区分中子星中的尖锐和平滑相变
Differentiating between sharp and smoother phase transitions in neutron stars
摘要：
中子星的内部组成在天体物理学中仍然是一个悬而未决的问题。它们最里面的区域不受光传播的影响，而引力波大多携带恒星的全局特征，这意味着只能间接推断它们的内部。在这里，我们假设一个假设的未来的情况下，由于相变的状态方程软化被确定和估计的观测精度区分尖锐的相变从一个平滑的（与混合相/状态，由于致密物质的表面张力的未知值）在一个区域的混合星通过一些电磁和引力波观测。我们发现，不同的过渡结构导致类似的恒星配置序列，由于其共同的热力学性质。在最乐观的情况下-一个强的夸克-强子密度跳跃相变-半径观测需要小于$1\%-2\%$的分数不确定性来区分混合态和急剧的相变。对于潮汐形变，相对不确定度应小于$5\%-10\%$。然而，对于稳定夸克核附近的质量，与强烈的急剧相变和混合态相关的相对潮汐变形性差异可能要大得多（高达$20\%-30\%$左右）。所有这些都表明，第2.5代和第3代引力波探测器以及近期的电磁探测任务可能能够开始评估中子星中相变的某些特定方面。此外，指出了利用典型中子星观测量恢复状态方程的局限性，以及系统不确定性对混合星状态方程建模的影响。最后，我们简要地讨论了其他观测值，也可能是相关的探测混合状态的恒星。
英文摘要：
The internal composition of neutron stars is still an open issue in astrophysics. Their innermost regions are impervious to light propagation and gravitational waves mostly carry global aspects of stars, meaning that only indirect inferences of their interiors could be obtained. Here we assume a hypothetical future scenario in which an equation of state softening due to a phase transition is identified and estimate the observational accuracy to differentiate a sharp phase transition from a smoother one (associated with a mixed phase/state due to the unknown value of the surface tension of dense matter) in a region of a hybrid star by means of some electromagnetic and gravitational wave observables. We show that different transition constructions lead to similar sequences of stellar configurations due to their shared thermodynamic properties. In the most optimistic case - a strong quark-hadron density jump phase transition - radius observations require fractional uncertainties smaller than $1\%-2\%$ to differentiate mixed states from sharp phase transitions. For tidal deformabilities, relative uncertainties should be smaller than $5\%-10\%$. However, for masses around the onset of stable quark cores, relative tidal deformability differences associated with strong sharp phase transitions and mixed states could be much larger (up to around $20\%-30\%$). All the above suggests that 2.5- and 3rd generation gravitational wave detectors and near-term electromagnetic missions may be able to start assessing some particular aspects of phase transitions in neutron stars. In addition, it points to some limitations on the equation of state recovery using typical neutron star observables and the impact of systematic uncertainties on modellings of the equation of state of hybrid stars. Finally, we briefly discuss other observables that may also be relevant for the probe of mixed states in stars.
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