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The Abundance and Isotopic Composition of Water in Howardite-Eucrite-Diogenite Meteorites

Volatile elements play a fundamental role in planetary formation and evolution through their influence on melting, silicate melt viscosity, magma crystallization and erup-tion processes [1]. The Howardite-Eucrite-Diogenite (HED) suite of meteorites represents the largest suite of crustal rocks available from a differentiated basaltic asteroid and account for between 2-3% of all meteorites collected globally [2]. Apatite is a widely distributed mineral, albeit in trace amounts, in planetary materials which acts as a recorder of vola-tile abundances in magmas and magmatic source regions [3] and is the most common volatile-bearing phase in lunar rocks [4, 5] and eucrites [3]. We are currently undertaking a detailed study of apatite in HED meteorites using Secondary Ion Mass Spectrome-try (SIMS) techniques to better constrain the volatile inventory and evolutionary history of their putative parent body, 4 Vesta [6, 7].