Nuclear and chemical processes in the early solar system revealed by Zr, Mo, and Ru isotope abundances in iron meteorites

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We are investigating how meteorite parent bodies formed by examining the isotopic composition of elements in the molybdenum mass region. Meteorites are great archives of the history of the Solar System. Within the mineral matrix are subtle clues that tell us how long it took for the planets to form and under what conditions. The isotope composition of molybdenum in meteorites is a key to unlock the secrets of the origins and evolution of our Solar System. Molybdenum has seven stable isotopes formed by a variety of nuclear processes. The seven stable isotopes of molybdenum span a mass range from 92 to 100 atomic mass units. These nuclides were formed by a combination of rapid and slow neutron capture and proton capture nucleosynthesis as well as the decay of short-lived radioactive parents. Isotope abundance variations can be caused by changes in the redox environment and condensation of high-temperature magmatic fluids. We interpret these data to better understand the fractional crystallization of elements during the formation of the parent bodies. Isotope abundance anomalies are investigated to elucidate the sources of nucleosynthetic material to the early Solar System and establish the timing and duration of planetary formation. In addition, distinct isotope signatures and elemental concentrations are used to identify the genetic origins of meteorites.