论文标题
相对论平均场模型的贝叶斯推断，从观察到NICER和GW170817/AT2017GFO的中子恒星物质。
A Bayesian inference of relativistic mean-field model for neutron star matter from observation of NICER and GW170817/AT2017gfo
论文作者
论文摘要
二进制中子星的光学和近红外对应物的观察不仅丰富了我们对宇宙中沉重元素丰富的知识，或者有助于揭示在合并的合并后的残余物体，而且还可以有效地约束密集的核物质和状态（EOS（EOS）（EOS）在合并星体内部。遵循对核物质的相对论均值描述，我们使用第一个多通讯生事件GW170817/AT2017GFO进行了对EOS和核物质特性的贝叶斯推断，以及对脉冲脉冲的质量质量更高。 KilOnova通过具有动力学喷射的辐射转移模型来描述，光曲线通过弹出性能（弹出质量，速度，不透明度或电子分数）和二进制参数（质量比和降低的潮汐降低可降低性）之间的准全面关系与EOS连接。发现从AT2017GFO分析中降低的潮汐变形性的后验分布显示了双峰结构，而GW170817数据则增强了第一个峰，导致EOSS略微软化，而第二个峰则无法通过其效果范围内的核EOS效果来实现第二个峰。在我们的分析中包含更好的数据会导致EOS后部僵硬，因为巨大的PULSAR PSR J0740+6620。我们从对这些观察数据的分析中，以核不压性，对称能及其斜率以及核子有效质量为核饱和密度提供结果。
The observations of optical and near-infrared counterparts of binary neutron star mergers not only enrich our knowledge about the abundance of heavy elements in the Universe, or help reveal the remnant object just after the merger as generally known, but also can effectively constrain dense nuclear matter properties and the equation of state (EOS) in the interior of the merging stars. Following the relativistic mean-field description of nuclear matter, we perform the Bayesian inference of the EOS and the nuclear matter properties using the first multi-messenger event GW170817/AT2017gfo, together with the NICER mass-radius measurements of pulsars. The kilonova is described by a radiation-transfer model with the dynamical ejecta, and light curves connect with the EOS through the quasi-universal relations between the ejecta properties (the ejected mass, velocity, opacity or electron fraction) and binary parameters (the mass ratio and reduced tidal deformability). It is found that the posterior distributions of the reduced tidal deformability from the AT2017gfo analysis display a bimodal structure, with the first peak enhanced by the GW170817 data, leading to slightly softened posterior EOSs, while the second peak cannot be achieved by a nuclear EOS with saturation properties in their empirical ranges. The inclusion of NICER data in our analyses results in stiffened EOS posterior because of the massive pulsar PSR J0740+6620. We give results at nuclear saturation density for the nuclear incompressibility, the symmetry energy and its slope, as well as the nucleon effective mass, from our analysis of those observational data.
