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Provenance and Concentration of Water in the Shergottite MantleThe water content of the martian mantle is controversial. In particular, the role of water in the petrogenesis of the shergottites has been much debated. Although the shergottites, collectively, contain very little water [e.g., 1,2], some experiments have been interpreted to show that percent levels of water are required for the petrogenesis of shergottites such as Shergotty and Zagami [3]. In this latter interpretation, the general paucity of water in the shergottites and their constituent minerals is attributed to late-stage degassing. Y980459 (Y98) is a very primitive, perhaps even parental, martian basalt, with a one-bar liquidus temperature of approx.1400 C. Olivine is the liquidus phase, and olivine core compositions are in equilibrium with the bulk rock [e.g., 4]. Petrogenetically, therefore, Y98 has had a rather simple history and can potentially help constrain the role of water in martian igneous processes. In particular, once trapped, melt inclusions should not be affected by subsequent degassing.
Document ID
20120003056
Acquisition Source
Johnson Space Center
Document Type
Conference Paper
Authors
Jones, J. H. (NASA Johnson Space Center Houston, TX, United States)
Usui, T. (Lunar and Planetary Inst. Houston, TX, United States)
Alexander, C. M. O'D. (Carnegie Institution of Washington Washington, DC, United States)
Simon, J. I. (NASA Johnson Space Center Houston, TX, United States)
Wang, J. (Carnegie Institution of Washington Washington, DC, United States)
Date Acquired
August 25, 2013
Publication Date
March 19, 2012
Subject Category
Geophysics
Report/Patent Number
JSC-CN-25797
Meeting Information
Meeting: 43rd Lunar and Planetary Science Conference
Location: The Woodlands, TX
Country: United States
Start Date: March 19, 2012
End Date: March 23, 2012
Sponsors: Lunar and Planetary Inst.
Distribution Limits
Public
Copyright
Public Use Permitted.

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