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QUANTIFYING THE ENVIRONMENTAL RESPONSE TO DEGLACIATION IN MARTIAN CRATERS

Introduction: The mid-latitudes of Mars have experienced extensive patterns of glaciation throughout the Late Amazonian due to climate excursions, which are primarily driven by quasi-periodic fluctuations in orbital parameters, the most influential of which being obliquity [1,2]. These variations in axial tilt and eccentricity have led to in the repeated migration of glacial ice between the polar caps and the mid-latitudes [1,3,4] due to global shifts in the distribution and seasonal intensity of solar illumination [2]. During periods of glacial accumulation at the mid-latitudes, ground-ice becomes unstable at the polar caps, resulting in the removal of ice from the polar regions and its ensuing deposition in the mid-latitude regions [1,3,5]. Glacial deposits in the mid-latitudes are thought to have been stable up to ~5 Ma, where the mean obliquity of Mars was ~35°[2]. Between ~5 and ~2.5 Ma, the mean obliquity is modeled to have decreased from ~35° to ~25°, leading to the mid-latitudes transitioning into a period of glacial ablation [2,5]. The deglaciation process would have rapidly begun to erode and modify the previously glaciated environment as the glaciers retreated [5,6]. The transitional stage between glacial and interglacial periods is known as a paraglacial period and it is accompanied by a host of diagnostic geologic features on Earth [7,8] that have also been identified on the surface of Mars [5]. The paraglacial features of interest in this study include spatulate depressions, washboard terrain, polygonal terrain, and gullies (Fig. 1). Spatulate depressions are sharply rimmed depressions with hummocky floors that can be found near the bottom of the crater slope [5]. In craters at the mid-latitudes of Mars, they are often located on the pole-facing side of the crater, and they are interpreted to be formed via enhanced ice sublimation mechanisms at the base of the crater wall [3,8]. Washboard terrain denotes a cluster of parallel scarps that are perpendicular to the crater slope, which could have been created through debuttressing and ice crevassing [5]. The morphology of the polygonal terrain in the craters of this study are similar to sublimation polygons, which are indicative of the periodic thermal cycling of near-surface ice-rich material [1,5,10]. Gullies, argued to have a wide range of formation mechanisms, are likely to have formed primarily via water-assisted flow, although they may also be modified by dry and CO2-assisted flow [5]. Aim of This Study: This work aims to draw comparisons between 5 unnamed craters near Terra Sirenum in the southern hemisphere (~160°W, 40°S) and 5 near Utopia Plantitia (~80°E, 40°N) in the northern hemisphere. The craters have previously been identified as containing paraglacial features by [3]. We mapped out the paraglacial features using Context Camera (CTX) [11] and HiRISE [12] observations of the specific craters and quantified the characteristics of each paraglacial feature along with conducting a spatialproximity analysis between the various paraglacial features. By understanding the patterns between the extent of these paraglacial features in relation to their local environment, we hope to better understand the specific nature of deglaciation and paraglacial modification in recent Mars history.