HR: 1340h
AN: V33C-1482    [Abstracts]
TI: Olympus Mass Movement Study from Mars Global Surveyor and Comparison with Io's Volcanoes and Mountains from Galileo Mission
AU: * Paganelli, F
EM: flora.paganelli@jpl.nasa.gov
AF: NASA Jet Propulsion Lab., California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 United States
AU: Lopes, R M
EM: rosaly.m.lopes@jpl.nasa.gov
AF: NASA Jet Propulsion Lab., California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 United States
AU: Turtle, E P
EM: turtle@pirl.lpl.arizona.edu
AF: Lunar and Planetary Lab., Dept. of Planetary Sciences University of Arizona, 1629 E. University Blvd., Tucson, CA 85721 United States
AU: Williams, D A
EM: david.williams@asu.edu
AF: Dept. of Geological Sciences, Arizona State University, Bateman Physical Sciences Bldg. F506B, Tempe, AZ 85287 United States
AB: The Olympus and Arsia Mons shield characteristics and surrounding deposits are addressed using data from the Mars Global Surveyor mission, and comparative observations of Io's shield volcanoes and mountains mass wasting features using data from the Galileo mission. Martian and Ionian mass wasting deposits suggest a possible tectonic origin. Martian mass wasting features are observed mainly as apron materials defining concentric ridges around the shield volcanoes Olympus and Arsia Mons. Io's shield volcanoes in the Zamama region are much smaller compared to the Martian examples and do not exhibit extensive mass wasting features. On the other hand, Io's mass wasting deposits show morphological characteristics similar to Martian corrugated apron materials. Io's mountains are typically on the order of tens to a hundred km in length and rise to heights of several kilometers, ranging from high sharp peaks to lower, smooth, rounded mountains. Sulfur-rich layers may provide zones of weakness that could facilitate extensive mass movements.
DE: 6200 PLANETOLOGY: SOLAR SYSTEM OBJECTS (New field)
SC: Volcanology, Geochemistry, Petrology [V]
MN: 2004 AGU Fall Meeting