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• W1619599814 abstract "Introduction: The recent advance in imaging of Mars confirmed that a number of previously hypothesized geomorphological feature types were related to ice flow, as well as revealed a variety of related new feature types. In the equatorial zone, the western slopes of the four major volcanoes bear a set of features interpreted as left by kilometers-thick cold-based ice sheets formed during epochs of high mean obliquity in the Amazonian [e.g., 1]. Martian midlatitudes display a very wide variety of features related to flow of ice or creep of permafrost; they include lobate debris aprons, lineated valley fill, slope-associated lobes interpreted as extinct or present rock and/or debris-covered glaciers, extinct ice sheets, etc. The abundance of such features in the midlatitudes is explained [2] by both relatively high year-average temperature, which enables flow of H2O ice or icy permafrost, and relatively good conditions for ice stability. At high latitudes, H2O ice is present in large amounts, forming the polar layered deposits (PLD) and the high-latitude ice-rich mantle, but ice flow is very limited. In general, this is naturally explained by the much lower year-average temperature at high latitudes. Here we describe very unusual deposits that depart from this general trend, and discuss their possible origin. Unusual extinct small cold-based glaciers: An unusual series of narrow ridges with lobate planforms occurs at high latitudes in the martian arctic (74°N 96°E), in association with the westand northwestfacing steep slopes of a PLD outlier (Fig. 1). The most striking aspect of these features is the large number of distinctive arch-like ridges (in planform view) forming more than 20 parallel and overlapping loops over a distance of about 75 km grouping in three sets with gaps between them (Fig. 1b). The individual ridges making up the loops are 15-80 m wide, are generally continuous, and show little width and height variation along their strike. The loops formed by these ridges are most typically 5-7 km in long axis, and ~1.5-3 km wide. No impact craters could be found that were clearly superposed on top of the ridges; in several cases, the ridges in the distal parts of loops are superposed on the extended deposits surrounding impact craters; no evidence of modification of the underlying deposits or structures are observed; these all suggest a relatively youthful age. High-resolution MOC images (E03/01183, R02/01333) show that the ridges are mantled and covered with typical high-latitude polygonal pattern uniformly with their surroundings. Some of the ridges, and thus the loops, are superposed on one another. In the middle group (Fig. 1c, top) a generally continuous ridge set that extends distally (with respect to the PLD outlier) for a distance of up to 15 km; the ridge is subdued in some places along its strike. Shorter loops contained within this deposit are clearly superposed on this larger ridge complex occurrence. Stratigraphic relationships for the middle group suggest that the earliest set of ridges was the broadest and reached the greatest distal limits; an intermediate set extended only about 3 km, and the latest set extended an intermediate distance. In the southern group, local stratigraphic relationships also support three stages. The proximal parts of the looped ridges are open toward the steep wall of the PLD outlier and are separated from it by a 10-20 km wide gap." @default.
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• W1619599814 date "2007-03-01" @default.
• W1619599814 modified "2023-09-23" @default.
• W1619599814 title "Unusual Glacial-like Features in the High-Arctic of Mars" @default.
• W1619599814 hasPublicationYear "2007" @default.
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