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Cited by 1,051

The DOI matches its Crossref record; 20 of the 20 references it cites were found in a registry or an index.

Propagation of Cosmic‐Ray Nucleons in the Galaxy

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Strong, Andrew W., Moskalenko, Igor V.·1998·The Astrophysical Journal

Abstract

We describe a method for the numerical computation of the propagation of primary and secondary nucleons, primary electrons, and secondary positrons and electrons. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields, and diffusive reacceleration is also incorporated. The models are adjusted to agree with the observed cosmic-ray B/C and 10 Be/ 9 Be ratios. Models with diffusion and convection do not account well for the observed energy dependence of B/C, while models with reacceleration reproduce this easily. The height of the halo propagation region is determined using recent 10 Be/ 9 Be measurements as >4 kpc for diffusion/convection models and 4-12 kpc for reacceleration models. For convection models, we set an upper limit on the velocity gradient of dV / dz < 7 km s -1 kpc -1 . The radial distribution of cosmic-ray sources required is broader than current estimates of the supernova remnant (SNR) distribution for all halo sizes. Full details of the numerical method used to solve the cosmic-ray propagation equation are given.

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Metadata

Authors
Strong, A. W., & Moskalenko, I. V.
Venue
The Astrophysical Journal
Published
1998-12-10
Volume
509
Issue
1
Pages
212-228
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2122658693
Cited by
1,051
References
20
FWCI
10.40
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: Propagation of Cosmic‐Ray Nucleons in the Galaxy. https://app.cochat.ai/papers/10.1086/306470
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Strong, A. W., & Moskalenko, I. V. (1998). Propagation of Cosmic‐Ray Nucleons in the Galaxy. The Astrophysical Journal. https://doi.org/10.1086/306470

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