Formation of eucrites and diogenites on a Vesta-sized asteroid. I - Core formation

Details Formation of eucrites and diogenites on a Vesta-sized asteroid. I - Core formation Formation of eucrites and diogenites on a Vesta-sized asteroid. I - Core formation

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28.1177r&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 179.

Computer Science

2

Vesta Asteroid, Planetary Cores, Planetary Evolution, Chondrites, Planetary Mantles, Chemical Composition, Melting, Planetary Composition

Scientific paper

Core formation in asteroid-sized planetesimals occurred early (less than 15 Ma after T(0)) as has been recently demonstrated using W-182/W-184 ratios. Depletion of siderophile elements in the mantle of the HED parent body has been cited as evidence that metal had segregated into a core before the eucrites formed. Calculations and experiments indicate that large degrees of melting are required to efficiently separate metal from silicate. Given the siderophile element data, it seems necessary to have large amounts of melting on a Vesta-sized body in order to facilitate core formation. The high temperatures necessary to melt a chondritic mantle could be provided early by the decay of Al-26 to Mg-26 and Fe-60 to Ni-60, by a hot T Tauri or FU Orionis stage, or a superluminous sun. We examined the issue of core formation in a CI chondritic HED parent body by considering siderophile element partitioning during metal-silicate equilibrium at high temperatures. Here we extend this work to investigate the effect of bulk composition by considering CM, CO, CV, H, L, and LL chondritic starting materials.

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