Emplacement Mechanisms of the Olympus Mons aureole deposits (OMAD)

Details Emplacement Mechanisms of the Olympus Mons aureole deposits (OMAD) Emplacement Mechanisms of the Olympus Mons aureole deposits (OMAD)

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p22d..02m&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #P22D-02

Astronomy and Astrophysics

Astrophysics

5417 Gravitational Fields (1227), 5470 Surface Materials And Properties, 5480 Volcanism (8450), 6225 Mars, 8414 Eruption Mechanisms

Scientific paper

The Olympus Mons aureole deposits (OMAD) on Mars consist of vast lobes of hummocky-textured material with well-defined ridges and troughs that surround the main volcanic edifice of Olympus Mons. Hypotheses for the formation of these deposits fall broadly into two categories: emplacement in-situ as some sort of volcanic product (e.g., pyroclastics, sub-glacial eruptions), and emplacment by mass movement of material derived from the flanks of the volcano (e.g., large landslides or slumps). However, most studies of OMAD preceeded a radical reassessment of the structure and evolution of large volcanoes, brought about by events such as the catastrophic failure of the flanks of Mt. St. Helens and the discovery of numerous large mass movements off the flanks of Hawaiian volcanoes. Furthermore, the Mars Global Surveyor (MGS) mission has yielded a plethora of topography, gravity, and imaging data with unprecedented resolution and accuracy. It is therefore timely to renew efforts to understand the emplacement mechanism(s) for the OMAD. We will apply new MGS data to evaluate the hypotheses outlined above, in order to constrain the formation mechanism(s) of the aureole lobes. We will analyze Mars Orbiter Laser Altimeter (MOLA) altimetry data and Mars Orbiter Camera (MOC) images to characterize aureole lobe morphologies, volumes, and short- and long-wavelength slopes. The characteristics of aureole lobe terminations and inter-lobe boundaries will be closely observed for clues to emplacement modes. Topographic characteristics of the aureole lobes will be compared to those of known pyroclastic and mass-movement features on Mars. We will also compare aureole topography to topography and bathymetry of landslides, slumps, and flows surrounding terrestrial volcanoes in a variety of settings. Geophysical modeling, incorporating MOLA topography and Radio Science experiment (RS) gravity data, will elucidate subsurface structures which may influence aureole development.

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