Evidence for Multiple Superposed Fluvial Deposits Within Reuyl Crater, Mars

Vijayan, S.; Sinha, Rishitosh K.; Harish,; Anilkumar, Ritu

doi:10.1029/2019je006136

Cited by 7 publications

(3 citation statements)

References 96 publications

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“… Graphical representation of model ages derived for each crater with and without using the ASCI, corresponding respectively to the green and the puple curve. The blue bar corresponds to the age reported in the literature and derived from isochron fitting from manual count: (a) Werner et al., 2014; (b) Mouginis‐Mark et al., 2012; (d) Lagain et al., 2020; (e) Sun and Miliken, 2014; (f) Robbins et al., 2013; (g) Tornabene et al., 2012; (h) Berman et al., 2011; (i) Fairen et al., 2010; (j) Mangold et al., 2012; (k) Vijayan et al., 2020. Large blue bars correspond to an interval of ages reported in the literature by additional authors: (c) W. K. Hartmann et al., 2010 based on isochron fitting; (g) Tornabene et al., 2012 report a modeled crater‐retention age consistent with late Noachian or Noachian–Hesperian time, roughly spanning a period from 3.5 and 3.8 Ga. ASCI, algorithm for the secondary crater identification.…”

Section: Results Age Derivation and Validationmentioning

confidence: 99%

Model Age Derivation of Large Martian Impact Craters, Using Automatic Crater Counting Methods

Lagain

Servis

Benedix

et al. 2021

Earth and Space Science

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Determining when an impact crater formed is a complex and tedious task. However, this knowledge is crucial to understanding the geological history of planetary bodies and, more specifically, gives information on erosion rate measurements, meteorite ejection location, impact flux evolution and the loss of a magnetic field. The derivation of an individual crater's age is currently performed through manual counting. Because crater size scales as a power law, this method is limited to small (and/or young) surface areas and, in the case of the derivation of crater emplacement age, to a small set of impact craters. Here, we used a Crater Detection Algorithm, specifically retrained to detect small impact craters on large‐ and high‐resolution imagery data set to solve this issue. We applied it to a global, 5 m/pixel resolution mosaic of Mars. Here, we test the use of this data set to date 10 large impact craters. We developed a cluster analysis tool in order to distinguish potential secondary crater clusters from the primary crater population. We then use this, filtered, crater population to date each large impact crater and evaluate our results against literature ages. We found that automated counting filtered through clustering analysis produced similar model ages to manual counts. This technique can now be expanded to much wider crater dating surveys, and by extension to any other kind of Martian surface. We anticipate that this new tool will considerably expand our knowledge of the geological events that have shaped the surface of Mars, their timing and duration.

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Section: Results Age Derivation and Validationmentioning

confidence: 99%

Model Age Derivation of Large Martian Impact Craters, Using Automatic Crater Counting Methods

Lagain

Servis

Benedix

et al. 2021

Earth and Space Science

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“…The basin topography and the fans observed at multiple elevations suggest that the base level of this water body changed over time (Figure 13), which is consistent with a scenario that involves the episodic formation of sedimentary structures associated with fluctuations in the water body. Such a scenario was recently proposed based on in situ observations at the Jezero crater and from orbiter data (e.g., Davis et al., 2018; Grau Galofre et al., 2020; Hughes et al., 2019; Mangold et al., 2021a; Vijayan et al., 2020). The elevation of these fans indicates that the lake within the crater could have exhibited up to three distinct water levels during its formation, as for the Gale crater (Palucis et al., 2016).…”

Section: Discussionmentioning

confidence: 98%

Prolonged Record of Hydroclimatic Changes at Antoniadi Crater, Mars

et al. 2023

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The first billion years of Martian geologic history consisted of surface environments and landscapes dramatically different from those seen today, with flowing liquid water sculpting river channels and ponding to form bodies of water. However, the hydro‐climatic context, the frequency, and the duration under which these systems existed remain uncertain. Addressing these fundamental questions may improve our understanding of early Mars climate. Here, we reconstruct a long‐lived archive consisting of an array of fluvial systems inside the Antoniadi crater––one of the largest lake basins on Mars (9.58 × 104 km2). We found that the fluvial activity occurred throughout four major intermittent active intervals during the Late Noachian to Early Amazonian (∼3.7 to >2.4 Ga). This resulted in at least two major lakes, which formed during periods of markedly increased surface runoff production. The record of these four riverine phases is preserved in fluvial ridges, valley networks, back‐stepping or down‐stepping fan‐shaped landforms, and terrace‐like formations within an outlet canyon. These morphologies point to lake‐controlled base‐level fluctuations suggestive of episodic precipitation‐fed surface runoff punctuated by intermittent catastrophic floods that were capable of breaching crater‐lake rims and incising outlet canyons. Fluvial‐deposit thickness, junction angles of channels, and lake morphometry suggest that riverine systems lasted at least 103–106 years and episodically occurred under primarily arid and semi‐arid climates. These findings place new regional constraints on the fluvial frequency, longevity, and climatic regime of one of the largest Martian lakes, thereby bolstering the hypothesis that episodic warming likely punctuated the planet's early history.

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“…Rainfall onto the ejecta has been proposed as a formation mechanism for incised networks surrounding other impact craters on Mars such as Mojave and Reuyl (Goddard et al, 2014; Vijayan et al, 2020). The Mojave impact site is a particularly good comparison to Hale crater, as both Hale and Mojave crater are located within outflow channels theorized to be a major water conduits in the past, so similar mechanisms for forming these linear depressions are considered.…”

Section: Discussion and Analysismentioning

confidence: 99%

Postimpact Evolution of the Southern Hale Crater Ejecta, Mars

et al. 2020

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As one of the youngest large (>100 km wide) impacts on Mars, Hale crater offers a unique opportunity to observe well‐preserved deposits of Mars' former interior. We utilize visible imagery (Context Camera [CTX] and High Resolution Imaging Science Experiment [HiRISE]) and elevation data (Mars Orbiter Laser Altimeter [MOLA], High Resolution Stereo Camera [HRSC], and HiRISE stereo pairs) to examine the region south of Hale crater, which contains the greatest density of landforms caused by with the impact. Linear depressions, mounds, and polygons indicate that the ejecta material contained volatiles and underwent substantial postimpact geomorphic evolution after it was emplaced. Ejecta landform formation was facilitated by volatiles, likely water ice displaced from the subsurface during the impact, contained within the material. We suggest that the ejecta flowed into valleys where it acted in a manner similar to terrestrial debris flows, leaving mounds, high‐standing deposits, lobate flow margins, and fan structures. Continued flow and settling of the ejecta then caused deposit dewatering, producing networks of linear depressions, particularly in places where the flows of ejecta were constricted. However, these landforms are not present everywhere, and their formation was likely influenced by topography. This work highlights that, while volatiles were present over much of Hale crater's ejecta blanket, the surface expression of them is spatially variable on local and regional scales.

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Evidence for Multiple Superposed Fluvial Deposits Within Reuyl Crater, Mars

Cited by 7 publications

References 96 publications

Model Age Derivation of Large Martian Impact Craters, Using Automatic Crater Counting Methods

Model Age Derivation of Large Martian Impact Craters, Using Automatic Crater Counting Methods

Prolonged Record of Hydroclimatic Changes at Antoniadi Crater, Mars

Postimpact Evolution of the Southern Hale Crater Ejecta, Mars

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