26Al, 244Pu, 50Ti,REE, and trace element abundances in hibonite grains from CM and CV meteorites |
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| Institution: | 1. Institut für Planetologie, University of Münster, Wilhelm-Klemm-Straße 10, Münster D-48149, Germany;2. Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, Göttingen D-37077, Germany;3. Centre de recherches pétrographiques et géochimiques (CRPG), CNRS, UMR 7358, F-54000, Nancy, France |
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| Abstract: | The ion microprobe was used to measure Ti and Mg isotopes as well as rare earth and other trace elements in ten hibonites from the CM carbonaceous chondrites Murchison, Murray, and Cold Bokkeveld and in two hibonites and Ti-rich pyroxene from the CV chondrite Allende. In hibonites from Murchison and Murray fission track densities were also measured, as were Th and U concentrations. Eight of the hibonites, from all four meteorites, exhibit large Ti isotopic anomalies, particularly in 50Ti. Two grains from Murray have 50Ti excesses of ~ 10%. At least four nucleosynthetic components are required to account for all the Ti isotopic data. Neutron-rich nuclear statistical equilibrium nucleosynthesis is the most likely process to account for a 50Ti-rich component (with ). The ion probe Ti isotopic measurements confirm that the solar nebula was isotopically heterogeneous on a small spatial scale and argue for a chemical memory origin of the Ti isotopic anomalies which were probably carried into the solar system in the form of refractory dust grains. However, there is no experimental evidence that such interstellar grains survived the formation of the hibonites. The REE and trace element patterns of the hibonites are similar to those seen in CAIs and can be interpreted in terms of fractionation effects during condensation from a gas of solar composition, thus arguing for a solar system origin of the hibonites. Additional evidence for such an origin is provided by the ratios, which are ~ 10−4, and by the Mg isotopic compositions which are normal except for 26Mg1 due to 26Al.Only three out of ten hibonites exhibit 26Mg1, consistent with previous studies which demonstrated the paucity of 26Mg1 in hibonites. Because of the refractory nature of hibonite and the presence of large Ti isotopic effects, we conclude that a heterogeneous distribution of 26Al in the early solar system is the most likely reason. In particular, our observations of δ50Ti = 15%. and of an isochron with ( in the FUN inclusion HAL are evidence against both late formation and Mg redistribution to explain the lack of 26Al in hibonites.There are no obvious correlations between the Ti isotopic compositions, the presence of 26Mg1, the presence of 244Pu, and the REE and trace element patterns in individual hibonites. This indicates that the anomalous 50Ti, as well as 26A1 and 244Pu, were not co-produced in a single astrophysical source, and/or that these nuclides were introduced into the solar nebula by different carriers before being incorporated into the hibonites. |
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