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• W81133239 abstract "Introduction: Presolar SiC grains form in a variety of types of stars, including asymptotic giant branch (AGB) red giant stars and supernovae. The dominant mechanisms of heavy element nucleosynthesis, the s-process and r-process, are thought to occur mainly in AGB stars and supernovae, respectively [1]. We have previously reported that mainstream SiC grains have strong enrichments in the s-process isotopes of Sr, Zr and Mo [2Ð5], which is consistent with an origin in AGB stars. We report here the isotopic compositions of Mo and Zr in X-type SiC grains, which have previously been identified as having formed from supernova ejecta. Experimental methods: SiC X-grains were identified in a mount containing ~1400 grains of Murchison SiC grain size separate KJG (~3 mm) by ion imaging [6] with an ion microprobe. The C, N and Si isotopic compositions of all X-grains and a number of other SiC grains were measured by ion microprobe. The isotopic compositions of Mo and Zr in a number of grains were measured by laser ablation laser resonant ionization mass spectrometry [2Ð4]. Results and discussion: As we reported earlier [7], two X-grains are enriched in Mo and Mo compared to solar system values, rather than in Mo (as would have been expected from the r-process that contributed to solar system abundances). The Zr isotopic compositions of three Xgrains are shown in Fig. 1, along with one mainstream SiC grain measured in the same series of analyses. Two grains are strongly enriched in Zr (which is predominantly produced in the rprocess) and the third shows a significant enhancement in Zr with no other significant isotopic anomalies. These patterns contrast with those in mainstream grains, which are characterized by large depletions in Zr and small depletions in Zr, Zr and Zr. The most likely origin for r-process nuclides is neutron-rich matter dragged by neutrino winds from the nascent neutron star that results from a Type II supernova [1]. The Si and C in SiC Xgrains are likely to come from the O/Si, He/C and C/O-zones of the presupernova star. Thus, it is not clear that r-process matter should be found in Xgrains. Perhaps a neutron burst in the supernova zones where Si and C are made could have produced both the Mo and Zr isotopic patterns. Acknowledgements: This work was supported by the Department of Energy, BESMaterials Sciences and by NASA. References: [1]EWallerstein G. et al. (1997) Rev. Modern Phys., 69, 995Ð1084. [2]ENicolussi G. K. et al. (1997) Science, 277, 1281Ð1283. [3]ENicolussi G. K. et al. (1998) GCA, 62, 109Ð1104. [4] Nicolussi G. K. et al. (1998) Phys. Rev. Lett., 81, 3583Ð3586. [5] Davis A. M. et al. (1999) in Nuclei in the Cosmos V (ed. Prantzos N.), in press. [6] Nittler L. R. et al. (1995) Ap. J., 453, L25ÐL28. [7] Pellin M. J. et al. (1999) LPS XXX, #1969." @default.
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• W81133239 date "1999-07-01" @default.
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• W81133239 title "Molybdenum- and Zirconium-Isotopic Compositions of Supernova Grains" @default.
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