By John P. Wefel (auth.), Maurice M. Shapiro, John P. Wefel (eds.)

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Watson, A. , 1984, Adv. , ~ 35. Webber, W. , 1983, in Composition and Origin of Cosmic Rays, ed. M. M. Shapiro (Dordrecht, Holland: D. ), p. 83. Webber, W. , 1982, Ap. , 252, 386. Webber, W. R. and Yushak, S. , 1983, Ap. , 275, 391. Webber, W. , Kish, J. C. and Schrier, D. , ~5, 19th ICRC Conference Papers, 2, 88. Webber, W. R. and Kish, Jr. , 1979, 16th ICRC Conference Papers, ~ 389. Webber, W. , Lezniak, J. , Kish, J. C. and Simpson, J. , 1977, Astro. , 18, 125. Weiler, K. , 1987~in Genesis and Propagation of Cosmic Rays, eds.

Do cosmic rays escape from confinement volume where most material is traversed by a diffusive process (scattering by magnetic field structures) or a convective process (associated with bursting of the confining magnetic field)? The relative abundance of various secondary cosmic rays, with different nuclear interaction mean path lengths helps to resolve this problem; the distribution of path lengths is broad and exponential in shape in the case of diffusive escape, and narrow in the case of convective escape.

Particle Confinement The fundamental questions in this area are "where" and "how". g. Hermsen and B10emen, 1984), but are these particles also confined for some part of their lifetime to regions around the source/acceleration sites and/or do they spend a significant amount of time in a low density halo around the galaxy? In this regard, the possibility of the existence of a galactic wind, constantly expelling gas from the galaxy (Jokipii, 1976), and its convective effect on the cosmic rays must be considered.

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