On The Description Of The Turbulent Diffusion Model

Details On The Description Of The Turbulent Diffusion Model On The Description Of The Turbulent Diffusion Model

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....5.1916s&link_type=abstract

Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int

Physics

1

Scientific paper

The Standard Leaky Box model is based on an injection spectrum close to E-2 as a natural consequence of strong parallel shock acceleration. Accordingly, an empirical energy dependence of E-0.6 for propagation distance in the Galaxy is invoked to interpret the observed spectrum below 105 GeV. There are strong arguments, on the other hand, that the interstellar propagation must be based on turbulent diffusion with an energy dependence of E-1/3 . A theory of origin and transport of cosmic-rays incorporating this concept has already been formulated. In this theory the bulk of cosmicray spallation takes place in the shell of stellar winds, and light and heavy nuclei have different propagation parameters. The diffusive parameters are obtained from the primary source spectra and are calculated from the measurement of observed secondary fluxes. The observational data on heavy secondaries such as Sc, Ti and V, and B, determine the parameters of massive stellar wind shells, while measurement of light secondary elements such as ¯p together with heavy secondary particles constrain the surrounding region of both low and high mass stars. The inferred propagation parameters also depend on the choice of the initial mass function of stars. Once these parameters are set, they can be checked by measurement of other secondaries such as 3 He, 2 H, and γ. In this report we discuss how this modeling is done.

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