49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2407.pdf Preliminary Volcanic Feature Analysis of Olympus and Ascraeus Mons, Mars. K.J. Mohr1, D.A. Williams1, W.B. Garry2, and Jacob E. Bleacher2 1School of Earth & Space Exploration, Arizona State University, Tempe, AZ 85282,
[email protected], 2Planetary Geology, Geophysics, and Geochemistry Laboratory, Code 698, NASA Goddard Space Flight Center, Greenbelt, MD 20771. Introduction/Background: Olympus Mons (OM) Only features observed on the flanks of the and Ascraeus Mons (AM) are two large shield volcanoes were used in this study. However, future volcanoes found in the Tharsis province on Mars. Both work will include small shields found on the volcanoes have been recently mapped at a 1:1,000,000 surrounding plains of each of the Tharsis Montes. scale using high resolution imagery [1,2]. Mapping of Geologic Observations: Both Olympus Mons and Arsia and Pavonis Montes are still in progress. With the Ascraeus Mons are dominated by flank channel flows completion of the Olympus and Ascraeus Montes maps, that embay older flank ridge flows, suggesting a change direct comparison of volcanic features found on each in lava properties from a less viscous effusive flow to a edifice can be done. Rose diagram analysis shows more viscous effusive flow [1,2]. Lava fans are also strong similarities in specific features found on the two observed on both volcanoes, which are fan-like features large volcanoes, further suggesting a similar formation where a sudden change in slope allowed for a tube-fed and evolution. flow or vent to extrude lava into a deltaic shape.