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Hot and dense matter beyond relativistic mean field theory

机译：超出相对论平均场理论的热和致密的物质

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Properties of hot and dense matter are calculated in the framework of quantum hadrodynamics by including contributions from two-loop (TL) diagrams arising from the exchange of isoscalar and isovector mesons between nucleons. Our extension of mean field theory (MFT) employs the same five density-independent coupling strengths which are calibrated using the empirical properties at the equilibrium density of isospin-symmetric matter. Results of calculations from the MFT and TL approximations are compared for conditions of density, temperature, and proton fraction encountered in the study of core-collapse supernovae, young and old neutron stars, and mergers of compact binary stars. The TL results for the equation of state (EOS) of cold pure neutron matter at sub-and near-nuclear densities agree well with those of modern quantum Monte Carlo and effective field-theoretical approaches. Although the high-density EOS in the TL approximation for cold and beta-equilibrated neutron-star matter is substantially softer than its MFT counterpart, it is able to support a 2M(circle dot) neutron star required by recent precise determinations. In addition, radii of 1.4M(circle dot) stars are smaller by similar to 1 km than those obtained in MFT and lie in the range indicated by analysis of astronomical data. In contrast to MFT, the TL results also give a better account of the single-particle or optical potentials extracted from analyses of medium-energy proton-nucleus and heavy-ion experiments. In degenerate conditions, the thermal variables are well reproduced by results of Landau's Fermi-liquid theory in which density-dependent effective masses feature prominently. The ratio of the thermal components of pressure and energy density expressed as Gamma(th) = 1 + (P-th/epsilon(th)), often used in astrophysical simulations, exhibits a stronger dependence on density than on proton fraction and temperature in both MFT and TL calculations. The prominent peak of Gamma(th) at supranuclear density found in MFT is, however, suppressed in TL calculations. This outcome is analogous to results of nonrelativistic models when exchange contributions from finite-range interactions are included in addition to those of contact interactions.
机译：通过从核心交换和核磁之间的交换中产生的两环（TL）图所产生的两环（TL）图的贡献，计算了热和致密物质的性质。我们的平均场理论（MFT）的延伸采用相同的五个密度无关的耦合强度，这些耦合强度使用索泊宾 - 对称物质的平衡密度处的经验性质进行校准。将MFT和TL近似的计算结果与核心崩溃超新星，年轻和旧中子恒星的研究中遇到的密度，温度和质子分数的条件进行比较，以及紧凑型二元恒星的合并。亚和近核密度下冷纯中子物质的状态（EOS）方程的TL结果与现代量子蒙特卡罗和有效的现场理论方法相同。尽管冷和β平衡的中子星形物的T1近似的高密度EOS比其MFT对应基本更柔软，但它能够支持近期精确测定所需的2M（圆点）中子星。此外，1.4M（圆点）恒星的半径相似至1km比在MFT中获得的那些，并且位于通过分析天文数据的分析所示的范围内。与MFT相反，TL结果还更好地说明了从中能量质子 - 核和重离子实验的分析中提取的单颗粒或光学电位。在退化条件下，通过Landau的费米液理论的结果，热变量很好地再现，其中密度相关的有效质量突出。以γ（th）= 1 +（第p-/ epsilon（第四））的压力和能量密度的热分量的比率通常用于天体物理模拟，对密度的更强依赖性而不是质子分数和温度MFT和TL计算。然而，在MFT中发现的γ（TH）的突出峰值在T1计算中抑制。这种结果类似于在除了联系相互作用之外包括有限范围相互作用的交换贡献时非素描模型的结果。

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