From neutron skins and neutron matter to the neutron star crust
From neutron skins and neutron matter to the neutron star crust
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DOI：
10.1016/j.physletb.2022.137481
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发表时间：
2021-11
影响因子：
4.4
通讯作者：
W. Newton;R. Preston;Lauren Balliet;M. Ross
中科院分区：
文献类型：
--
作者：
W. Newton;R. Preston;Lauren Balliet;M. Ross
我们提出了第一个贝叶斯推断的中子星星地壳属性，将中子皮肤的数据，包括最近PREX测量的中子皮肤的208铅，结合最近的手征有效场理论预测的纯中子物质的统计误差。使用可压缩液滴模型和扩展的Skyrme能量密度泛函，我们得到了迄今为止最严格的临界压力Pcc = 0.33 - 0.07+ 0.07 MeV fm-3和化学势μ cc= 12.6 - 1.9+ 1.8 MeV（控制中子星星壳的质量、转动惯量和厚度），包含pasta相的质子分数yp = 0.115 - 0.017+ 0.016和ycc = 0.041 - 0.006+ 0.007，以及非球形核层的相对质量和转动惯量Δ Mp/Δ Mc = 0.54 - 0.09+ 0.05和厚度Δ Rp/Δ Rc = 0.129 - 0.030+ 0.019（核意大利面）在地壳。
We present the first Bayesian inference of neutron star crust properties to incorporate neutron skin data, including the recent PREX measurement of the neutron skin of 208 Pb, combined with recent chiral effective field theory predictions of pure neutron matter with statistical errors. Using a compressible liquid drop model with an extended Skyrme energy-density functional, we obtain the most stringent constraints to date on the transition pressure P cc= 0.33− 0.07+ 0.07 MeV fm− 3 and chemical potential μ cc= 12.6− 1.9+ 1, 8 MeV (which control the mass, moment of inertia and thickness of a neutron star crust), the proton fractions that bracket the pasta phases y p= 0.115− 0.017+ 0.016 and y cc= 0.041− 0.006+ 0.007, as well as the relative mass and moment of inertia Δ M p/Δ M c≈ Δ I p/Δ I c= 0.54− 0.09+ 0.05 and thickness Δ R p/Δ R c= 0.129− 0.030+ 0.019 of the layers of non-spherical nuclei (nuclear pasta) in the crust.