Geomorphic evolution of the Martian highlands through ancient fluvial processes

Craddock, Robert A.; Maxwell, Ted A.

doi:10.1029/92je02508

Cited by 242Planetary Science and ExplorationAstro and Planetary ScienceGeological formations and processes

Geomorphic evolution of the Martian highlands through ancient fluvial processes

Craddock, Robert A., Maxwell, Ted A.·1993·Journal of Geophysical Research: Planets

DOI 10.1029/92je02508

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Abstract

Craters in the Martian highlands are preserved in various stages of degradation. As a result of an erosional process active from the Middle Noachian (4.40–3.92 b.y.) through the Hesperian (3.55–1.8 b.y.), ejecta associated with fresh impact craters became etched, hummocky, and dissected by runoff channels. With time, interior gullies became deeply incised and ejecta deposits were entirely removed. Infilling of the craters followed until, in some instances, the craters were completely buried. Only fluvial processes explain these morphologic variations, the size range of affected craters, and the size‐frequency distribution curves associated with these crater populations. Based on the number of superposed fresh impact craters, fluvial processes affecting the highlands ceased entirely by the end of the Hesperian. No correlation between cessation of degradation and latitude exists. However, a strong correlation exists between cessation of degradation and elevation. Degradation ended at higher elevations (e.g., 3–4 km; N [5]=∼200, Late Noachian) before lower elevations (e.g., 1–2 km; N[5]=∼180, Early Hesperian), suggesting that cessation was coupled to desiccation of the volatile reservoir and degassing of a 5–20 bar primordial atmosphere. Volatiles released to the surface by runoff channel formation and seepage may have been part of a complex hydrologic cycle that included periodic, heavy amounts of precipitation. Rainfall was principally responsible for degrading the highlands,…

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Crater erosion rates in the Noachian may have been caused by precipitation.
“Also, crater erosion rates in the Noachian may have been caused by precipitation [Craddock and Maxwell, 1993].”
From A chemical model for evaporites on early Mars: Possible sedimentary tracers of the early climate and implications for exploration (1999) · cites this paper as Craddock and Maxwell, 1993

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Authors: Craddock, R. A., & Maxwell, T. A.
ORCID: Craddock, Robert A.
Venue: Journal of Geophysical Research: Planets
Publisher: American Geophysical Union (AGU)
Published: 1993-02-25
Volume: 98
Issue: E2
Pages: 3453-3468
ISSN: 0148-0227 (ISSN-L)
DOI: 10.1029/92je02508
OpenAlex: W2153889975
Cited by: 242
References: 81
Citations by year: 2026: 1 · 2025: 2 · 2024: 6 · 2023: 4 · 2022: 9 · 2021: 3 · 2020: 6 · 2019: 9 · 2018: 16 · 2017: 6 · 2016: 9 · 2015: 7 · 2014: 11 · 2013: 6 · 2012: 8
FWCI: 7.81
Type: journal article
Language: en
Open access: closed
Licence: onlinelibrary.wiley.com/termsAndConditions#vor (vor, 7148 d)
Locations: Journal of Geophysical Research Atmospheres (publishedVersion)
Smithsonian Digital Repository (Smithsonian Institution) (submittedVersion)
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 highlands, fluvial erosion, gully incision, crater size-frequency distribution, Hesperian, Late Noachian, groundwater recharge, denudation rates, periglacial erosion

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Geomorphic evolution of the Martian highlands through ancient fluvial processes

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