Other
Scientific paper
Jul 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992metic..27q.223g&link_type=abstract
Meteoritics, vol. 27, no. 3, volume 27, page 223
Other
2
Scientific paper
The production of krypton isotopes from target elements Rb (Rb2SO4), Sr (SrF2), Y, Zr and of xenon in Ba (Ba glass), La (LaF2) have been studied in a simulation experiment. This investigation is part of the experiment LNS 172 by which a 50-cm- diameter artificial meteoroid (gabro) was isotropically irradiated at SATURNE with 1.6-GeV protons to simulate the galactic cosmic ray proton bombardement of meteoroids in space (Michel et al, 1991). More than 1400 individual targets consisting of pure elements, suitable chemical compounds, natural minerals and degassed meteoritic materials, were located at various depths in the artificial meteoroid. In this work, depth profiles for the production of Kr and Xe isotopes are measured by conventional mass spectrometry. In order to interpret the experimental data, the depth dependant spectra of primary and secondary particles is calculated in the artificial meteoroid by Monte Carlo techniques using the Hermes code system (Cloth et al., 1988). From these spectra, theoretical production depth profiles are derived on the basis of experimental (when available) or calculated thin-target excitation functions. New thin-target cross sections for radionuclides and for Kr and Xe isotopes in Rb, Sr, Y, Zr are also measured in order to enhance the cross section database and to get information to what quality depth profiles can be explained by the model calculations for these target mass regions. The elemental production rates and the production rate ratios are analyzed versus shielding depth. Empirical correlations between different cosmogenic nuclides such as Kr and Xe isotopes versus e.g. ^22Ne/^21Ne are discussed and compared with the calculated and with the measured depth profiles in the St Severin chondrite (Lavielle and Marti, 1988). From preliminary results, the ^83Kr production rate in Y increases by ~50% with shielding depth from the surface to the center of the sphere. Analysis of the other target elements is still in progress. REFERENCES: Cloth et al.(1988), Juel-2203; Lavielle B. and Marti K. (1988) Proc. Lunar Planet. Sci. 18th, 565-572; Michel et al., (1991) Meteoritics 26, 372a.
Gilabert Eric
Herpers Ulrich
Lavielle Bernard
Lupke M.
Michel Rigo
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