I. V. Moskalenko, S. G. Mashnik, A. W. Strong
Published 2001-06-27, updated 2001-08-17Version 2
We use a new version of our numerical model for particle propagation in the Galaxy to study radioactive secondaries. For evaluation of the production cross sections we use the Los Alamos compilation of all available experimental cross sections together with calculations using the improved Cascade-Exciton Model code CEM2k. Using the radioactive secondary ratios 26Al/27Al, 36Cl/Cl, 54Mn/Mn, we show how the improved cross-section calculations together with the new propagation code allow us to better constrain the size of the CR halo.
Comments: error in units (GeV->MeV) in Fig.1 is corrected; 4 pages, 8 ps-figures, to appear in the Proc. of 27th Int. Cosmic Ray Conf. (Hamburg, 2001), OG 1.3. More details can be found at http://www.gamma.mpe-garching.mpg.de/~aws/aws.html
Journal: Proc. 27th ICRC (Hamburg), 2001, pp.1836-1839
Non-thermal Origin of the EUV and Soft X-rays from the Coma Cluster - Cosmic Rays in Equipartition with the Thermal Medium
Clusters of Galaxies: Shock Waves and Cosmic Rays
Light Elements and Cosmic Rays in the Early Galaxy
