Physics
Scientific paper
Jul 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....4.2249w&link_type=abstract
Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I
Physics
Scientific paper
The source of galactic cosmic-ray nuclei is unknown, but there is a general consensus that galactic cosmic rays are accelerated by supernova shocks in the interstellar medium. The evidence in support of this picture is strong but indirect. However, the fact that the cosmic-ray spectrum extends continuously, without steps or peaks, to more than five orders of magnitude in energy beyond the limit of supernova shock acceleration appears to be incompatible with this picture, at least without extreme fine-tuning of models. A "smoking gun" is needed to definitively establish that supernova shocks are indeed the accelerator of galactic cosmic rays. If galactic cosmic rays are accelerated in supernova shocks, they will be enhanced in freshly-synthesized r-pro cess material. We are currently studying the R-pro cess Isotop e Observer (RIO) as a Mission of opportunity for the International Space Station. RIO will make the first measurements of the isotopic abundances of the "ultraheavy" galactic cosmic rays (those in the range 32 ≤ Z ≤ 42) and will determine the fractional contribution of freshly-synthesized r-pro cess material in galactic cosmic rays through the measurement of several key isotopic ratios.
Weaver Benjamin A.
Westphal Andrew J.
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