Characterization of fluvial activity in Parana Valles using different age-dating techniques
Résumé
Martian valley networks provide the best evidence that the climate on Mars was different in the past. Although these features are located primarily in heavily cratered terrain of Noachian age (>3.7 Ga), the ages of the features and the time when they were active is not well understood. From superposed craters several recent global studies determined that most valley networks formed during the Late Noachian to Early Hesperian; however, there were some disparities between the techniques. In this study, our principal objective was to test the reliability of the different age-dating techniques to better understand their accuracy and limitations. We applied these techniques to Parana Valles using a variety of high-resolution images taken from different instruments that allow us to identify smaller craters ( D > 125 m) while providing sufficient coverage to support a statistically reliable sampling of crater populations, which is necessary to reduce the uncertainties in age determination. Our results indicate that Parana Valles formed during the Early Hesperian Period but that the crater density ( D > 353 m) is heterogeneous inside the Parana Valles basin. The crater population decreases from the headwaters downstream recording a resurfacing event that is most likely related to the erosion of downstream sub-basins. The terrain near the source area is Late Noachian to Early Hesperian in age while terrains closer to the outlet are Early to Late Hesperian in age. Crater densities ( D > 125 m) inside the valley are also heterogeneous and record several resurfacing events on the valley floor. Where the width of the valley network narrows to