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Propagation of cosmic-ray nuclei in a diffusing galaxy with convective halo and thin matter diskA diffusion model for cosmic-ray propagation in the galaxy that includes the effects of convection in the halo is presented. Calculations are made for 13 primary and secondary nuclei with rigidities between 1 and 1000 GV using interaction loss rates, secondary production rates, and radioactive decay on the basis of recent new cross-section measurements. It is found that, in order to fit the rather weak radial dependence of cosmic-ray protons derived from gamma-ray data, the radial profile of the cosmic-ray sources must also have a weak radial dependence. It is suggested that convection perpendicular to the disk of the Milky Way Galaxy may not be important even at rigidities less than a few GV. The obtained limits on halo thicknesses are consistent with what can be determined for the distribution of cosmic-ray electrons in the halo based on the distribution of radio synchrotron emission in this and other galaxies.
Document ID
19920052761
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Webber, W. R.
(New Mexico State University Las Cruces, United States)
Lee, M. A.
(New Hampshire, University Durham, United States)
Gupta, M.
(New Mexico State University Las Cruces, United States)
Date Acquired
August 15, 2013
Publication Date
May 1, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 390
Issue: 1 Ma
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
92A35385
Funding Number(s)
CONTRACT_GRANT: NAGW-76
CONTRACT_GRANT: NSF ATM-89-03703
CONTRACT_GRANT: NAGW-2016
CONTRACT_GRANT: NAGW-1530
Distribution Limits
Public
Copyright
Other

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