Modeling of the high-energy galactic cosmic-ray anisotropy
Modeling of the high-energy galactic cosmic-ray anisotropy
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DOI：
10.5194/astra-6-49-2010
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发表时间：
2010-12
期刊：
影响因子：
--
通讯作者：
M. Amenomori
中科院分区：
文献类型：
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作者：
M. Amenomori
讨论了 TeV 能量的银河宇宙线大范围各向异性的可能起源。它可以通过全局各向异性和中尺度各向异性的叠加来很好地建模。全球各向异性将由银河宇宙射线与日光层周围 2 pc 尺度的局部星际空间中的磁场相互作用而产生。另一方面，中尺度各向异性可能是由日尾星系宇宙射线的调制引起的，它被表示为沿着氢偏转平面放置的两个强度增强，每个强度增强都对称地远离日尾方向。我们发现，在 4-30 TeV 能量范围内，日尾方向与每次增强之间的分离角随着能量的增加而单调减小。
A possible origin of the large-scale anisotropy of galactic cosmic rays at TeV energies is discussed. It can be well modeled by a superposition of the Global Anisotropy and the Midscale Anisotropy. The Global Anisotropy would be generated by galactic cosmic rays interacting with the magnetic field in the local interstellar space of scale 2 pc surrounding the heliosphere. On the other hand, the Midscale Anisotropy, possibly caused by the modulation of galactic cosmic rays in the heliotail, is expressed as two intensity enhancements placed along the Hydrogen Deflection Plane, each symmetrically centered away from the heliotail direc- tion. We find that the separation angle between the helio- tail direction and each enhancement monotonously decreases with increasing energy in an energy range 4-30 TeV.