In the Wattenberg Field, the Reservoir Characterization Project at the Colorado School of Mines and Occidental Petroleum Corporation (Oxy) (formerly the Anadarko Petroleum Corporation) collected time-lapse seismic data for characterization of changes in the reservoir caused by hydraulic fracturing and production in the Niobrara Formation and Codell Sandstone member of the Carlile Formation. We have acquired three multicomponent seismic surveys to understand the dynamic reservoir changes caused by hydraulic fracturing and production of 11 horizontal wells within a 1 mi2 section (the Wishbone Section). The time-lapse seismic survey acquisition occurred immediately after the wells were drilled, another survey after stimulation, and a third survey after two years of production. In addition, we integrate core, petrophysical properties, fault and fracture characteristics, as well as P-wave seismic data to illustrate reservoir properties prior to simulation and production. Core analysis indicates extensive amounts of bioturbation in zones of high total organic content (TOC). Petrophysical analysis of logs and core samples indicates that chalk intervals have high amounts of TOC (>2%) and the lowest amount of clay in the reservoir interval. Core petrophysical characterization included X-ray diffraction analysis, mercury intrusion capillary pressure, N2 gas adsorption, and field emission scanning electron microscopy. Reservoir fractures follow four regional orientations, and chalk facies contain higher fracture density than marl facies. Integration of these data assist in enhanced well targeting and reservoir simulation.

The mapped crater region of Mars is located in the Southern Highlands specifically in the Eridania basin between the latitudes 179ºW-176 ºW and the longitudes ºS-40 ºS. The striking features within the mapping region are the two large, main craters, the east to west crosscutting Sirenum Fossae complex, the enigmatic chaotic terrain, and the north to south oriented wrinkle ridges. This study describes the geologic units of the region based on their unique morphological differences. Analysis of the units generated a geologic map of the area and an accompanying stratigraphic column placing the units into a relative age relationship. The resulting geologic map was produced using MOLA, CTX, THEMIS, and HiRISE images. By comparing the results to previous studies of the Martian surface, an interpretation of the geologic units and the processes that dominated their unique morphologies is determined. The final step of this study created a geologic history documenting the changing climate, depositional sequences, and structural influences that occurred within the mapping area. This analysis documents heavy tectonism, volcanism, eolian activity, fluvial activity, and lacustrine effects on the area. Also documented is a changing Martian climate from one that was warm and wet in the early history to one of a colder and dryer nature as time progressed.