The effects of oxygen fugacity and sulfur on the pressure of vapor-saturation of magma
Abstract
Geobarometers are commonly used to determine the pressure (and hence depth) of magmatic bodies. For instance, at equilibrium, the concentration of dissolved volatiles in a vapor-saturated melt can be used as a barometer: this is the pressure of vapor-saturation (Pₛₐₜ^𝜈). Most determinations of Pₛₐₜ^𝜈 assume that melt and vapor contain only oxidized C-O-H species. However, sulfur is the third most abundant volatile element in magmas, and oxygen fugacity (fO2) exerts a strong influence on the speciation of the melt and vapor. To explore how S and fO2 affect calculations of Pₛₐₜ^𝜈, we model a Hawaiian tholeiite that contains both reduced and oxidized C-O-H-S species in the melt and vapor. We find that excluding reduced C-O-H species in the system can result in significant underestimations of Pₛₐₜ^𝜈 under reducing conditions (ΔFMQ < 0). The effect of S on Pₛₐₜ^𝜈 is small except in the vicinity of the “sulfur solubility minimum” (SSmin; 0 < ΔFMQ < +2), where excluding S-bearing species can result in underestimates of Pₛₐₜ^𝜈.
The implications of these results depend on the volatile concentration of the system being investigated, its fO2, and the melt composition and temperature. Our results suggest there will be little impact on Pₛₐₜ^𝜈 calculated for mid-ocean ridge basalts because their fO2 is above where reduced C-O-H species become important in the melt and vapor and yet below the SSmin. However, the fO2 of ocean island and arc basalts are close enough to the SSmin and their S concentrations high enough to influence Pₛₐₜ^𝜈. However, high-CO2 and high-H2O concentrations are predicted to reduce the effect of the SSmin. Hence, Pₛₐₜ^𝜈 calculated for shallowly trapped melt inclusions and matrix glass are more affected by the SSmin than deeply trapped melt inclusions. Lunar and martian magmas are typically more reduced than terrestrial magmas, and therefore accurate Pₛₐₜ^𝜈 calculations for them require the inclusion of reduced C-O-H species.
Copyright and License
© 2024 Mineralogical Society of America.
Acknowledgement
We thank Kayla Iacovino and an anonymous reviewer for their helpful comments that greatly improved the paper, and Justin Filiberto for their editorial handling of the paper. E.C.H. was funded by a Caltech Geology Option Post-Doctoral Fellowship and a Caltech Centre for Comparative Planetary Evolution (3CPE) research grant and is supported by the New Zealand Ministry of Business, Innovation and Employment (MBIE) through the Hazards and Risk Management and New Zealand Geothermal Futures programme (Strategic Science Investment Fund, contract C05X1702). P.L. is funded by an Embiricos Trust scholarship from Jesus College, University of Cambridge.
Data Availability
Files
Name | Size | Download all |
---|---|---|
md5:cf09399aae671a9654610411f184d8c1
|
2.4 MB | Download |
md5:5215775d90c3d9e0322a2ee6272258d5
|
9.4 MB | Download |
md5:e52cefa6aff387dd032841758507dd54
|
11.6 MB | Preview Download |
Additional details
- ISSN
- 1945-3027
- California Institute of Technology
- Postdoctoral Fellowship Division of Geological and Planetary Sciences
- California Institute of Technology
- Caltech Center for Comparative Planetary Evolution
- Ministry of Business, Innovation and Employment
- C05X1702
- University of Cambridge
- Embiricos Trust
- Caltech groups
- Division of Geological and Planetary Sciences, Caltech Center for Comparative Planetary Evolution