温度依赖的奇异物质的出现使新生中子星旋转更快
Temperature dependent appearance of exotic matter makes nascent neutron stars spin faster
摘要：
中子星提供了研究物质在地球实验无法达到的密度和温度下的行为的机会。对中子星合并双星的引力波观测可以约束合并前后的中子星状态方程。在中子星双星合并后，超子可以在残余物中形成，改变中子星状态方程的行为。在这项研究中，我们使用有限熵的状态方程来表明，合并后的残留物可以旋转起来，由于冷却。上旋的大小取决于中子星状态方程。如果超子存在，当每个重子的熵从$s=2$ $k_B$下降到$s=0$ $k_B$时，合并后的自旋上升会使峰值引力波频率改变$\sim 540$ Hz。如果不存在超子，合并后的自旋上升会改变$\sim 360$ Hz，为奇异物质提供引力波信号。我们期望在触发温度依赖性相变时具有相同的定性行为。
英文摘要：
Neutron stars offer the opportunity to study the behaviour of matter at densities and temperatures inaccessible to terrestrial experiments. Gravitational-wave observations of binary neutron star coalescences can constrain the neutron-star equation of state before and after merger. After the neutron star binary merges, hyperons can form in the remnant, changing the behaviour of the neutron-star equation of state. In this study, we use finite-entropy equations of state to show that a post-merger remnant can spin up due to cooling. The magnitude of the spin-up depends on the neutron-star equation of state. If hyperons are present, the post-merger spin-up changes the peak gravitational-wave frequency by $\sim 540$ Hz, when the entropy per baryon drops from $s=2$ $k_B$ to $s=0$ $k_B$. If hyperons are not present, the post-merger spin-up changes by $\sim 360$ Hz, providing a gravitational-wave signature for exotic matter. We expect the same qualitative behaviour whenever temperature dependent phase transitions are triggered.
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