Source composition of cosmic rays at energies 1-1000 TeV per nucleon

Details Source composition of cosmic rays at energies 1-1000 TeV per nucleon Source composition of cosmic rays at energies 1-1000 TeV per nucleon

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363..265s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 1, 1990, p. 265-269. Research supported by NATO and U.S. Navy.

Astronomy and Astrophysics

Astrophysics

19

Cosmic Rays, Cosmochemistry, Nuclear Astrophysics, Nucleons, Supernovae, Abundance, Acceleration (Physics), Astronomical Models, Nuclear Fusion, Stellar Winds, Wolf-Rayet Stars

Scientific paper

A model is developed for deriving the source composition of cosmic rays at energies 10 to the 12th - 10 to the 15th eV per nucleon. The model is based on the acceleration theory of Voelk and Biermann and on the nucleosynthesis processes in presupernova stars, i.e., red and blue supergiants and of the Wolf-Rayet (WR) stars. Very strong shock waves in a young supernova remnant accelerate the wind particles of the presupernova star to energies up to 10 to the 15th eV per nucleon. The winds of these stars contain the nucleosynthesis products of the CNO cycle and of helium burning. Hence, the high-energy cosmic rays should be enriched in these products when compared with the cosmic rays at energies below 10 to the 12th eV per nucleon. Observational data on the 'arriving' abundances greater than 1 TeV per nucleon, while still scanty, support such enrichment of He, C, and O relative to H, Mg, and Si. Tests are outlined for the possibility that acceleration at old supernova remnants becomes inefficient above 10 to the 14th eV per nucleon, and for the possible contribution of neutron-star surface material to Fe at E not less than 10 to the 15th eV per nucleon.

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