Endogenic modification in lunar floor-fractured craters can constrain spatial variations in early lunar conditions. The nature of these constraints, however, depends on the assumed mechanism of crater modification. For viscous relaxation, the extent of crater modification depends on the surrounding crustal viscosity and thus provides loose constraints on the history of crustal heating within a ...

clinopyroxene phenocrysts and microphenocrysts in potassic and sodic eosen alkaline volcanic rocks from the northern lahrud (nw iran) record various stages in the crystallization and evolution history of the alkaline melt as well as its origin. the rock series hosting the clinopyroxene phenocrysts is phonolitic tephrite and tephritic phonolite composition. theses rocks generally show porphyriti...

The Bushveld Complex formed by the crystallization of successive basaltic magmatism may be of the order of several million years. For example, the Columbia River Basalts (Hooper, injections of magma, which were sufficiently closely spaced in time that each previous magma had not cooled and differentiated 1988) were erupted in the period 17–12 Ma, with minor eruptions for a further 5 my, althoug...

BASALTS: MAGMA OCEAN DIFFERENTIATION AND SOURCE HETEROGENEITY. L.J. Hallis, R.C. Greenwood, M. Anand, S.S. Russell, M. F. Miller and I. A. Franchi. [email protected]. Department of Mineralogy, The Natural History Museum, Cromwell Rd, London, SW7 5BD, UK. Dept. of Earth and Environmental Sciences, The Open University, Milton Keynes MK7 6AA, UK. PSSRI, The Open University, Milton Keynes MK7 6AA,...

Introduction: A wide variety of morphologic features representing a range of eruption styles has been documented on the Moon [e.g., 1-2]. We have characterized the nature of numerous steep-sided domes, small shields, cones, dark halo craters of internal origin, dark mantle deposits, linear rille-related deposits, and sinuous rille-related deposits on the Moon using Clementine multis-pectral, Ap...

Introduction: Nakhlites are olivine-augite cumulates that formed in flows or shallow intrusions of basaltic magma on Mars [1]. There have been at least 6 independent attempts to determine the composition of the Nakhla parent magma, and at least 14 variants have been published [2-12]. Four distinct methods have been used: 1) mass balance; (2) augite/melt element partitioning; 3) melt inclusions ...