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Mantle Melting as a Function of Water Content beneath the Mariana Arc

Kelley, Katherine A. and Plank, Terry and Newman, Sally and Stolper, Edward M. and Grove, Timothy L. and Parman, Stephen and Hauri, Erik H. (2010) Mantle Melting as a Function of Water Content beneath the Mariana Arc. Journal of Petrology, 51 (8). pp. 1711-1738. ISSN 0022-3530. https://resolver.caltech.edu/CaltechAUTHORS:20100809-135251204

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Abstract

Subduction zone magmas are characterized by high concentrations of pre-eruptive H_2O, presumably as a result of an H_2Oflux originating from the dehydrating, subducting slab. The extent of mantle melting increases as a function of increasing water content beneath back-arc basins and is predicted to increase in a similar manner beneath arc volcanoes. Here, we present new data for olivine-hosted, basaltic melt inclusions from the Mariana arc that reveal pre-eruptive H_2O contents of ~1•5-6•0 wt %, which are up to three times higher than concentrations reported for the Mariana Trough back-arc basin. Major element systematics of arc and back-arc basin basalts indicate that the back-arc basin melting regime does not simply mix with wet, arc-derived melts to produce the observed range of back-arc magmatic H_2O concentrations. Simple melting models reveal that the trend of increasing extents of melting with increasing H_2O concentrations of the mantle source identified in the Mariana Trough generally extends beneath the Mariana volcanic front to higher mantle water contents and higher extents of melting. In detail, however, each Mariana volcano may define a distinct relationship between extent of melting and the H_2O content of the mantle source. We develop a revised parameterization of hydrous melting, incorporating terms for variable pressure and mantle fertility, to describe the distinct relationships shown by each arc volcano. This model is used in combination with thermobarometry constraints to show that hydrous melts equilibrate at greater depths (34-87 km) and temperatures (>1300°C) beneath the Mariana arc than beneath the back-arc basin (21-37 km), although both magma types can form from a mantle of similar potential temperature (~1350°C).The difference lies in where the melts form and equilibrate. Arc melts are dominated by those that equilibrate within the hot core of the mantle wedge, whereas back-arc melts are dominated by those that equilibrate within the shallow zone of decompression melting beneath the spreading center. Despite higher absolute melting temperatures (>1300°C), Mariana arc melts reflect lower melt productivity as a result of wet melting conditions and a more refractory mantle source.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/petrology/egq036DOIArticle
http://petrology.oxfordjournals.org/cgi/content/abstract/51/8/1711PublisherArticle
ORCID:
AuthorORCID
Newman, Sally0000-0003-0710-995X
Stolper, Edward M.0000-0001-8008-8804
Hauri, Erik H.0000-0002-7449-4774
Additional Information:© The Author 2010. Published by Oxford University Press. Received December 4, 2009; accepted June 10, 2010; advance access publication July 3, 2010. Thanks go to Fred Anderson for his great generosity in sharing his Mariana arc scoria collection with us. Many thanks also go to Neel Chatterjee at MIT and Chris Hadidiacos at GL/CIW for essential assistance with electron microprobe operations, and to Jianhua Wang at DTM/CIW for essential support with SIMS analyses. Marc Hirschmann, Charlie Langmuir, Rich Katz, Mark Behn and Liz Cottrell provided inspirational and progressive discussion over the course of this work. We are grateful to Paul Asimow, Jon Blundy, Julian Pearce and Paul Wallace for detailed, thoughtful and constructive reviews.
Issue or Number:8
Record Number:CaltechAUTHORS:20100809-135251204
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20100809-135251204
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:19347
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:09 Aug 2010 21:16
Last Modified:03 Oct 2019 01:55

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