arXiv 2302.083722023-02hep-phastro-ph.HEnucl-exnucl-th

基于QCD求和规则与中子星-黑洞质量间隙的无限核介质性质

Properties of Infinite Nuclear Medium from QCD Sum Rules and the Neutron Star-Black Hole Mass Gap

Bijit Singha, Debasish Das, Leonard S. Kisslinger

备注：: 3 Figures

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AI总结：

研究利用QCD求和规则计算核子介质自能并结合相对论平均场与Einstein方程，预言中子星-黑洞质量谱存在[3.48M⊙,5.47M⊙]质量间隙。

摘要：

本文提供了一个非微扰框架，用于在中高密度区间将QCD与核唯象学联系起来。利用QCD求和规则，将核子的介质中标量和矢量自能作为无限核介质密度的函数进行计算。在Borel改进的重求和方案中，这些自能被用于高密度核介质的相对论平均场理论拉格朗日量，以求得介质中核子的结合能以及轻夸克凝聚值，即⟨q̄q⟩_vac = −(0.288 GeV)^3。理想中子星的临界质量是通过将冷密核物质的均匀饱和能量密度与流体静力学平衡中的Einstein方程耦合得到的。由于中子星核心较难避免退禁闭并进入刚性矢量排斥相（在该相中声速可从共形极限平滑趋近因果极限），恒星质量谱中应存在一个间隙[3.48M⊙, 5.47M⊙]，在该区间内很难发现任何孤立、寒冷、不旋转的中子星或黑洞。

英文摘要：

A non-perturbative framework is provided to connect QCD with nuclear phenomenology in the intermediate and high density regime. Using QCD Sum Rules, in-medium scalar and vector self-energies of nucleons are calculated as functions of the density of an infinite nuclear medium. The self-energies are used in the relativistic mean field theory lagrangian of a high-density nuclear medium to find the binding energy of in-medium nucleons and the value of light quark condensate, $\langle \bar{q} q \rangle_{\rm{vac}} = -~(0.288 ~\rm{GeV})^3$, in the Borel-improved resummation scheme. The critical mass of an ideal neutron star is obtained by coupling a uniform saturation energy density of cold, dense nuclear matter to Einstein equation in hydrostatic equilibrium. Since it is less likely for a neutron star core to avoid deconfinement and enter the rigid vector repulsion phase where the speed of sound can smoothly approach from conformal to causal limit, a gap should exist in the stellar mass spectrum, $[3.48M_\odot, 5.47M_\odot]$, where it would be rare to find any isolated, cold, non-rotating neutron star or a black hole.

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