发表机构
School of Physics, University of Hyderabad（海德拉巴大学物理学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过旋转群不可约表示分析磁流体湍流相干结构，发现高斯与非高斯磁场产生不同结构，极化各向异性主导，影响早期宇宙粒子输运。
AI 中文摘要
本文利用SO(3)和SO(2)旋转群的不可约表示，研究了磁流体动力学湍流中相干结构的拓扑类别。我们探测了宇宙中轴对称磁场周围的相干结构。这种轴对称场可以在丝状结构以及宇宙弦周围找到。我们考虑了高斯和非高斯磁场两种情况。我们发现，场分布导致这两种情况产生不同的相干结构。我们的结果表明，粒子从高斯结构中的散射主要依赖于两个长度尺度。在非高斯分布的情况下，我们可以定义第三个中间长度尺度，类似于泰勒长度尺度。在两种情况下，我们都发现极化各向异性占主导地位，这表明场梯度被强制进入刚性空间构型。在早期宇宙中，这将改变重子和轻子在相干结构中的平均自由程。在具有重尾分布的磁场情况下，带电粒子的俘获及其加速将更加频繁。因此，靠近这些结构的密度不均匀性的长度尺度将由磁场的分布决定。
英文摘要
The topological classes of coherent structures in magnetohydrodynamic turbulence are studied using the irreducible representations of the SO(3) and SO(2) rotation groups. We probe the coherent structures around axisymmetric magnetic fields in the universe. Such axisymmetric fields can be found around filamentary structures as well as cosmic strings. We have considered a Gaussian and a non Gaussian magnetic field. We find that the field distribution leads to different coherent structures for the two cases. Our results show that the scattering of particles from the Gaussian structure depends predominantly on two lengthscales. In the case of the non Gaussian distribution, we can define a third intermediate lengthscale, similar to the Taylor lengthscale. In both the cases, we find that there is a dominance of the polarization anisotropy which indicates that the field gradients are forced into rigid spatial configurations. In the early universe, this will change the mean free path of the baryons and leptons in the coherent structures. Trapping of charged particle as well as their acceleration will be more frequent in the case of a magnetic field with a heavy tailed distribution. The lengthscale of density inhomogeneities close to these structures will thus be determined by the magnetic field distribution of the fields.
Comments16 pages 12 figures
