The aim of this thesis is to analyze zonality of the thermal contraction crack polygons on the surface of Mars. Their morphology and its variation are analyzed in relation to the latitude of Mars. For spatial and morphological analysis were selected 64 images from the HiRISE (Mars Reconnaissance Orbiter) polychromatic camera dataset, images are covering the bandwidths proportionally. Images were first visually analyzed using HiView. 258 areas containing the thermal contraction crack polygons (with total area of 1184 km2 ) and 1036 well developed thermal contraction crack polygons were further vectorized using ArcMap. The thermal contraction crack polygons were found in every searched latitude which proves the ubiquity of permafrost. The largest amount of the thermal contraction crack polygons have been found in latitudes ±60ř and 45ř. In these latitudes were also found the largest and probably the deepest thermal contraction crack polygons (average length ranges from 42,1 - 73,6 m). The smallest polygons (average length 7,7 m) were found around the equator. "Altitude" has no effect on the spread of the thermal contraction crack polygons on Mars; however it has the effect on its morphology. The most widespread are pentagonal polygons, which occur mainly in the southern hemisphere. The next most...

Rock glaciers play a significant role in the alpine debris transport system. For practical and engineering considerations, identifying the internal structure and its relationship to surface characteristics is significant in terms of how a rock glacier settles during periods of melting, and the mode of deformation. A better understanding of these factors is important for engineers, engineering geologists and geomorphologists who must make prudent evaluations of rock glaciers as potential sites for human development and uses. It is equally important for evaluating potential stores for water on other planets such as Mars. Ground penetrating radar (GPR) shows that the internal structure of a lobate rock glacier located in the San Juan Mountains of southwest Colorado consists of continuous to semi-continuous horizontal layers of ice-supersaturated sediments and coarse blocky rockslide debris which likely formed through catastrophic episodes of rockfall from the cirque headwall. Folds in the uppermost layers correspond to the surface expression of ridges and furrows, indicating that compressive stresses originating in the steep accumulation zone are transmitted downslope through the rock glacier. The rock glacier is a composite feature that formed by a process involving the development and overlap of discrete flow lobes that have overridden older glacial moraine and protalus rampart materials. The latter materials have been incorporated into the present flow structure of the rock glacier. The discovery of rock glacier-like features on Mars suggests the presence of flowing, or once-flowing ice-rock mixtures. These landforms, which include lobate debris aprons, concentric crater fill and lineated valley fill, hold significant promise as reservoirs of stored water ice that could be used as fuel sources for human exploration of Mars and provide a frozen record of the climatic history of the planet. To this end, the rock glacier in this study was used as a surrogate for similar Martian landforms. Liquid water, found to be abundant in this rock glacier, occurs within a network of interconnected channels that permeate throughout the landform. In terms of water storage within Martian analogs, consideration must include the possibility that some water ice may be stored in relatively pure form within lenses and vein networks that are supplied by seasonal frost accumulation and/or water influx from below.