在宇宙微波背景内的晚期各向异性和辐射阻力
Late-time anisotropy and radiation drag within the cosmic microwave background
摘要：
我调查的辐射拖曳力的影响，对恒星的运动相对于宇宙微波背景（CMB）在z = 0。正如预期的那样，扰动非常小，对星系内恒星的轨道运动或星系团内星系的轨道运动没有可观测的影响。通过这种机制在星系中以立方米为单位耗散的能量比宇宙微波背景辐射的能量密度小10^{14}，因此可以忽略各向异性的来源。然而，从最后一个散射表面到第III星族星（30 < z < 1000），粒子的辐射阻力可能在各向异性的出现和密度的快速形成中发挥了重要作用。
英文摘要：
I investigate the effect of the radiation drag force on a star moving relative to the Cosmic Microwave Background (CMB) at z = 0. As expected, the perturbation is extremely small and has no observable consequences on orbital motions of stars within a galaxy or on orbital motions of galaxies within a cluster. The energy dissipated by cubic meter in a galaxy via this mechanism is 10^{14} smaller than the energy density of the CMB and, thus, is a negligible source of anisotropy. However, from the last scattering surface to population III stars (30 < z < 1000), radiation drag on particles may have played a major role in the apparition of anisotropy and rapid formation of densities.
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