Abstract
The source composition of cosmic rays is presented. An origin in supernova shock-wave interactions with boundary regions of the stellar wind, or acceleration of stellar flare particles accounts for most cosmic rays, though some contribution of Wolf-Rayet star material to 12C, 160 and 22Ne improves the fit. After the principal acceleration of stellar particles to cosmic-ray energies by strong shocks of young supernova remnants, a moderate reacceleration takes place by shocks of old supernova remnants that occupy a large part of the total volume of the galactic disk. This distributed acceleration is interspersed with periods of cosmic ray traversal of dense interstellar clouds, when most of the cosmic ray spallation reactions occur, accompanied also by gamma rays from π0 - decay. The effects of distributed acceleration on the ratios of secondary-to-primary cosmic rays are presented. The cosmic rays we observe near the earth probably diffuse in the Galactic disk and the inner part of the Galactic halo, since their confinement time of 107 years deduced from the abundance of 10Be exceeds that of the disk confinement model. The gamma-ray data acquired on COS-B imply a large halo as a long-duration confinement region from which cosmic rays ultimately escape into the inter-galactic space.
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Silberberg, R., Tsao, C.H., Letaw, J.R. (1989). Origin, Propagation and Distributed Acceleration of Cosmic Rays. In: Shapiro, M.M., Wefel, J.P. (eds) Cosmic Gamma Rays, Neutrinos, and Related Astrophysics. NATO ASI Series, vol 270. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0921-2_35
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DOI: https://doi.org/10.1007/978-94-009-0921-2_35
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