以提供关于状态方程的高密度部分的丰富信息。此外，中子恒星通过它们的进化可以为我们提供标准，以确定旋转紧凑型恒星的最终命运。散装中子恒星特性对大规模脱落极限的状态方程的敏感性是本研究的主要主题。

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