动摩擦中多体相互作用的修正效应
Corrective effect of many-body interactions in dynamical friction
摘要：
动力学摩擦是天体物理中一个基本而重要的现象。Escherasekhar公式是一个众所周知的分析估计的效果。然而，目前的天体物理学家已经意识到，在某些情况下，由于公式中的几个近似和/或真实宇宙中复杂的非线性，该公式是不正确的。例如，已经表明，尽管在恒定密度下，Mr. rasekhar公式预测了阻力，但在核心密度分布（中心区域的恒定密度）中动态摩擦不起作用。在本文的前半部分，我讨论了多体相互作用在实际的动力学摩擦中也是重要的，虽然推导的Eschrasekhar公式是基于两体相互作用的假设，通过N体模拟。在模拟中，多体相互作用是由极少数场粒子与微扰器共同旋转引起的。然而，来自多体相互作用的贡献占实际动力学摩擦的不可忽略的部分。在后半部分，我讨论了为什么核心配置文件抑制动力学摩擦。一种可能的解释是，多体相互作用的校正效应驱动了微扰器的轨道运动。即使在浅尖点密度剖面中，通过这种校正效应停止动力学摩擦也是可行的，尽管浅尖点可能演变成恒定密度。
英文摘要：
Dynamical friction is a fundamental and important phenomenon in astrophysics. The Chandrasekhar formula is a well-known analytical estimation of the effect. However, current astrophysicists have realized that the formula is not correct in some cases because of several approximations dared in the formulation and/or complex non-linearities in the real universe. For example, it has been indicated that the dynamical friction doesn't work in cored density profiles (constant density in the central region) despite that the Chandrasekhar formula predicts drag force even in the constant densities. In the former half of this paper, I discuss by N-body simulations that many-body interactions are also important in actual dynamical friction though derivation of the Chandrasekhar formula is based on the assumption of two-body interaction. In the simulation, the many-body interactions are caused by a very small number of field particles co-rotating with a perturber. However, the contribution from the many-body interactions accounts for a non-negligible fraction of the actual dynamical friction. In the latter half, I discuss why the cored profiles suppress the dynamical friction. One possible explanation is that corrective effect of the many-body interactions drive orbital motion of the perturber. The cessation of dynamical friction by this corrective effect would be feasible even in shallow cusp density profiles although the shallow cusp may evolve into a constant density.
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