The role of H2O in Martian magmatic systems

Amer. Mineral.,
83, 942-947, 1998

Bjorn O. Mysen Ý ,
David Virgo Ý,
Robert K. Popp *, and Constance M. Bertka Ý

Ý Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Rd., NW, Washington DC 20015-1305, USA

* Department of Geology and Geophysics Texas A&M University, College Station TX 77843

Abstract

We have estimated the water content of the interior or Mars by employing analyzed water contents of kaersutite inclusions from SNC meteorites in conjunction with an experimentally-derived crystal-chemical model of kaersutite amphibole. This model predicts quantitatively the relationships between iron oxidation and hydrogen deficiency in the kaersutite. The H2O contents of the magma from which the kaersutites in SNC meteorites could have crystallized is in the 100-1000 ppm range. That H2O content leads to an estimated water content of 1-35 ppm for a Martian mantle that could have been the source rock for such magmas.

SCOPE OF RESEARCH INTERESTS	RESEARCH INTERESTS	CURRENT RESEARCH ACTIVITIES
ABSTRACTS (LIST)	SCIENTIFIC PUBLICATIONS

[1], [2], [3], [4],
[5], [6], [7], [8], [9], [10], [11], [12], [13], [14], [15], [16], [17], [18],
[19], [20], [21], [22], [23], [24], [25]

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Email: mysen@gl.ciw.edu