Erosion rates on Mars and implications for climate change: Constraints from the Pathfinder landing site

By M. Golombek, N. Bridges. 2000

190 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Earth-Surface Processes

View Paper: https://www.semanticscholar.org/paper/7a45c56344aa5bcc129737ac5e53cf294ad3d51a

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Citations in the corpus

Rock size-frequency distributions on Mars and implications for Mars Exploration Rover landing safety and operations : Mars exploration rover mission and landing sites (2003, background): “…suggested a less dusty environment than Viking 1 and 2 [Golombek et al., 1997a, 1999b; Bell et al., 2000] and interpretations of the surface around the Pathfinder lander suggest a region of net erosion or loss of material [Greeley et al., 1999, 2000; Ward et al., 1999; Golombek and Bridges, 2000].”
Formation of Martian Gullies by the Action of Liquid Water Flowing Under Current Martian Environmental Conditions (2005, background): “The current Martian erosion rates and dust deposition rates are not sufficient to bury or erase gullies thought to be 10 m deep in only 250,000 years [Golombek and Bridges, 2000].”
The rayed crater Zunil and interpretations of small impact craters on Mars (2005, background): “If they were mary craters that are shallow due to eolian fill, then th must have been a very recent depositional event bec few or no bowl-shaped craters have subsequently form Furthermore, the reduction of the crater’s depth/diamete tios by significant erosion and infilling after formation not suppo”
Widespread surface weathering on early Mars: A case for a warmer and wetter climate (2015, background): “For example, Arabia Terra has the highest concentration of weathering sequences and is thought to have experienced intense erosion (Golombek and Bridges, 2000; Fergason and Christensen, 2008) mainly during the Amazonian.”
Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) (2007, background): “One example is whether the rocks at the Pathfinder landing site were emplaced directly from ancient catastrophic floods or as more recent impact ejecta, which in turn is key to questions such as estimation of long term average erosion rates [Golombek and Bridges, 2000].”
Geologic history of Mars (2010, background): “Golombek and Bridges (2000) and Golombek et al. (2006) in summarizing all the data available on martian erosion rates concluded that although Noachian erosion rates were 2–5 orders of magnitude higher than they were subsequently, they still appear to have been lower than average terrestrial rates,…”
Oceans on Mars: An assessment of the observational evidence and possible fate (2002, background): “…and the formation of the large outflow channels, which are mainly Hesperian in age [Tanaka, 1986], and because low cumulative amounts of erosion since the end of the Noachian [Arvidson et al., 1979; Carr, 1992; Golombek and Bridges, 2000] cause most post-Noachian landforms to be well preserved.”