Explosive volcanism and the compositions of cores of differentiated asteroids

Details Explosive volcanism and the compositions of cores of differentiated asteroids Explosive volcanism and the compositions of cores of differentiated asteroids

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993e%26psl.117..111k&link_type=abstract

Earth and Planetary Science Letters (ISSN 0012-821X), vol. 117, no. 1-2, p. 111-124.

Computer Science

35

Asteroids, Iron Meteorites, Meteoritic Composition, Planetary Cores, Volcanology, Magma, Trace Elements, Asteroids, Core, Differentiation, Volcanism, Explosions, Composition, Parent Bodies, Meteorites, Iron Meteorites, Crystallization, Buoyancy, Magma, Melts, Sulfur, Depletion, Hypotheses, Origin, Formation, Size, Model, Theoretical Studies, Pressure, Calculations, Partial Melting, Gases, Transport, Surface, Fractional Crystallization

Scientific paper

Eleven iron meteorite groups show correlations between Ni and siderophile trace elements that are predictable by distribution coefficients between liquid and solid metal in fractionally crystallizing metal magmas. These meteorites are interpreted to be fragments of the fractionally crystallized cores of eleven differentiated asteroids. Many of these groups crystallized from S-depleted magmas which we propose resulted from removal of the first partial melt (the Fe,Ni-FeS cotectic melt) by explosive pyroclastic volcanism of the type envisaged by Wilson and Keil (1991). We show that these dense, negatively buoyant melts can be driven to asteroidal surfaces due to the presence of excess pressure in the melt and the presence of buoyant bubbles of gas which decrease the density of the melt. We also show that, in typical asteroidal materials, veins will form which grow into dikes and serve as pathways for migration of melt and gas to asteroidal surfaces. Since cotectic Fe, Ni-FeS melt consists of about 85 wt pct FeS and 15 wt pct Fe, Ni, removal of small volumes of eutectic melts results in major loss of S but only minor loss of Fe,Ni, thus leaving sufficient Fe,Ni to form sizeable asteroidal cores.

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