Implications of turbulence-dependent diffusion on cosmic-ray spectra. (arXiv:2110.06676v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dorner_J/0/1/0/all/0/1">J. Dörner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichherzer_P/0/1/0/all/0/1">P. Reichherzer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Merten_L/0/1/0/all/0/1">L. Merten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tjus_J/0/1/0/all/0/1">J. Becker Tjus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fichtner_H/0/1/0/all/0/1">H. Fichtner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pueschel_M/0/1/0/all/0/1">M. J. Pueschel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zweibel_E/0/1/0/all/0/1">E. G. Zweibel</a>
The propagation of cosmic rays can be described as a diffusive motion in most
galactic environments. High-energy gamma-rays measured by Fermi have allowed
inference of a gradient in the cosmic-ray density and spectral energy behavior
in the Milky Way, which is not predicted by models. Here, a
turbulence-dependent diffusion model is used to probe different types of
cosmic-ray diffusion tensors. Crucially, it is demonstrated that the observed
gradients can be explained through turbulence-dependent energy-scaling of the
diffusion tensor.
The propagation of cosmic rays can be described as a diffusive motion in most
galactic environments. High-energy gamma-rays measured by Fermi have allowed
inference of a gradient in the cosmic-ray density and spectral energy behavior
in the Milky Way, which is not predicted by models. Here, a
turbulence-dependent diffusion model is used to probe different types of
cosmic-ray diffusion tensors. Crucially, it is demonstrated that the observed
gradients can be explained through turbulence-dependent energy-scaling of the
diffusion tensor.
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