Early planetesimal melting from an age of 4.5662Gyr for differentiated meteorites

Details Early planetesimal melting from an age of 4.5662Gyr for differentiated meteorites Early planetesimal melting from an age of 4.5662Gyr for differentiated meteorites

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005natur.436.1127b&link_type=abstract

Nature, Volume 436, Issue 7054, pp. 1127-1131 (2005).

Physics

67

Scientific paper

Long- and short-lived radioactive isotopes and their daughter products in meteorites are chronometers that can test models for Solar System formation. Differentiated meteorites come from parent bodies that were once molten and separated into metal cores and silicate mantles. Mineral ages for these meteorites, however, are typically younger than age constraints for planetesimal differentiation. Such young ages indicate that the energy required to melt their parent bodies could not have come from the most likely heat source-radioactive decay of short-lived nuclides (26Al and 60Fe) injected from a nearby supernova-because these would have largely decayed by the time of melting. Here we report an age of 4.5662 +/- 0.0001billion years (based on Pb-Pb dating) for basaltic angrites, which is only 1Myr younger than the currently accepted minimum age of the Solar System and corresponds to a time when 26Al and 60Fe decay could have triggered planetesimal melting. Small 26Mg excesses in bulk angrite samples confirm that 26Al decay contributed to the melting of their parent body. These results indicate that the accretion of differentiated planetesimals pre-dated that of undifferentiated planetesimals, and reveals the minimum Solar System age to be 4.5695 +/- 0.0002billion years.

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