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Flow depth (blue) and river routes (red) based on model calculations in the target area. Note that the edge of the Jezero Crater runs as an arc-shaped darker blue (steep and thus small flow depth, dominated by fast runoff) area, from the upper right toward lower left. The indicated terrain is the same as in Figure 4 at 18.48°N; 77.37°E.
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Identifying surface sites with significant astrobiological potential on Mars requires a comprehensive understanding of past geological processes and conditions there, including the shallow subsurface region. Numerical modelling could distinguish between regions dominated by erosion and those characterized by sediment accumulation in ancient wet env...
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Citations
... To achieve the goal of this study, we recognized the need to select regions on Earth that exhibit geomorphological characteristics similar to those observed on interesting sites on Mars, such as Jezero crater (e.g., [9,10]). This Martian crater, with a diameter of approximately 49 km, and located to the northwest of the Isidis impact basin on Mars, displays unique features suggesting a history rich in fluvial activity [11]. ...
The comparative analysis of hyperspectral data from different instruments can provide detailed information on the composition and geology of similar environments on different planets. This study aims to compare data acquired from the PRISMA satellite, used for Earth observation, with those collected by the CRISM spectrometer onboard the Mars Reconnaissance Orbiter, orbiting Mars, in order to analyze the geological and mineralogical differences between the morphologies present on the two planets of interest. The comparison of these data will allow us to examine the mineralogical composition, highlighting the similarities and differences between the terrestrial and Martian environments. In particular, in this study, we present a method to refine the interpretation of spectral features of minerals commonly found in paleo-hydrological environments on Mars and identified also by field analysis of similar terrestrial sites, thus allowing us to improve the Martian sites’ characterization. Thanks to this approach, we have been able to find spectral similarities (e.g., band positions, band ratios) among specific Earth and Mars sites, thus demonstrating that it could be further expanded, by systematically using Earth-observation orbiting instruments to better characterize and constrain Martian spectral data.
