Meteoritics & Planetary Science 1–13 (2016) doi: 10.1111/maps.12624 Constraints on the water, chlorine, and fluorine content of the Martian mantle 1* 2,3 4 Justin FILIBERTO , Juliane GROSS , and Francis M. MCCubbin 1Department of Geology, Southern Illinois University, 1259 Lincoln Dr, MC 4324, Carbondale, Illinois 62901, USA 2Department of Earth and Planetary Sciences, Rutgers University, 610 Taylor Road, Piscataway, New Jersey 08854, USA 3Department of Earth and Planetary Sciences, The American Museum of Natural History, New York, New York 10024, USA 4NASA Johnson Space Center, Mail Code XI2, 2101 NASA Parkway, Houston, Texas 77058, USA *Corresponding author. E-mail: fi
[email protected] (Received 30 July 2015; revision accepted 22 January 2016) Abstract–Previous estimates of the volatile contents of Martian basalts, and hence their source regions, ranged from nearly volatile-free through estimates similar to those found in terrestrial subduction zones. Here, we use the bulk chemistry of Martian meteorites, along with Martian apatite and amphibole chemistry, to constrain the volatile contents of the Martian interior. Our estimates show that the volatile content of the source region for the Martian meteorites is similar to the terrestrial Mid-Ocean-Ridge Mantle source. Chlorine is enriched compared with the depleted terrestrial mantle but is similar to the terrestrial enriched source region; fluorine is similar to the terrestrial primitive mantle; and water is consistent with the terrestrial mantle. Our results show that Martian magmas were not volatile saturated; had water/chlorine and water/fluorine ratios ~0.4–18; and are most similar, in terms of volatiles, to terrestrial MORBs. Presumably, there are variations in volatile content in the Martian interior as suggested by apatite compositions, but more bulk chemical data, especially for fluorine and water, are required to investigate these variations.