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Cosmic-ray propagation and interactions in the Galaxy
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Cosmic-ray propagation and interactions in the Galaxy
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We survey the theory and experimental tests for the propagation of cosmic rays in the Galaxy up to energies of 10^15 eV. A guide to the previous reviews and essential literature is given, followed by an exposition of basic principles. The basic ideas of cosmic-ray propagation are described, and the physical origin of its processes are explained. The various techniques for computing the observational consequences of the theory are described and contrasted. These include analytical and numerical techniques. We present the comparison of models with data including direct and indirect - especially gamma-ray - observations, and indicate what we can learn about cosmic-ray propagation. Some particular important topics including electrons and antiparticles are chosen for discussion.
Forward citations
Cited by 11 Pith papers
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Charge-dependent spectral softenings of primary cosmic-rays below the knee
Direct measurements reveal charge-dependent spectral softenings in primary cosmic rays at a common rigidity of ~15 TV, rejecting mass-dependent softening at >99.999% confidence.
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PeV particle acceleration and non-thermal emission in the `minimalist' model of the extended jets in W50/SS433
A model of SS433/W50's extended jets with diffusive shock acceleration reproduces X-ray spectra, gamma-ray emission, and >20% X-ray polarization, with >10% of jet power going into PeV protons.
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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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Hybrid Simulations of Proton Acceleration at Oblique High-$\beta$ Shocks
Weak quasi-perpendicular high-β ICM shocks accelerate protons inefficiently (ε_CR ≲ 0.1%), while Ms ≳ 10 or ϑ ≲ 45° shocks reach a few percent with steep spectra.
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SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics
A self-consistent multi-zone kinetic model reproduces SN 1006's spectrum and morphology, finding ~20% CR acceleration efficiency in quasi-parallel shocks, <1% in quasi-perpendicular shocks, and predominantly leptonic ...
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On The Nonthermal Power Laws In Magnetized Turbulent Plasmas
Derives and validates via PIC simulations a scaling law for nonthermal spectral tails in mildly to strongly magnetized turbulent plasmas, with application to black-hole coronae.
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On the contribution of the bow shock pulsar wind nebula PSR J0437-4715 to the observed fluxes of GeV-TeV positrons and antiprotons
The bow shock pulsar wind nebula around PSR J0437-4715 explains the GeV-TeV positron excess and hundreds-of-GeV antiproton flux with an energy-independent ratio by using 25% of the pulsar's wind power.
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Constraints on Primordial Black Holes from Galactic Diffuse Synchrotron Emissions
Galactic synchrotron emissions above 20 MHz can set tighter upper limits on the abundance of primordial black holes with masses above 10^16 grams than previous cosmic-ray electron data.
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Proton-Proton to Antinucleon Cross Sections for Cosmic Ray Applications
NLO perturbative QCD calculations predict only a mild few-percent excess of antineutrons over antiprotons in pp collisions, not supporting the ~30% excess reported by NA49.
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On The Nonthermal Power Laws In Magnetized Turbulent Plasmas
A scaling law for nonthermal power-law tails in magnetized turbulent plasmas is derived from particle transport principles and confirmed by PIC simulations with escape, with applications to black hole coronae.
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Probing Low-Luminosity Gamma-Ray Emission from SNR G296.5+10.0 and CCO 1E 1207.4-5209 with CTAO
Numerical modeling with GALPROP predicts CTAO detectability of gamma rays from SNR G296.5+10.0 and CCO 1E 1207.4-5209 at 5 sigma after 50 hours, with hadronic processes dominating at lower energies and leptonic at higher.
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