Cosmic Rays From ISM Gas and Dust

Details Cosmic Rays From ISM Gas and Dust Cosmic Rays From ISM Gas and Dust

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.624e&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

We show that the cosmic ray composition, with no exceptions, can be accounted for to within experimental uncertainties if SNR shocks accelerate ambient ISM material consisting of gas and dust. Standard and well-tested assumptions for efficient diffusive shock acceleration, combined with a simple model for the energy losses and sputtering of the shock accelerated grains, result in an enhancement (relative to hydrogen) of volatile elements which is an increasing function of mass, and a net, nearly mass-independent enhancement of refractory elements. The relatively high abundances of C, O are accounted for since these elements are partially locked in grains and/or have a Wolf-Rayet contribution. The high H/He ratio may indicate the role of weak shocks. Furthermore, our shock accelerated spectra are consistent with observed spectra below the `knee' if a fairly steep rigidity dependent escape (i.e., ~R^{0.65}) from the galaxy is assumed.

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