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Direct astrophysical tests of chiral effective field theory at supranuclear densities

机译：上颅核密度的手性有效场理论的直接天体性试验

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Recent observations of neutron stars with gravitational waves and x-ray timing provide unprecedented access to the equation of state (EoS) of cold dense matter at densities difficult to realize in terrestrial experiments. At the same time, predictions for the EoS equipped with reliable uncertainty estimates from chiral effective field theory (chi EFT) allow us to bound our theoretical ignorance. In this work, we analyze astrophysical data by using a nonparametric representation of the neutron-star EoS conditioned on x EFT to directly constrain the underlying physical properties of the compact objects without introducing modeling systematics. We discuss how the data alone constrain the EoS at high densities when we condition on chi EFT at low densities. We also demonstrate how to exploit astrophysical data to directly test the predictions of chi EFT for the EoS up to twice nuclear saturation density, in order to estimate the density at which these predictions might break down. We find that the existence of massive pulsars, gravitational waves from GW170817, and NICER observations of PSR J0030 + 0451 favor LEFT predictions for the EoS up to nuclear saturation density over a more agnostic analysis by as much as a factor of seven for the quantum Monte Carlo (QMC) calculations used in this work. While chi EFT predictions using QMC are fully consistent with gravitational-wave data up to twice nuclear saturation density, NICER observations suggest that the EoS stiffens relative to these predictions at or slightly above nuclear saturation density. Additionally, for these QMC calculations, we marginalize over the uncertainty in the density at which chi EFT begins to break down, constraining the radius of a 1.4M(circle dot) neutron star to R-1.4 = 11.40(-1.04)(+.138)(12.54(-0.63)(+0.71)) km and the pressure at twice nuclear saturation density to p(2n(sat)) = 14.2(-8.4)(+18.1) (28.7(-15.0)(+15.3)) MeV/fm(3) with massive pulsar and gravitational-wave (and NICER) data.
机译：最近通过引力波和x射线计时对中子星进行的观测，提供了前所未有的途径，可以在地球实验中难以实现的密度下获得冷稠密物质的状态方程（EoS）。同时，根据手征有效场理论（chi-EFT）对物态方程的预测以及可靠的不确定性估计，使我们能够限制我们的理论无知。在这项工作中，我们通过使用x EFT条件下中子星状态方程的非参数表示来分析天体物理数据，以直接约束致密物体的基本物理性质，而不引入建模系统学。我们讨论了当我们在低密度条件下进行chi EFT时，仅数据如何在高密度条件下约束EoS。我们还演示了如何利用天体物理数据直接测试高达两倍核饱和密度的状态方程的chi-EFT预测，以便估计这些预测可能崩溃的密度。我们发现，大质量脉冲星、来自GW170817的引力波的存在，以及对PSR J0030+0451的更好观测，有利于对EoS的左预测，使其达到核饱和密度，而不是更不可知论的分析，对于本工作中使用的量子蒙特卡罗（QMC）计算，左预测高达7倍。虽然使用QMC进行的chi-EFT预测与核饱和密度高达两倍的引力波数据完全一致，但更好的观测表明，相对于这些预测，EoS在或略高于核饱和密度时会变硬。此外，对于这些QMC计算，我们忽略了chi EFT开始分解时密度的不确定性，将1.4M（圆点）中子星的半径限制在R-1.4=11.40（-1.04）（+138）（12.54（-0.63）（+0.71））km，并将两倍核饱和密度下的压力限制在p（2n（sat））=14.2（-8.4）（+18.1）（28.7（-15.0）（+15.3））MeV/fm（3），并提供大量脉冲星和引力波（以及更好的）数据。

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