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Origin of the Cosmic Ray Spectral Hardening
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Recent data from ATIC, CREAM and PAMELA indicate that the cosmic ray energy spectra of protons and nuclei exhibit a remarkable hardening at energies above 100 GeV per nucleon. We propose that the hardening is an interstellar propagation effect that originates from a spatial change of the cosmic-ray transport properties in different regions of the Galaxy. The key hypothesis is that the diffusion coefficient is not separable into energy and space variables as usually assumed. Under this scenario, we can reproduce the observational data well. Our model has several implications for the cosmic-ray acceleration/propagation physics and can be tested by ongoing experiments such as the Alpha Magnetic Spectrometer or Fermi/LAT.
Forward citations
Cited by 4 Pith papers
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On the Contribution of Local Sources to the Galactic Cosmic-Ray Spectrum: An Exact Series Solution for Two-Zone Diffusion
Derives series solution for two-zone cosmic-ray diffusion and finds local-source probability at 10 TeV rises from 0.4% to 1.7-2.2% but remains model-dependent.
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Uncertainty in Hadronic Diffuse $\gamma$-Ray Emission from the Temporal Stochasticity of Cosmic-Ray Sources
Temporal stochasticity of cosmic-ray sources causes a normalization uncertainty in the local proton flux that propagates into a hadronic gamma-ray uncertainty of 30-100%, comparable to or exceeding experimental errors...
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Influence of interstellar environment near the solar system on cosmic-ray spectra and dipole anisotropy
A three-component cosmic-ray model that includes the local interstellar cloud's motion and magnetic field reproduces the energy-dependent dipole anisotropy of cosmic rays from GeV to PeV energies, but with many fitted...
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Implication of multiple source populations of Galactic cosmic rays from proton and helium spectra
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