Martian cratering 8: Isochron refinement and the chronology of Mars

By W. Hartmann. 2005

607 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/60e72a0a5326c1ecfb601b439a509aeccf9f7f90

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Citations in the corpus

The global martian volcanic evolutionary history (2009, background): “In recent years there has been an ongoing discussion (Hartmann, 2005) about the use of small craters in cratering statistics; specifically whether it is appropriate to count craters 300 m diameter because they might be distant secondary craters rather than primary craters (McEwen et al.”
THE IMPORTANCE OF SECONDARY CRATERING TO AGE CONSTRAINTS ON PLANETARY SURFACES (2006, background): “Hartmann (1999, 2005) has argued that counting both the primaries and what appear to be spatially random secondaries is acceptable, but offered no quantitative justification or methodology to define the uncertainties.”
Redefinition of the crater-density and absolute-age boundaries for the chronostratigraphic system of Mars (2011, methodology): “Therefore, the diversity of crater size–frequency distribution (SFD) shapes (most recently e.g., Ivanov, 2001; Hartmann, 2005) and the combination of fitting the crater SFD and translation to absolute ages has resulted in differing definitions of the epoch boundaries (Hartmann and Neukum, 2001).”
Geologic Constraints on Early Mars Climate (2018, methodology): “Absolute date estimates used in this paper, reproduced from Table 1 of Michael (2013) which in turn follows the Hartmann (2005) chronology.”
Selection of the InSight Landing Site (2017, background): “The average regolith gradation with depth can then be predicted by taking into account the cratering production functions and the age of the surface (Hartmann 2005).”
The current martian cratering rate (2010, methodology): “Unlike the Hartmann (2005) iteration, the Neukum PF was constructed for craters large enough not to be affected by the atmospheric passage of the projectile, so it does not include the ‘‘Popova correction’’ (Popova et al., 2003) that Hartmann made in 2005 for ablation during the projectile’s…”
The timing of martian valley network activity : Constraints from buffered crater counting (2008, methodology): “The cause of this discrepancy is the removal of small craters, which are more subject to infilling and/or erosion than their large counterparts (e.g., Hartmann and Neukum, 2001; Hartmann, 2005).”
Large impact crater histories of Mars: The effect of different model crater age techniques (2013, methodology): “The first stand – picking a system, Hartmann (2005) or Neukum et al. (2001) – is not one that can be taken at this time.”
Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, background): “Although quantitative crater counts have not been done within the smooth-floored craters,typicalexamples(e.g.,Figures10and11)haveonlya few small ( Hartmann, 2005 ], which coincides with the timing of volcanism implied by most of the Martian meteorites excluding Chassigny (180 Ma to 1.4 Ga) [McSween ”
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).”
Sequence of infilling events in Gale Crater, Mars: Results from morphology, stratigraphy, and mineralogy (2013, positive): “Taking into account that the Late Noachian is ranging from 3.85Ga to 3.57Ga [Hartmann, 2005; Werner and Tanaka, 2011] and the uncertainties of the measurement, we estimate the age of the Gale impact to range between ~3.55Ga and ~3.65Ga and hence to be Late Noachian/Early Hesperian.”
An overview of the 1985-2006 Mars Orbiter Camera science investigation (2010, neutral): “From these observations, Malin et al. (2006) noted that the modeled cratering rate described by Hartmann (2005) compares favorably with the observed, present-day cratering rate.”
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.”
Very recent and wide‐spread basaltic volcanism on Mars (2011, result): “These models are in contradiction to several studies, however, which seem to indicate ongoing volcanic activity, perhaps as recent as a few million years ago [Hartmann, 2005; Hartmann and Berman, 2000; Hartmann et al., 1999, 2008; Neukum et al., 2004; Vaucher et al., 2009a].”