Ascent and eruption of a lunar high-titanium magma as inferred from the petrology of the 74001/2 drill core
Article first published online: 4 FEB 2010
1999 The Meteoritical Society
Meteoritics & Planetary Science
Volume 34, Issue 4, pages 527–540, July 1999
How to Cite
WEITZ, C. M., RUTHERFORD, M. J., III, J. W. H. and McKAY, D. S. (1999), Ascent and eruption of a lunar high-titanium magma as inferred from the petrology of the 74001/2 drill core. Meteoritics & Planetary Science, 34: 527–540. doi: 10.1111/j.1945-5100.1999.tb01361.x
- Issue published online: 4 FEB 2010
- Article first published online: 4 FEB 2010
- Received 1998 August 13; accepted in revised form 1999 February 10
Abstract— An analysis of the orange glasses and crystallized beads from the 68 cm deep 74001/2 core has been conducted to understand the processes occurring during ascent and eruption of the Apollo 17 orange glass magma. Equilibrium between melt and metal blebs (Fe85Ni14Co1) within the core, along with Cr contents in olivine phenocrysts, suggest there was an oxidation of C and a reduction of the melt at an O fugacity of IW-1.3 and 1320 °C to form CO gas at 200 bars or ∼4 km depth. This was followed by development of more oxidized conditions during ascent. Also during ascent, there was formation of euhedral, homogeneous Fo81 olivine crystals and spinel crystals with higher Al and Mg contents than the smaller spinels in the crystallized beads. Both the metal blebs and Al-rich spinels were trapped inside the Fo81 olivine phenocrysts as they grew prior to eruption. The composition of the orange glasses are homogeneous throughout the core, except for a few distinct glasses at the top that appear to have been mixed in by micrometeorite reworking. A few glassy melt inclusions of orange glass composition trapped in the Fo81 phenocrysts contain 600 ± 100 ppm S and ∼50 ppm Cl compared to the 200 ppm S and 50 ppm Cl in the orange glass melt when quenched. These inclusions therefore document the addition of 400 ppm S to the CO-rich volcanic gas during the eruption.
The size and distribution of different volcanic beads in the Apollo 17 deposit indicate a mode of eruption in which the orange glasses and partially crystallized beads formed further away from the volcanic vent where cooling rates were faster. Progressively larger and more numerous crystals in the black beads reflect slower cooling rates at higher optical densities in the volcanic plume. The development of a brown texture in the orange glasses at the bottom of the core, where the black beads dominate, is interpreted to result from devitrification by subsolidus heating either as the orange glasses fell back through the hot plume or after deposition on the surface. The change from domination by orange glasses to black beads in the core probably reflects a decrease in gas content over time, which consequently would increase the plume optical density and favor slower cooling rates.