Main Results:
1) With the exception of containing an area (presumably older) that appears to have been eroded by fluvial activity and a much heavier mantling of dust, the geology NE of Gusev appears to be similar to the geology within the crater, dominated by two widespread rock types (high thermal inertia materials) and by wind-blown dust (high albedo, low thermal inertia).
2) The two rock types within Gusev have been investigated by the Spirit rover and their origin appears to be volcanogenic. One of the rock types (smooth morphology) has been interpreted to have crystallized from a younger basaltic lava flow and the other (rough morphology/more susceptible to aeolian erosion) probably formed from an older ash-fall resulting in volcanoclastic deposits, also of basaltic composition. Based on geomorphic, thermophysical, and stratigraphic similarities, we infer that these two volcanogenic rock types cover a significant portion of the area NW of Gusev.
3) This volcanogenic stratigraphy appears to be laterally continuous (to the north of the area studied) with materials that presumably originate from the Apollinaris Patera volcano. Thus it is tempting to identify this volcano as the main source of material which forms the Martian surface in the areas north of and within Gusev Crater.
Durham Academy Final Report
