Year: 2013
Type: conference-paper
Abstract: Introduction: Havel Vallis is a SW-NE trending, ~260 km long valley (Fig. 1).It is adjacent to Juventae Chasma and Baetis Chaos systems which are the source regions for Maja Valles [1] and (partially) for Havel Vallis.The elevation of Havel Vallis ranges from about 0 m in Mutch crater up to 1030 m above Martian datum in crater A. This abstract focuses on the formation of Havel Vallis and discusses two possible scenarios.In addition, potential depositional mechanisms for some related fluvial deposits are presented.Methods: Mapping of Havel Vallis and adjacent areas is based on THEMIS IR day/night time datasets.For detailed observations in the visible spectra HRSC, CTX, and MOC data were utilised.Topographic analysis is based on a HRSC-DTM mosaic.We used ESRI's ArcGIS suite for the vector mapping, crater statistics, and raster overlays.Crater counts were performed and analysed following the procedures described in [2][3][4][5].Topography and hyperconcentrated flow deposits: The valley system is divided into four areas: 1) crater A with its two outlets to the east and west, 2) a central valley, 3) a basin-like depression, and 4) the floor of Mutch crater.Gorges, 250-400 m of relief, separate areas 2-4 (Fig. 2).Floor deposits in areas 2-4
Language: English
Subfield: Space and Planetary Science
Field: Earth and Planetary Sciences
Domain: Physical Sciences
Open Access status: green
OpenAlex ID: W136357988