First Ionization Potential vs. Volatility in Galactic Cosmic Rays

Details First Ionization Potential vs. Volatility in Galactic Cosmic Rays First Ionization Potential vs. Volatility in Galactic Cosmic Rays

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aps..aprw16006g&link_type=abstract

American Physical Society, April Meeting, April 29-May 2, 2000 Long Beach, CA, abstract #W16.006

Physics

Scientific paper

The observed abundances of galactic cosmic rays reflect the composition of the pool of source material from which the particles are accelerated as well as the effects of propagation through the Galaxy en route to Earth. Careful modeling of the galactic transport suggests that the source composition is remarkably similar to that of our own solar system but with a fractionation which depends on chemical properties such as the first ionization potential (FIP). An alternative ordering parameter might be the condensation temperature, or volatility, which is generally correlated with FIP. A convincing indication that one of these is the correct parameter would have strong implications for models of the origin and acceleration of galactic cosmic rays. Seven elements below Z=34, (Na, P, S, Cu, Zn, Ga, Ge), have been identified as being potentially useful for distinguishing between FIP and volatility fractionation with varying degrees of discriminating power. New measurements of these elements from the Cosmic Ray Isotope Spectrometer (CRIS) instrument on board the Advanced Composition Explorer (ACE) spacecraft will be used to provide new estimates of the source abundances of these elements in the context of an updated leaky box propagation model.

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