磁化温度自关联的半解析方法
Semi-analytical approach to magnetized temperature autocorrelations
摘要：
用半解析方法计算了由磁化绝热模曲率不均匀性引起的宇宙微波背景（CMB）温度自关联。正如最新的CMB数据所建议的那样，绝热模式的近尺度不变的光谱是一致的。在这种情况下，一个完全不均匀的磁场的影响进行了仔细检查和约束，特别注意谐波是相关的多普勒振荡的区域。取决于随机磁场的参数，峰可以取代角功率谱的第二峰。只有当磁功率谱具有准平坦的斜率和典型的振幅（在Mpc大小的共动尺度上平滑，并红移到原星系的引力坍缩时期）超过0.1 nG时，才有望对多普勒区域产生可检测的影响。如果磁能谱更蓝（即频率更陡），则平滑振幅的允许值相对地变得更大（在20 nG的范围内）。讨论了这一研究对宇宙中大尺度磁场起源的意义。与即将到来的实验观测CMB温度波动的连接也建议和部分探讨。
英文摘要：
The cosmic microwave background (CMB) temperature autocorrelations, induced by a magnetized adiabatic mode of curvature inhomogeneities, are computed with semi-analytical methods. As suggested by the latest CMB data, a nearly scale-invariant spectrum for the adiabatic mode is consistently assumed. In this situation, the effects of a fully inhomogeneous magnetic field are scrutinized and constrained with particular attention to harmonics which are relevant for the region of Doppler oscillations. Depending on the parameters of the stochastic magnetic field a hump may replace the second peak of the angular power spectrum. Detectable effects on the Doppler region are then expected only if the magnetic power spectra have quasi-flat slopes and typical amplitude (smoothed over a comoving scale of Mpc size and redshifted to the epoch of gravitational collapse of the protogalaxy) exceeding 0.1 nG. If the magnetic energy spectra are bluer (i.e. steeper in frequency) the allowed value of the smoothed amplitude becomes, comparatively, larger (in the range of 20 nG). The implications of this investigation for the origin of large-scale magnetic fields in the Universe are discussed. Connections with forthcoming experimental observations of CMB temperature fluctuations are also suggested and partially explored.
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