Spectral properties of the Marius Hills volcanic complex and implications for the formation of lunar domes and cones

We have used multispectral data from the Clementine UV-visible camera to st udy the volcanic features of the Marius Hills complex and their comparison to other lunar domes and cones. There are several mare units identified in the complex, each with a unique Ti content, as indicated by their 415/750 n m value, The domes in Marius Hills are spectrally identical to the mare pla ins of the complex, supporting similar compositions. In contrast, most of t he volcanic cones. of the complex are lower in reflectance, bluer in color, and have weaker mafic absorptions than the mare and domes. The spectral ch aracteristics of the cones can best be explained by fine-grainad crystalliz ation in the spatter that compose the cones. Other lunar cones, such as Mon s Esam in northern Tranquillitatis, have spectral properties similar to tho se at Marius Hills. The Rima Parry cones and their associated dark mantle d eposit appear redder with a stronger mafic absorption than the Marius Hills cones. The cones Isis and Osiris in southern Mare Serenitatis, the domes o f Rumker Hills, and several domes in northern Mare Tranquillitatis are spec trally similar to adjacent mare units. The Mairan and Gruithuisen domes in northern Oceanus Procellarum have a feldspathic signature characteristic of highland material although they are redder and brighter than adjacent high land soils. They appear to represent highland material that resembles domes rather than actual mare domes, like those at Marius and Rumker Hills. The diversity of lunar volcanic features can best be explained by differences i n accumulation rates and cooling of ejected clasts from various eruption st yles. Mare domes may have formed at lower effusion rates, thereby allowing lava to construct small shields with slopes <3 degrees. The steeper domes a t Marius Hills require higher viscosities resulting from even lower effusio n rates and enhanced crystallization in the magmas during the terminal stag es of earlier eruptions that emplaced the mare. Cones like Mons Esam, Rima Parry, Isis, and Osiris are aligned along linear rilles and are interpreted to result from degassing of near-surface dikes. In contrast, the cones of Marius Hills show no linear alignment and may result from strombolian erupt ions at the terminal stages of earlier effusive eruptions that emplaced the domes and mare in the complex.