Mathematics – Logic
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm...p31a09f&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #P31A-09
Mathematics
Logic
5416 Glaciation, 5462 Polar Regions, 6225 Mars
Scientific paper
Building upon previous studies of the north polar region of Mars [e.g., 1, 2, 3, and 4], we [5] outlined evidence for retreat of the polar cap from the 180° W direction, including the presence of polar material remnants and kettle-like features in an arc of irregular, low-lying topography (the Olympia Depression) south of and concentric to Olympia Planitia [5]. In this study, we further characterize and categorize features in this region using Viking and MOC images and high-resolution MOLA data. Within the Olympia Depression are large, deep depressions interpreted to be kettle-like features [5] higher-standing topography surrounding these depressions (some of which is interpreted to be polar material remnants [5]). Together, these constitute the rough terrain. The irregular shape and rough, high-standing floor of the rough terrain is not consistent with these being degraded impact craters. These features appear to have undergone significant removal of volatiles and subsequent collapse to form depressions. Evidence of ridges which may be moraines, sedimentation at the margins and drainage channels has also been found. Dome-like features lie just to the south of the rough terrain. The morphology and dimensions are dissimilar from Martian south polar region and terrestrial volcanic domes [13] in that the width to height ratio is much larger and they are highly degraded. If these domes represent central peak structures, any evidence of rims is gone. Alternatively, these domes could be volatile-rich, representing early stages of what will become the rough terrain. We interpret the individual features of the Olympia Depression to represent kame and kettle topography, resulting from the ablation (melting and sublimation) and retreat of the polar cap. On Mars, the high concentration of polar deposit inter-layered debris (about 40%) will favor the development of kames as ablation occurs and sediment remains. The morphologic features within the Olympia Depression are transitional to Olympia Planitia and to the main polar cap. We interpret the rough terrain as large, proximal kame and kettle features and armored ice remnants. The dome-like features are interpreted as distal, smaller kame and kettle features and armored ice remnants. Retreat of the polar cap has apparently occurred geologically relatively recently (in Late Amazonian times). [1] Dial, A. (1984) U.S.G.S. Misc. Invest. Ser. Map I-1640. [2]Tanaka, K. and D. Scott (1987) U.S.G.S. Misc. Invest. Ser. Map I-1802-C. [3] Thomas, P., S. Squyres, K. Herkenhoff, A. Howard, and B. Murray, (1992) in Mars, H. Kieffer et al., eds., Univ. of Ariz. Press, 767-795. [4] Zuber, M. et al. (1998), Science 282, 2053-2060. [5] K. Fishbaugh and J. Head (2000), JGR 105, 22455-22486.
Fishbaugh Kathryn E.
Head James W.
Marchant David R.
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