Martian drainage densities

Carr, M. H.; Chuang, F. C.

doi:10.1029/97je00113

Cited by 119 publications

(121 citation statements)

References 21 publications

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“…2c by the low density of tributaries and the paucity of high-order streams that are not significantly different inside and outside the drainage basin boundaries. Further, drainage density is low when compared with typical terrestrial runoff environments (24,25).…”

Section: Stream Profiles On Marsmentioning

confidence: 99%

Drainage basins and channel incision on Mars

Aharonson

Zuber

Rothman

et al. 2002

Proc. Natl. Acad. Sci. U.S.A.

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Measurements acquired by the Mars Orbiter Laser Altimeter on board the Mars Global Surveyor indicate that large drainage systems on Mars have geomorphic characteristics inconsistent with prolonged erosion by surface runoff. We find the topography has not evolved to an expected equilibrium terrain form, even in areas where runoff incision has been previously interpreted. By analogy with terrestrial examples, groundwater sapping may have played an important role in the incision. Longitudinally flat floor segments may provide a direct indication of lithologic layers in the bedrock, altering subsurface hydrology. However, it is unlikely that floor levels are entirely due to inherited structures due to their planar cross-cutting relations. These conclusions are based on previously unavailable observations, including extensive piece-wise linear longitudinal profiles, frequent knickpoints, hanging valleys, and small basin concavity exponents.

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Section: Stream Profiles On Marsmentioning

confidence: 99%

Drainage basins and channel incision on Mars

Aharonson

Zuber

Rothman

et al. 2002

Proc. Natl. Acad. Sci. U.S.A.

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“…Coupled with high-resolution imagery data, it finally became possible to compare the density and location of valley networks with topography (Fig. IB), thus enabling tests of previous assertions that the drainage densities of valley networks were low (Fieri, 1976;Carr and Chuang, 1997) and the networks occurred as isolated features or in clusters (Gulick, 1998). Both observations are frequently cited in support of the assertion that the valley networks resulted from hydrothermally induced groundwater sapping.…”

Section: Fig 1 Our Understanding Of Valley Network Has Evolved As mentioning

confidence: 58%

“…This information can then be used to characterize a number of parameters useful for describing a valley network system {e.g., contributing area, relief, stream order, etc.). Although the techniques used in each study are slightly different, the general assessment is that the drainage densities of martian valley networks are several orders higher than previously deduced from Viking imagery data (Carr and Chuang, 1997). Despite this fact, it is not immediately clear whether these drainage densities are more comparable to terrestrial systems carved by surface runoff or groundwater sapping (R.A. Craddock and R.P.…”

Section: Fig 1 Our Understanding Of Valley Network Has Evolved As mentioning

confidence: 78%

Key Science Questions from the Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life

et al. 2005

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In October 2004, more than 130 terrestrial and planetary scientists met in Jackson Hole, WY, to discuss early Mars. The first billion years of martian geologic history is of particular interest because it is a period during which the planet was most active, after which a less dynamic period ensued that extends to the present day. The early activity left a fascinating geological record, which we are only beginning to unravel through direct observation and modeling. In considering this time period, questions outnumber answers, and one of the purposes of the meeting was to gather some of the best experts in the field to consider the current state of knowledge, ascertain which questions remain to be addressed, and identify the most promising approaches to addressing those questions. The purpose of this report is to document that discussion. Throughout the planet's first billion years, planetary-scale processes•including differentiation, hydrodynamic escape, volcanism, large impacts, erosion, and sedimentation•rapidly modified the atmosphere and crust. How did these processes operate, and what were their rates and interdependencies? The early environment was also characterized by both abundant liquid water and plentiful sources of energy, two of the most important conditions considered necessary for the origin of life. Where and when did the most habitable environments occur? Did life actually occupy them, and if so, has life persisted on Mars to the present? Our understanding of early Mars is critical to understanding how the planet we see today came to be.

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“…Glacial landforms identified in Viking images were considered to be a common type of landform in the Amazonian period (Carr 1996). In contrast, only weak evidence for liquid water during this period was reported, such as the presence of local outflow channels, whose catastrophic origin does not require a warmer climate.…”

Section: Episodic Fluvial Activity During the Amazonian Periodmentioning

confidence: 99%

“…At the same time, outflow channels were discovered in more recent terrains, like Chryse Planitia, east of Valles Marineris. They were interpreted as the signature of violent, episodic floods, possibly due to the rupture of sub-surface reservoirs under high artesian pressure (Carr 1995(Carr , 1996. These two types of landforms still define two end-members in martian fluvial activity.…”

Section: Fluvial Landformsmentioning

confidence: 99%

Mars: a small terrestrial planet

Mangold

Baratoux

Witasse

et al. 2016

Astron Astrophys Rev

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Mars is characterized by geological landforms familiar to terrestrial geologists. It has a tenuous atmosphere that evolved differently from that of Earth and Venus and a differentiated inner structure. Our knowledge of the structure and evolution of Mars has strongly improved thanks to a huge amount of data of various types (visible and infrared imagery, altimetry, radar, chemistry, etc) acquired by a dozen of missions over the last two decades. In situ data have provided ground truth for remote-sensing data and have opened a new era in the study of Mars geology. While large sections of Mars science have made progress and new topics have emerged, a major question in Mars exploration-the possibility of past or present life-is still unsolved. Without entering into the debate around the presence of life traces, our review develops various topics of Mars science to help the search of life on Mars, building on the most recent discoveries, going from the exosphere to the interior structure, from the magmatic evolution to the currently active processes, including the fate of volatiles and especially liquid water.

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Martian drainage densities

Cited by 119 publications

References 21 publications

Drainage basins and channel incision on Mars

Drainage basins and channel incision on Mars

Key Science Questions from the Second Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life

Mars: a small terrestrial planet

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