Cosmic ray small-scale anisotropies in quasi-linear theory

被引：8

作者：

Mertsch, P. ^{[1
,2
,3
]}

Ahlers, M. ^{[2
,3
]}

机构：

[1] Rhein Westfal TH Aachen, Inst Theoret Particle Phys & Cosmol TTK, D-52056 Aachen, Germany

[2] Niels Bohr Int Acad, Blegdamsvej 17, DK-2100 Copenhagen, Denmark

[3] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, DK-2100 Copenhagen, Denmark

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2019年 / 11期

关键词：

cosmic ray theory; galactic magnetic fields; DIFFUSION; TURBULENCE; PARTICLES; TRANSPORT;

D O I：

10.1088/1475-7516/2019/11/048

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The distribution of arrival directions of cosmic rays is remarkably isotropic, which is a consequence of their repeated scattering in magnetic fields. Yet, high-statistics observatories like IceCube and HAWC have revealed the presence of small-scale structures at levels of 1 part in 10,000 at hundreds of TeV, which are not expected in typical diffusion models of cosmic rays. We follow up on the suggestion that these small-scale anisotropies are a result of cosmic ray streaming in a particular realisation of the turbulent magnetic field within a few scattering lengths in our local Galactic neighbourhood. So far, this hypothesis has been investigated mostly numerically, by tracking test particles through turbulent magnetic fields. For the first time, we present an analytical computation that through a perturbative approach allows predicting the angular power spectrum of cosmic ray arrival directions for a given model of turbulence. We illustrate this method for a simple, isotropic turbulence model and we find remarkable agreement with the results of numerical studies.

引用

页数：12

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