The case for rainfall on a warm, wet early Mars

By R. Craddock, Alan D. Howard. 2002

552 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/f84263160414b80f91946af67d27876b63f0e957

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Geologic Constraints on Early Mars Climate (2018, background): “Craters could not have been modified in one short pulse, in part because the most degraded craters tend to be older than slightly less degraded craters (Craddock and Howard 2002; Forsberg-Taylor et al. 2004; Quantin-Nataf et al. 2019).”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, background): “gy of large valley networks, the very high global erosion rate inferred for the early Noachian period, or the formation of extensive deposits of phyllosilicates like in the Mawrth Vallis region (e.g. Craddock and Howard, 2002, Bibring et al. 2006, McKeown et al. 2009). In any case, there is no doubt”
Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars (2007, background): “We speculate that acidic aqueous activity, including precipitation and infiltration in the southern highlands [Craddock and Maxwell, 1993; Craddock and Howard, 2002; Scott et al., 1995; Baker, 2001] could leach Fe, which is relatively easily leached at low pH, from the surface and carry the weathe”
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].”
Geologic history of Mars (2010, background): “The number of fresh appearing craters with well preserved ejecta patterns on Noachian terrains is comparable to the number on Hesperian terrains, which also suggests that high erosion rates persisted until the end of the Noachian and then rapidly declined (Craddock and Howard, 2002).”
Characterization of phyllosilicates observed in the central Mawrth Vallis region, Mars, their potential formational processes, and implications for past climate (2009, background): “Phyllosilicate deposits have been identified only in early to middle Noachian–aged terrain, leading Bibring et al. [2006] to name this period the ‘‘phyllosian’’ era, characterized by nonacidic aqueous alteration.”
The Climate of Early Mars (2016, background): “This geomorphology strongly suggests an origin due to a hydrological cycle driven by precipitation (as rain or snow) (Craddock & Howard 2002; Mangold et al. 2004; Stepinski & Stepinski 2005; Barnhart, Howard & Moore 2009; Hynek, Beach & Hoke 2010; Matsubara, Howard & Gochenour 2013) rather than…”
The geological and climatological case for a warmer and wetter early Mars (2018, background): “24); (2) CO2–H2 absorbs in spectral regions where CO2 and H2O absorb poorly23; and (3) absorption by CH4 is significant at solar wavelengths23.”
Large alluvial fans on Mars (2005, unknown): “[19] Howard and Craddock [2000] and Craddock and Howard [2002] noted that the floors of strongly degraded Noachian craters that appeared to be flat-floored in Viking images actually sloped gently from the base of the interior crater rim to the crater center.”
Sequence and timing of conditions on early Mars (2011, background): “Valley networks have numerous tributaries (Hynek et al., 2010), often begin near drainage divides (Craddock and Howard, 2002), and were interconnected across great distances, at least during their period of peak activity (see, e.g., Irwin et al., 2005; Fassett and Head, 2008a).”
Large impact crater histories of Mars: The effect of different model crater age techniques (2013, result): “…the planet around the latter half of the Middle Noachian to the Late Noachian, in agreement with previous work (e.g., Craddock and Maxwell , 1993; Craddock and Howard, 2002; Forsberg- Taylor et al., 2004; Boyce and Garbeil, 2007; Hoke and Hynek, 2009 ), including the approximat e amount of…”
Crustal structure of Mars from gravity and topography (2004, background): “Erosional modification of the surficial expression of the boundary [e.g., Hynek and Phillips, 2001; Craddock and Howard, 2002] possibly occurred after the crust had cooled significantly and was able to support elastic stresses.”
Updated global map of Martian valley networks and implications for climate and hydrologic processes (2010, background): “Many more recent local to regional studies on the basis of post‐Viking data have elucidated the characteristics of Martian valley networks and made inferences to the amount,duration,timing,andcapacityof water requiredfor their formation [e.g., Gulick, 2001; Williams and Phillips, 2001; Hynek and Phi”
The timing of martian valley network activity : Constraints from buffered crater counting (2008, background): “Warm, wet conditions in this scenario are long-lived, as crater degradation throughout the Noachian is interpreted to be due to fluvial erosion linked to pluvial precipitation (Craddock et al., 1997; Craddock and Howard, 2002).”
Deltaic deposits at Aeolis Dorsa: Sedimentary evidence for a standing body of water on the northern plains of Mars (2013, background): “, incised valley networks, streamlined islands, and cutoff meanders [Baker and Milton, 1974; Sharp and Malin, 1975; Carr, 1996; Craddock and Howard, 2002]), it is challenging for early Mars climate models to sustain clement mean annual surface temperatures primarily due to lower solar luminosity ear”
Context Camera Investigation on board the Mars Reconnaissance Orbiter (2007, background): “[Sharp and Malin, 1975; Pieri, 1980; Malin and Carr, 1999; Grant, 2000; Craddock and Howard, 2002; Aharonson et al., 2002].”
Impact‐induced hydrothermal activity on early Mars (2005, background): “[6] Ancient valley networks, some of which are interpreted as surface runoff [e.g., Williams and Phillips, 2001; Craddock and Howard, 2002], as well as chemical, mineralogical, and structural data from the Opportunity rover [Squyres et al.”