Rapid Timescales for Magma Ocean Crystallization on the Howardite-Eucrite-Diogenite Parent Body

Details Rapid Timescales for Magma Ocean Crystallization on the Howardite-Eucrite-Diogenite Parent Body Rapid Timescales for Magma Ocean Crystallization on the Howardite-Eucrite-Diogenite Parent Body

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...740l..22s&link_type=abstract

The Astrophysical Journal Letters, Volume 740, Issue 1, article id. L22 (2011).

Astronomy and Astrophysics

Astronomy

5

Astrochemistry, Meteorites, Meteors, Meteoroids, Minor Planets, Asteroids: General, Protoplanetary Disks

Scientific paper

Asteroid 4 Vesta has long been postulated as the source for the howardite-eucrite-diogenite (HED) achondrite meteorites. Here we show that Al-free diogenite meteorites record variability in the mass-independent abundance of 26Mg (26Mg*) that is correlated with their mineral chemistry. This suggests that these meteorites captured the Mg-isotopic evolution of a large-scale differentiating magma body with increasing 27Al/24Mg during the lifespan of the short-lived 26Al nuclide (t 1/2 ~ 730,000 yr). Thus, diogenites and eucrites represent crystallization products of a large-scale magma ocean associated with the differentiation and magmatic evolution of the HED parent body. The 26Mg* composition of the most primitive diogenites requires onset of the magma ocean crystallization within 0.6-0.4 + 0.5 Myr of solar system formation. Moreover, 26Mg* variations among diogenites and eucrites imply that near complete solidification of the HED parent body occurred within the following 2-3 Myr. Thermal models predict that such rapid cooling and magma ocean crystallization could only occur on small asteroids (<100 km), implying that 4 Vesta is not the source of the HED meteorites.

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