HR: 0800h
AN: P11A-0949    [Abstracts]
TI: Lava Domes of the Arcadia Region of Mars
AU: * Rampey, M L
EM: mrampey@utk.edu
AF: Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, 306 Geological Sciences Bldg., Knoxville, TN 37996 United States
AU: Milam, K A
EM: kmilam@utk.edu
AF: Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, 306 Geological Sciences Bldg., Knoxville, TN 37996 United States
AU: McSween, H Y
EM: mcsween@utk.edu
AF: Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, 306 Geological Sciences Bldg., Knoxville, TN 37996 United States
AU: Moersch, J E
EM: jmoersch@utk.edu
AF: Planetary Geosciences Institute, Department of Earth and Planetary Sciences, University of Tennessee, 306 Geological Sciences Bldg., Knoxville, TN 37996 United States
AB: It is widely accepted that the volcanic rocks on the surface of Mars are basic to intermediate in composition. A few locations on Mars, however, have been considered by some workers as possibly consisting of silicic volcanic rocks, based primarily on morphologic considerations. If it could be demonstrated that silicic volcanism occurred on the surface of Mars then the poorly-differentiated, basic to intermediate crust model would have to be discarded in favor of a more magmatically diversified one. Past efforts at demonstrating the presence of silicic volcanic rocks at these locations, however, were thwarted by the lack of spatial and spectral resolution of the data available at the time. One of these locations, referred to in this study as the Tyndall Volcanic Field (TVF), in the western Arcadia Planitia region, possesses $>$ 600 small ($<$ 6 km diameter) edifices that morphologically resemble terrestrial lava domes. They consist of massive, steep-sided rock bodies, frequently partly covered by boulders, occasionally possessing what we interpret to be summit collapse features and crease structures and are usually surrounded by rock talus aprons. Curious, between-dome lineaments occur that are tentatively interpreted as being fissures. Our work uses Mars Orbiter Camera (MOC), Mars Orbiter Laser Altimeter (MOLA), Thermal Emission Spectrometer (TES) and Thermal Emission Imaging System (THEMIS) orbital imagery data to study the morphologic, morphometric and thermal IR spectral characteristics of the TVF features, comparing them with possible Earth analogue volcanic features of known lithologies. Work on deconvolving TES and THEMIS spectra is in progress. A main goal is to determine the identities of the lithologies that make up the material of the domes.
DE: 5410 Composition
DE: 5464 Remote sensing
DE: 5480 Volcanism (8450)
DE: 6225 Mars
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting