Physics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusm.v31a..03h&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #V31A-03
Physics
5410 Composition (1060, 3672), 5430 Interiors (8147), 1015 Composition Of The Core, 1027 Composition Of The Planets, 1060 Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008)
Scientific paper
The existence of iron meteorites indicates that core formation began in bodies as small as several kilometers due to low pressure melting from heat supplied by the decay of radioactive isotopes. Therefore, the terrestrial planets would be accreted from previously differentiated material. Much of this material could have moved to the center of the planet at the embryo-planet formation stage to form a growing core through percolation and compaction without losing its low-pressure partitioning signature. It is generally thought that the core formation of terrestrial planets such as the Earth involved a magma ocean where metal-silicate equilibration occurred at high pressure in order to explain the observed siderophile element depletions in the Earth's upper mantle. This indicates that the cores of terrestrial planets may be formed from a combination of material: earlier material that equilibrated at low pressures along with later material that equilibrated in deep magma oceans at high pressure. Such core formation process would lead to distinct geochemical signatures dependent on the size of the embryo-planet core formed by the low-pressure process and the pressure dependence of metal-silicate partition coefficients. We have developed models to examine how the overall partitioning signature seen in the modern terrestrial planetary mantles would be affected by this type of multistage partitioning process.
Fei Yingwei
Hier-Majumder C. A.
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