Germanium and lead: Significant differences between meteoritic and photospheric abundances?

Details Germanium and lead: Significant differences between meteoritic and photospheric abundances? Germanium and lead: Significant differences between meteoritic and photospheric abundances?

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....3....5g&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 3 p 5-8 (SEE N85-34862 23-93)

Computer Science

1

Abundance, Cosmic Rays, Galactic Radiation, Germanium, Ionization Potentials, Lead (Metal), Radiation Sources, Carbonaceous Chondrites, Heavy Elements, Interstellar Matter, Mass Distribution, Metallic Stars, Potential Energy, Stellar Atmospheres

Scientific paper

The order of the Galactic cosmic ray source (GCRS) composition in terms of first ionization potential (FIP) was examined. For most elements, the degree of volatility is (positively) correlated with the value of the FIP, so that it is not easy to distinguish a correlation of GCRS abundances anomalies with FIP from a correlation with volatility. Only a few permit to distinguish between the two kinds of ordering: if they are depleted relative to refractory metals, volatility must be relevant, if not, FIP is relevant. Among them Cu and Zn would seem to favor FIP. Among the best indicators are Ge and Pb. The abundance anomalies in GCRS are defined relative to a standard which, for the heavy elements concerned, is commonly taken as C1 Carbonaceous Chondrites. Photospheric abundances are more directly representative of the protosolar nebula, and hence of ordinary local galactic (LG) matter. The Ge and Pb reference abundance determinations in the Photosphere and in C1 meteorites are examined and their relevance to the problem with FIP vs. volatility in GCRs is discussed.

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