非理想自引力和宇宙学：宇宙大尺度结构动力学中相关性的重要性
Non-ideal self-gravity and cosmology: the importance of correlations in the dynamics of the large-scale structures of the Universe
摘要：
受相互作用粒子系综（BBGKY层次）统计力学的启发，我们提出了一个非理想的维里定理和非理想的纳维-斯托克斯方程使用的引力分解成一个近场和远场分量推导的自引力天体物理流体的小尺度不均匀性。这些方程涉及对径向分布函数（类似于两点关联函数），类似于液体中的相互作用能和状态方程。小尺度相关导致引力相互作用能的非理想放大，其省略导致质量缺失问题，例如，在星系和星系团中。我们还提出了一个扩展的弗里德曼方程在非理想政权。我们估计重子的引力相互作用能的非理想放大因子在5到20之间，这可能解释了哈勃参数的观测值。在这个框架内，膨胀的加速自然出现，因为引力坍缩引起的子结构的数量增加，这增加了它们对总引力能的贡献。一个简单的估计预测一个非理想的减速参数qni~-1;这可能是第一次确定的观察值的基础上直观的物理参数。我们认为，相关性和引力相互作用可能会产生一个过渡到粘性制度，可以导致平坦的旋转曲线。这种转变也可以解释（开普勒）LSB椭圆星系和（非开普勒）螺旋星系旋转轮廓之间的二分法。总的来说，我们的研究结果表明，非均匀性引起的非理想效应必须考虑，以正确地确定星系和更大尺度的宇宙的引力动力学。
英文摘要：
Inspired by the statistical mechanics of an ensemble of interacting particles (BBGKY hierarchy), we propose to account for small-scale inhomogeneities in self-gravitating astrophysical fluids by deriving a non-ideal Virial theorem and non-ideal Navier-Stokes equations using a decomposition of the gravitational force into a near- and far-field component. These equations involve the pair radial distribution function (similar to the two-point correlation function), similarly to the interaction energy and equation of state in liquids. Small-scale correlations lead to a non-ideal amplification of the gravitational interaction energy, whose omission leads to a missing mass problem, e.g., in galaxies and galaxy clusters. We also propose an extension of the Friedmann equations in the non-ideal regime. We estimate the non-ideal amplification factor of the gravitational interaction energy of the baryons to lie between 5 and 20, potentially explaining the observed value of the Hubble parameter. Within this framework, the acceleration of the expansion emerges naturally because of the increasing number of sub-structures induced by gravitational collapse, which increases their contribution to the total gravitational energy. A simple estimate predicts a non-ideal deceleration parameter qni~-1;this is potentially the first determination of the observed value based on an intuitively physical argument. We suggest that correlations and gravitational interactions could produce a transition to a viscous regime that can lead to flat rotation curves. This transition could also explain the dichotomy between (Keplerian) LSB elliptical galaxy and (non-Keplerian) spiral galaxy rotation profiles. Overall, our results demonstrate that non-ideal effects induced by inhomogeneities must be taken into account in order to properly determine the gravitational dynamics of galaxies and the larger scale universe.
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