HR: 0800h
AN: C51A-0092    [Abstracts]
TI: Tropical Mountain Glaciers on Mars: Altitude-Dependence of Ice Accumulation, Accumulation Conditions, Formation Times, Glacier Dynamics, and Implications for Planetary Spin- Axis/Orbital History
AU: * Fastook, J L
EM: fastook@maine.edu
AF: University of Maine, Climate Change Institute, Orono, ME 04469, United States
AU: Head, J W
EM: James_Head@brown.edu
AF: Brown University, Geological Sciences, Providence, RI 02912, United States
AU: Marchant, D R
EM: marchant@bu.edu
AF: Boston University, Earth Sciences, Boston, MA 02215, United States
AB: Lobate deposits up to ~166,000 km2 in area are found on the northwest flanks of the huge Tharsis Montes volcanos in the tropics of Mars. Recent spacecraft data have confirmed earlier hypotheses that these lobate deposits are glacial in origin. Increased knowledge of polar-latitude terrestrial glacial analogs in the Antarctic Dry Valleys has been used to show that the lobate deposits are the remnants of cold-based glaciers that formed in the extremely cold, hyper-arid climate of Mars. Mars atmospheric general circulation models (GCM) show that these glaciers form during periods of high obliquity when upwelling and adiabatic cooling of moist polar air favor deposition of snow on the northwest flanks of the Tharsis Montes. We present a simulation of the Tharsis Montes ice sheets produced by a static accumulation pattern based on the GCM results and compare this with the nature and extent of the geologic deposits. We use the fundamental differences between the atmospheric snow accumulation environments (mass balance) on Earth and Mars, geological observations and ice sheet models to show that two equilibrium lines should characterize ice sheet mass balance on Mars, and that glacial accumulation should be favored on the flanks of large volcanos, not on their summits as seen on Earth. Predicted accumulation rates from such a parameterization, together with sample spin-axis obliquity histories, are used to show that mean obliquity in excess of 45 degrees and multiple 120,000 year obliquity cycles are necessary to produce the observed deposits. Our results indicate that the formation of these deposits required multiple successive stages of advance and retreat before their full extent could be reached, and thus imply that spin-axis obliquity remained at these high values for millions of years during the Late Amazonian period of Mars history. Spin-axis obliquity is one of the main factors in the distribution and intensity of solar insolation, and thus in determining the climate history of Mars. Unfortunately, reconstruction of past climate history is inhibited by the fact that calculations of spin-axis geometry histories prior to about 20 Ma ago are not possible due to the chaotic nature of the solutions. We show, however, that the geological record, combined with glacial modeling, can be used to provide insight into the nature of the spin-axis/orbital history of Mars in the Late Amazonian, and to begin to establish data points for the geologically-based reconstruction of the climate and orbital history of Mars.
DE: 0700 CRYOSPHERE (4540)
DE: 0726 Ice sheets
DE: 0774 Dynamics
DE: 0798 Modeling
DE: 1621 Cryospheric change (0776)
SC: Cryosphere [C]
MN: 2007 Fall Meeting