摘要
磁场:决定宇宙偏差的偏置示踪元素
作者(年代):苏亚塔M,拉玛娜H,拉杰什G在这个宇宙中,90%的物质是不可见的暗物质,10%的物质是可见的重子物质。重子物质包括我们今天看到的所有星系。但是大尺度结构的演化包含了潜在的暗物质。暗物质只受引力场的影响,而重子物质则受引力场、辐射压力、磁场等的影响。这种差异导致了偏差因素的研究,称为宇宙学偏差。研究领域对宇宙学性质的研究是开放的,这是可能的宇宙学偏差的研究。它是重子物质密度与暗物质密度之比。宇宙学偏差的研究确实是一个有趣的话题,揭示了更多关于大尺度结构演化的谜团。宇宙学偏差提供了一个广泛的范围,以了解潜在的暗物质的性质。所以宇宙学偏差是一个值得研究的重要课题。 Magneto hydrodynamic equations containing magnetic field as the source term in matter dominated era treated as the basic equations to find the required equation for matter density. This equation contains the information about dark matter density (δ_DM) and the baryonic matter density (δ_b) . This equation is solved analytically at different red shift values (z). The value of b is found to be 6.327 at z=0. As the value of z decreases from z=1000 to z=0 the value of bias increases from 0 to 6.327 which indicates that presence of magnetic field is amplified that means the magnetic field can be one of the bias tracer element.
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