The timing of martian valley network activity : Constraints from buffered crater counting

By Caleb I. Fassett, James W. Head III. 2008

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View Paper: https://www.semanticscholar.org/paper/ef24306d8a27b832e3943bed7234f82bdc96eff1

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In Astronomy and Astrophysics

Citations in the corpus

Redefinition of the crater-density and absolute-age boundaries for the chronostratigraphic system of Mars (2011, methodology): “Additionally, as already pointed out by Ivanov (2001), Hartmann and Neukum (2001), as well as Fassett and Head (2008), the three crater production functions used here differ most in the diameter range between 2 and 20 km, and this requires a detailed description of the utilized function sets and…”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, methodology): “However, still working with the same model, Forget and Pierrehumbert (1997) later showed that the inclusion of the CO2 ice cloud radiative effect at both solar and thermal infrared wavelengths led to a net warming of the surface rather than a cooling.”
Geologic Constraints on Early Mars Climate (2018, background): “Many but not all lakes overspilled at this time (e.g. Goudge & Fassett 2018, Fassett & Head 2008b), which was the only time in Mars history for which we see a record of pervasive and regionally-integrated valley networks.”
Hydrovolcanic tuff rings and cones as indicators for phreatomagmatic explosive eruptions on Mars (2013, background): “The relatively smooth flanks of the cones, which do not show evidence of fluvial dissection, also point to a formation time after the main period of fluvial activity on Mars [Fassett and Head, 2008].”
A chronology of early Mars climatic evolution from impact crater degradation (2012, background): “…et al., 2005; Bibring et al., 2006; Loizeau et al., 2007; Mangold et al., 2007; Mustard et al., 2009; Dehouck et al., 2010] and fluvial valley networks [e.g., Carr, 1996; Craddock and Howard, 2002; Howard et al., 2005; Irwin et al., 2005; Ansan and Mangold, 2006; Fassett and Head, 2008, 2011].”
The Climate of Early Mars (2016, background): “In general, low drainage ratios and a large number of open crater lakes indicate high precipitation rates and a wet climate (Fassett & Head 2008; Barnhart, Howard & Moore 2009).”
Sequence and timing of conditions on early Mars (2011, methodology): “Given the observations on the timing of valley network formation, three key questions remain to be definitively addressed: (1) how active was the period of valley network formation in the Noachian to the Early Hesperian, (2) how common/continuous were the periods when valleys were forming on early M”
Transient reducing greenhouse warming on early Mars (2016, background): “Because peak valley network formation occurs toward the end of the Noachian, a period of higher impact ﬂux than today [ Fassett and Head , 2008b, 2011], this mechanism deserves detailed investigation in future.”
Subsurface water and clay mineral formation during the early history of Mars (2011, background): “However, valley networks, deltas and outflow channels provide geomorphic evidence of Noachian and Hesperian surface water”
Juvenile Chemical Sediments and the Long Term Persistence of Water at the Surface of Mars (2009, methodology): “Morphologic evidence shows that water was present on early Mars and was perhaps abundant enough to leave signs of an integrated subsurface hydrology (Fassett and Head, 2008b).”
Formation timescales of large Martian valley networks (2011, background): “…et al., 2010), together with the locations and morphologies of the Martian deltas (e.g. Di Achille and Hynek, 2010) and ancient paleolakes (e.g. Fassett and Head, 2008a; Irwin et al., 2005a), provides strong evidence that the Martian surface environment was once capable of sustaining liquid…”
Geologic history of Mars (2010, background): “The intensity of valley formation also steeply declined, although not to zero (Fassett and Head, 2008b).”