Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm...v42a05g&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #V42A-05
Physics
6225 Mars, 8414 Eruption Mechanisms, 8429 Lava Rheology And Morphology, 8450 Planetary Volcanism (5480)
Scientific paper
An active Martian lava flow has yet to be observed, so that eruption and emplacement parameters must be inferred from the resulting lava flow morphologies. Mars Global Surveyor (MGS) has provided a wealth of new information about Martian lava flows, and has allowed us to refine our interpretations of Martian volcanic behavior-and how this behavior varies in time and space. Somewhat surprisingly, MOC high-resolution images provide information on lava flow surface textures only for extremely young flows; typically, Martian lavas are covered with dust and/or dunes. MOLA data also reveal several details of lava flow morphologies that were not apparent in Viking Orbiter (VO) images, but at larger scales and also for more weathered flows than can be resolved in MOC images. MOLA data show that true lava flow boundaries (identified by topographic profiles) tend to lie outside those identified in VO images. Additionally, MOLA exposes central channels in lava flows that were believed to be flat-topped on the basis of VO images. As a result, flows previously labeled flat-topped are often slightly wider channel-fed flows, and flows previously identified as containing discontinuous channels or depressions are revealed to contain a subtle ridge with axial collapse structures characteristic of lava tube-fed flows. Using lava channel or tube collapse dimensions and underlying slopes obtained from MOLA, we have estimated the flow velocities and effusion rates for a range of flow lobes across Mars: Tyrrhena Patera, Syrtis Major, Elysium Mons, Arsia Mons, and Olympus Mons. In general, Martian lavas appear to have effusion rates and flow velocities that are at least 10 times higher than the highest basaltic effusion rates yet observed on Earth (Mauna Loa, Hawaii, 1984 eruption). However, the rates obtained are comparable to those estimated for mid-ocean ridge eruptions. Lava flow lobes at Tyrrhena Patera were emplaced at rates similar to those observed for Mauna Loa and Kilauea volcanoes, Hawaii. The relatively low rates for the Tyrrhena Patera flows may be related to the low underlying slopes there, or perhaps to a unique lava composition and/or emplacement style.
Gregg T. K.
Sakimoto Susan E.
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