A United Model for the cosmic ray energy spectra and anisotropy in the energy range 100 - 100 000 GeV

TL;DR

This paper introduces a model where a recent nearby supernova influences cosmic ray spectra and anisotropy, explaining observed spectral features and anisotropy in the 100-100,000 GeV energy range.

Contribution

The model uniquely combines a local supernova event with the local bubble environment to explain cosmic ray spectral features and anisotropy.

Findings

Explains the spectral hardening at 200 GeV.

Accounts for the steepening above 50 TeV.

Describes the energy dependence of cosmic ray anisotropy.

Abstract

We propose a model where a supernova explodes in some vicinity of our solar system (some tens of parsecs) in the recent past (some tens of thousands years) with the energy release in cosmic rays of order of $ 10 ^ {51} $ erg. The flux from this supernova is added to an isotropic flux from other sources. We consider the case where the Sun's location is not in some typical for Our Galaxy average environment, but in the Local Superbubble about 100 pc across, in which the diffusion coefficient $D (E) = D_0 \times E ^ {0.6} $, with the value of $ D_0 \sim 10 ^ {25} cm^ 2 s^ {-1} $. We describe the energy dependence of the anisotropy of cosmic rays in the TeV region, together with the observed features of the energy spectrum of protons found in direct measurements. Our model provides a natural explanation to the hardening of the proton spectrum at 200 GeV, together with the observed steepening of the spectrum above 50 TeV.