Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusm.p32a..07f&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #P32A-07
Physics
5400 Planetology: Solid Surface Planets, 5480 Volcanism (8450), 6225 Mars, 8450 Planetary Volcanism (5480)
Scientific paper
MOLA data reveals a very large lava flow unit extending almost 2000 km northeast from the base of the Olympus Mons aureole across northern Amazonis Planitia and southern Arcadia Planitia. Though its provenance is uncertain, as its proximal extent is buried under the aureole, several lines of evidence indicate that the flow unit most probably represents pre-aureole volcanism from Olympus Mons. As the aureole margin there is 900 km from the Olympus Mons summit caldera, the original flow length has an upper limit of approximately 3000 km. Observations from MOLA data include: 1) The flow is roughly radial to Olympus Mons and appears to be following the regional topography. 2) The northern flow margin shows more dramatic relief and steeper slopes than the southern margin, suggesting that younger units within Amazonis Planitia have mantled and softened the flow boundary. 3) The flow structure is surrounded by very smooth terrain. Observations from MOC images include: 1) Extensive layering within the flow unit suggests that it was emplaced as a series of high-volume eruptions, perhaps similarly to the major basaltic provinces on Earth (e.g. Deccan Traps, Columbia River Flood Basalts). 2) The surrounding smooth terrain shows evidence of surface water and ground ice, including small channels; the channels may represent mobilization of ground ice or dewatering from the lava flow emplacement.
Fuller Elizabeth R.
Head James W.
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