Formation timescales of large Martian valley networks

Hoke, Monica R.T.; Hynek, Brian M.; Tucker, Gregory E.

doi:10.1016/j.epsl.2011.09.053

Cited by 158Planetary Science and ExplorationAstro and Planetary ScienceGeological formations and processes

Formation timescales of large Martian valley networks

Hoke, Monica R.T., Hynek, Brian M., Tucker, Gregory E.·2011·Earth and Planetary Science Letters

DOI 10.1016/j.epsl.2011.09.053

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Landform evolution models suggest minimum formation timescales for the Martian valley networks of 10^5 to 10^7 years under climate conditions appropriate to arid regions on Earth.
“Landform evolution models suggest minimum formation timescales for the valley networks of 10 5 to 10 7 years under climate conditions appropriate to arid regions on Earth (Barnhart, Howard & Moore 2009; Hoke, Hynek & Tucker 2011).”
From The Climate of Early Mars (2016) · cites this paper as Hoke, Hynek & Tucker 2011
The largest Martian valley networks extend thousands of kilometers over the surface.
“The largest networks are huge, extending thousands of kilometers over the surface in some cases (Howard, Moore & Irwin 2005; Hoke, Hynek & Tucker 2011).”
From The Climate of Early Mars (2016) · cites this paper as Hoke, Hynek & Tucker 2011
There is a large discrepancy between the estimated valley network erosion rates and the amount of rainfall produced post-impact.
“First, for transient impact-driven warming, there appears to be a large discrepancy between the estimated valley network erosion rates (Barnhart, Howard & Moore 2009; Hoke, Hynek & Tucker 2011) and the amount of rainfall produced post-impact (Toon, Segura & Zahnle 2010).”
From The Climate of Early Mars (2016) · cites this paper as Hoke, Hynek & Tucker 2011
A successful theory for surface warming must yield valley network erosion rates consistent with the geologic evidence but avoid extensive surface carbonate formation and aqueous alteration of sediments.
“A successful theory for surface warming must yield valley network erosion rates consistent with the geologic evidence (Hoke, Hynek & Tucker 2011) but avoid extensive surface carbonate formation and aqueous alteration of sediments (Tosca & Knoll 2009; Ehlmann et al. 2011).”
From The Climate of Early Mars (2016) · cites this paper as Hoke, Hynek & Tucker 2011

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Authors: Hoke, M. R. T., Hynek, B. M., & Tucker, G. E.
Affiliations: University of Colorado Boulder (US)
Cooperative Institute for Research in Environmental Sciences (US)
Corresponding author: Hoke, Monica R.T.
ORCID: Hynek, Brian M.
Tucker, Gregory E.
Venue: Earth and Planetary Science Letters
Publisher: Elsevier BV
Published: 2011-12
Volume: 312
Issue: 1-2
Pages: 1-12
ISSN: 0012-821X (ISSN-L)
DOI: 10.1016/j.epsl.2011.09.053
OpenAlex: W2036026278
Cited by: 158
References: 79
Citations by year: 2026: 8 · 2025: 13 · 2024: 10 · 2023: 9 · 2022: 13 · 2021: 10 · 2020: 13 · 2019: 12 · 2018: 14 · 2017: 10 · 2016: 9 · 2015: 15 · 2014: 10 · 2013: 9 · 2012: 2
FWCI: 3.59
Type: journal article
Language: en
Open access: closed
Licence: www.elsevier.com/tdm/userlicense/1.0/ (tdm)
www.elsevier.com/legal/tdmrep-license (tdm)
doi.org/10.15223/policy-017 (stm-asf)
doi.org/10.15223/policy-037 (stm-asf)
doi.org/10.15223/policy-012 (stm-asf)
doi.org/10.15223/policy-029 (stm-asf)
doi.org/10.15223/policy-004 (stm-asf)
Locations: Earth and Planetary Science Letters (publishedVersion)
Funders: National Aeronautics and Space Administration (NNX06AE08G)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Planetary Science and Exploration
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
Physical Sciences › Earth and Planetary Sciences › Earth-Surface Processes › Geological formations and processes
Keywords: Martian valley networks, sediment transport, Darcy-Weisbach equation, flow velocity, valley incision

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