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

  title={Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites},
  author={Joel A. Baker and Martin Bizzarro and Nadine Wittig and James N. Connelly and Henning Haack},
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… 
Rapid Timescales for Accretion and Melting of Differentiated Planetesimals Inferred from 26Al-26Mg Chronometry
Constraining the timescales for the assembly and differentiation of planetary bodies in our young solar system is essential for a complete understanding of planet-forming processes. This is best
Iron meteorites as remnants of planetesimals formed in the terrestrial planet region
It is shown that the iron-meteorite parent bodies most probably formed in the terrestrial planet region, and it is predicted that some asteroids are main-belt interlopers and a select few may even be remnants of the long-lost precursor material that formed the Earth.
Timing and Origin of the Angrite Parent Body Inferred from Cr Isotopes
Angrite meteorites are some of the oldest materials in the solar system. They provide important information on the earliest evolution of the solar system and accretion timescales of protoplanets.
Chronology of the Solar System’s Oldest Solids
Determining the origins of our solar system and, by proxy, other planetary systems, depends on knowing accurately and precisely the timing and tempo of the transformation of the disk of gas and dust
26Al–26Mg dating of asteroidal magmatism in the young Solar System
Evidence for a Late Supernova Injection of 60Fe into the Protoplanetary Disk
Decoupling the first appearance of 26Al and 60Fe constrains the environment where the Sun's formation could have taken place, indicating that it occurred in a dense stellar cluster in association with numerous massive stars.
Chondrules and the Protoplanetary Disk
AbstractMajor advances in deciphering the record of nebula processes in chondrites can be attributed to analytical improvements that allow coordinated isotopic and mineralogical studies of components
Multiple and fast: the accretion of ordinary chondrite parent bodies
Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and


Mg isotope evidence for contemporaneous formation of chondrules and refractory inclusions
The presence of excess 26Mg resulting from in situ decay of the short-lived 26Al nuclide in CAIs and chondrules from the Allende meteorite is reported, indicating that Allende chondrule formation began contemporaneously with the formation of CAIs, and continued for at least 1.4 Myr.
A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites
Measurements of tungsten isotope compositions and hafnium–tungsten ratios of several meteorites indicate that the bulk of metal–silicate separation in the Solar System was completed within <30 Myr, completely consistent with other evidence for rapid planetary formation.
Early solar system events and timescale
— Some recent information on the Mn-Cr and Al-Mg systems is reviewed. This information is used to derive constraints on the timing of processes and events, which took place in the early solar system.
Constraints on the Origin of Chondrules and CAIs from Short-lived and Long-lived Radionuclides
The high time resolution Pb-Pb ages and short-lived nuclide based relative ages for CAIs and chondrules are reviewed. The solar system started at 4567.2 {+-} 0.6Ma inferred from the high precision
Timescales for planetary accretion and the structure of the protoplanetary disk