Cratering Chronology and the Evolution of Mars

By W. Hartmann, Gerhard Neukum. 2001

1,182 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/8ec6aed35b63549fe7dc68a6fc61e0216c087399

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Citations in the corpus

The rayed crater Zunil and interpretations of small impact craters on Mars (2005, background): “The observation of a relatively steep SFD (b from 3.1 to 3.7) for small craters (∼0.2 to 1 km) on the asteroi Gaspra, where secondaries are thought to be absent d the very low escape velocity, has been considered st evidence for a steep primary SFD for craters smaller t 1 km (Neukum and Ivanov, 1994”
Sequence and timing of conditions on early Mars (2011, methodology): “At the Noachian–Hesperian boundary the impact rate may be a factor of 80 greater than rates at present (Neukum et al., 2001; Hartmann and Neukum, 2001).”
Constraints on the Martian lithosphere from gravity and topography data and implication for volcanism and possible mantle heterogeneities (2005, methodology): “As recent studies have highlighted the evidence for recent volcanic activity on Mars [Nyquist et al., 2001; Hartmann and Neukum, 2001; Neukum et al., 2004], the Martian mantle must be still active, and variations in either temperature or composition are likely to play an important role in the observ”
Tropical mountain glaciers on Mars: Altitude-dependence of ice accumulation, accumulation conditions, formation times, glacier dynamics, and implications for planetary spin-axis/orbital history (2007, background): “Impact crater size-frequency distributions on glacial deposits (Shean et al., 2006; Kadish et al., 2008), calibrated to impact flux (Hartmann and Neukum, 2001; Hartmann, 2005) provide estimates of deposit absolute ages and corresponding historical epochs.”
Redefinition of the crater-density and absolute-age boundaries for the chronostratigraphic system of Mars (2011, background): “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…”
A chronology of early Mars climatic evolution from impact crater degradation (2012, background): “There is a shift from model isochrons below 1 km, as usually observed in case of resurfacing [e.g., Hartmann and Neukum, 2001].”
Nonuniform cratering of the terrestrial planets (2008, background): “In essence, a fresh surface will accumulate craters at a given rate, and the number of craters per square kilometer can be converted to an approximate age (e.g., Neukum et al., 2001; Stöffler and Ryder, 2001; Hartmann and Neukum, 2001).”
EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, methodology): “These dating methods are imprecise, especially for younger Hesperian and Amazonian surfaces for which ages may be in error by a factor of 2 to 3 (Hartmann & Neukum 2001).”
Map-projection-independent crater size-frequency determination in GIS environments—New software tool for ArcGIS (2011, methodology): “Theoretical modelling and observational data of fluxes of crater-forming impactors for different parts of our solar system made it possible to calibrate this lunar chronology function for different terrestrial planets and satellites (e.g., Neukum et al., 2001a; Ivanov, 2001; Hartmann and Neukum, 200”
Geologic history of Mars (2010, background): “The Noachian period is estimated to have ended around 3.7 Gyr ago and the Hesperian period around 2.9– 3.3 Gyr ago (Ivanov, 2001; Hartmann and Neukum, 2001).”
Records of an ancient Martian magnetic field in ALH84001 (2001, background): “7 Ga) [59] inferred for the surfaces associated with the Martian crustal magnetizations.”
Origin and evolution of a cold-based tropical mountain glacier on Mars: The Pavonis Mons fan-shaped deposit (2005, methodology): “In addition, the Tharsis Montes fan-shaped deposits are primarily depositional features of Figure 31. Crater-counting data N(0.063)–N(0.75) from THEMIS daytime IR and VIS mosaics for the Pavonis fanshaped deposit plotted on the Ivanov [2001] isochrons derived from lunar crater count data by Neukum f”
Very recent and wide‐spread basaltic volcanism on Mars (2011, background): “and the impact‐cratering chronology model coefficients of Hartmann and Neukum [2001] .”
Context Camera Investigation on board the Mars Reconnaissance Orbiter (2007, methodology): “[50] With the advent of new data from MOC, THEMIS, and HRSC, plus MGS MOLA topography, there have been renewed investigations regarding the Martian cratering record and relation of craters to absolute age [Hartmann et al., 1999; Hartmann and Neukum, 2001; Neukum et al., 2004; Hartmann, 2005].”