Effects of Turbulent Magnetic Fields in Cosmic Ray Ansiotropy

López-Barquero, Vanessa; Farber, Ryan; Desiati, P.; Lazarían, A.

doi:10.22323/1.236.0514

Cited by 2 publications

(3 citation statements)

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“…Giacinti and Sigl (2012) also showed that these local magnetic field structures could create such anisotropies. Similar work to our code was calculated in López- Barquero et al (2015). However, that study primarily looked at particles with PeV-scale energies, where the Larmor radius and mean-free-path are on parsec scales, similar in size to the coherence length of the magnetic turbulence.…”

Section: Discussionmentioning

confidence: 90%

“…Full MC integration of these TeV particles is intractably slow, so this was why a hybrid diffusion+MC method was needed. Additionally, López-Barquero et al (2015) assumed that the source population was diffuse, which allowed them to timereverse incoming particles to get maps of the anisotropic sky. However, our code allows for general source distributions in which particular CR sources are dominating the anisotropy.…”

Section: Discussionmentioning

confidence: 99%

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Explaining Tev Cosmic-Ray Anisotropies With Non-Diffusive Cosmic-Ray Propagation

Harding

Fryer

Mendel

2016

ApJ

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Constraining the behavior of cosmic ray data observed at Earth requires a precise understanding of how the cosmic rays propagate in the interstellar medium. The interstellar medium is not homogeneous; although turbulent magnetic fields dominate over large scales, small coherent regions of magnetic field exist on scales relevant to particle propagation in the nearby Galaxy. Guided propagation through a coherent field is significantly different from random particle diffusion and could be the explanation of spatial anisotropies in the observed cosmic rays. We present a Monte Carlo code to propagate cosmic particle through realistic magnetic field structures. We discuss the details of the model as well as some preliminary studies which indicate that coherent magnetic structures are important effects in local cosmic-ray propagation, increasing the flux of cosmic rays by over two orders of magnitude at anisotropic locations on the sky. The features induced by coherent magnetic structure could be the cause of the observed TeV cosmic-ray anisotropy.

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Section: Discussionmentioning

confidence: 90%

Section: Discussionmentioning

confidence: 99%

Explaining Tev Cosmic-Ray Anisotropies With Non-Diffusive Cosmic-Ray Propagation

Harding

Fryer

Mendel

2016

ApJ

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“…The new understanding of the statistics and dynamics of turbulent magnetic fields can shed light on some long-standing problems and observational puzzles (e.g., Palmer, 1982;Evoli and Yan, 2014;López-Barquero et al, 2016;Krumholz et al, 2020;Xu, 2021). It was found that the numerically tested model of MHD turbulence, rather than isotropic Kolmogorov turbulence, can satisfactorily interpret the high-precision AMS-02 measurements of CRs (Fornieri et al, 2021).…”

Section: Interactions Of Crs With Mhd Turbulencementioning

confidence: 99%

Reviews in astronomy and space sciences

2024

Frontiers Research Topics

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Effects of Turbulent Magnetic Fields in Cosmic Ray Ansiotropy

Cited by 2 publications

References 11 publications

Explaining Tev Cosmic-Ray Anisotropies With Non-Diffusive Cosmic-Ray Propagation

Explaining Tev Cosmic-Ray Anisotropies With Non-Diffusive Cosmic-Ray Propagation

Reviews in astronomy and space sciences

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