The origin of boninites on Mercury: An experimental study of the northern volcanic plains lavas

• Published in: Geochimica et cosmochimica acta Vol. 173; pp. 246 - 263
• Main Authors: Vander Kaaden, Kathleen E., McCubbin, Francis M.
• Format: Journal Article
• Language: English
• Published: Elsevier Ltd 15-01-2016
• ISSN: 0016-7037; 1872-9533
• DOI: 10.1016/j.gca.2015.10.016

Phase equilibrium experiments were conducted on a synthetic rock composition matching that of the northern volcanic plains of Mercury as measured by the MErcury Surface, Space ENvironment, GEochemistry and Ranging spacecraft (MESSENGER). The northern volcanic plains are smooth plains of suspected volcanic origin that cover more than 6% of the surface area of Mercury. The northern volcanic plains are less cratered than their surroundings and reported to be the product of flood volcanism, making them a prime candidate for experimental study. The bulk composition of the northern volcanic plains is that of an alkali-rich boninite and represents the first silica-enriched crustal terrane identified on an extraterrestrial planet from orbital data. Phase equilibrium experiments were conducted over the pressure range of the mercurian mantle (0.5–5GPa) at very low oxygen fugacity (∼ΔIW0 to −7) using a piston-cylinder apparatus (P 0.5–1.7GPa) and a Walker-style multi-anvil device (P⩾2.5GPa). Our results indicate the origin of the northern volcanic plains lavas (boninites) are best explained by high degrees of partial melting of an olivine-dominant, pyroxene- and plagioclase-bearing mantle source at low pressure (⩽1.4GPa) and does not require hydrous melting to achieve the silica-enriched melt composition. The formation mechanism for boninites on Mercury contrasts substantially with terrestrial boninites, which typically occur in oxidized and hydrous arc environments associated with subduction zones. Instead, mercurian boninites form at exceptionally low oxygen fugacity and do not require melting of hydrated source materials. The NVP lavas represent a novel mechanism by which planetary bodies can form silica-enriched secondary crusts without the aid of water.