Physics
Scientific paper
Jul 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999m%26ps...34..625i&link_type=abstract
Meteoritics & Planetary Science, vol. 34, no. 4, pp. 625-636 (1999).
Physics
3
Scientific paper
The Asuka-881931 meteorite is an unbrecciated ferroan ureilite, and consists mainly of equigranular olivine and pigeonite grains, metal-sulfide network, interstitial silicates, and glass. Peripheral portions of equigranular olivine grains are often replaced by fine-grained forsterite-metal aggregates and sometimes by fine-grained enstatite-metal aggregates. These aggregates may have been produced from the equigranular olivine by reduction. Peripheral portions of equigranular pigeonite grains also are sometimes replaced by fine-grained orthopyroxene aggregates with tiny patches of Si-rich glass, and may have been produced from the pigeonite by reduction reaction with silicate melt. Interstitial silicates are mainly orthopyroxene, magnesian pigeonite, high-Ca pyroxene (diopside/fassaite), and CaO-poor enstatite, and they crystallized from interstitial silicate melt. Interstitial glass is classified into two types, Si-poor and Si-rich. The Si-poor glass is always in contact with equigranular olivine, but the Si-rich glass never contacts equigranular olivine and is in contact with pyroxene and metal-sulfide network. Both types of glass were produced from an original interstitial silicate melt, but the Si-poor glass formed mainly by fractional crystallization of pyroxenes, and the Si-rich glass may have formed by addition of Si mainly from nearby metal-sulfide melt, as well as crystallization of pyroxenes. The Si-poor and Si-rich melts were finally quenched as interstitial glasses under a rapid cooling condition.
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