Constraints on the spatially dependent cosmic-ray propagation model from Bayesian Analysis

Abstract

The energy spectra of primary and secondary cosmic rays (CR) generally harden at several hundreds of GeV, which can be naturally interpreted by propagation effects. We adopt a spatially dependent CR propagation model to fit the spectral hardening, where a slow-diffusion disk (SDD) is assumed near the Galactic plane. We aim to constrain the propagation parameters with the Bayesian parameter estimation based on a Markov chain Monte Carlo sampling algorithm. The latest precise measurements of carbon spectrum and B/C ratio are adopted in the Bayesian analysis. The ${}^{10}\mathrm{Be}{/}^9\mathrm{Be}$ and Be/B ratios are also included to break parameter degeneracies. The fitting result shows that all the parameters are well constrained. Especially, the thickness of the SDD is limited to 0.4-0.5 kpc above and below the Galactic plane, which could be the best constraint for the slow-diffusion region among similar works. The $\bar{p}/p$ ratio and amplitude of CR anisotropy predicted by the SDD model are consistent with the observations, while the predicted high-energy electron and positron fluxes are slightly and significantly lower than the observations, respectively, indicating the necessity of extra sources.

14 pages, 16 figures

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• Interpretations of the cosmic ray secondary-to-primary ratios measured by DAMPE
• Testing the universality of cosmic-ray nuclei from protons to oxygen with AMS-02
• Can the Production Cross-Section Uncertainties Explain the Cosmic Fluorine Anomaly?
• Weighing the Local Interstellar Medium using Gamma Rays and Dust
• Combined analyses of the antiproton production from cosmic-ray interactions and its possible dark matter origin