Seasonal Flows on Warm Martian Slopes

  title={Seasonal Flows on Warm Martian Slopes},
  author={Alfred S. McEwen and Lujendra Ojha and Colin M. Dundas and Sarah S. Mattson and Shane Byrne and James J. Wray and Selby C. Cull and Scott L. Murchie and Nicolas Thomas and Virginia C. Gulick},
  pages={740 - 743}
Rare meter-scale slope features on Mars might be explained by transient flows of liquid salty water. Water probably flowed across ancient Mars, but whether it ever exists as a liquid on the surface today remains debatable. Recurring slope lineae (RSL) are narrow (0.5 to 5 meters), relatively dark markings on steep (25° to 40°) slopes; repeat images from the Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment show them to appear and incrementally grow during warm seasons and… 

Recurring slope lineae in equatorial regions of Mars

The presence of liquid water is a requirement of habitability on a planet. Possible indicators of liquid surface water on Mars include intermittent flow-like features observed on sloping terrains.

Formation of recurring slope lineae by liquid brines on present‐day Mars

Recurring Slope Lineae (RSL) are small scale seasonal flow features identified by Mars Reconnaissance Orbiter that present several interesting characteristics such as an albedo contrast, seasonal

Granular flows at recurring slope lineae on Mars indicate a limited role for liquid water

Recent liquid water flow on Mars has been proposed based on geomorphological features, such as gullies. Recurring slope lineae — seasonal flows that are darker than their surroundings — are candidate

The water content of recurring slope lineae on Mars

Observations of recurring slope lineae (RSL) from the High‐Resolution Imaging Science Experiment have been interpreted as present‐day, seasonally variable liquid water flows; however, orbital

A deep groundwater origin for recurring slope lineae on Mars

Observations and heat-flow modelling suggest that briny groundwater surfacing from fractures forms recurring slope lineae on Mars, and it is suggested that deep groundwater occasionally surfaces on Mars in present-day conditions.

Melt-water formed dark streaks on slopes of Haughton crater as possible Mars analogues

Abstract Haughton crater in the Canadian Arctic has been extensively used as a Mars (and lunar) analogue over the past 20 years. Here we report on small scale, dark, semi-seasonal slope streaks

HiRISE observations of Recurring Slope Lineae (RSL) during southern summer on Mars

High‐Resolution Thermal Environment of Recurring Slope Lineae in Palikir Crater, Mars, and Its Implications for Volatiles

A thermophysical model for rough terrain is developed that is capable of processing spatial domains of megapixel size. This computational advance makes it possible to characterize thermal



Indications of brine related local seepage phenomena on the northern hemisphere of Mars

Martian Slope Streaks Form Sporadically Throughout the Year

Introduction: Slope streaks are dark mass movements on Martian slopes, which occur only in areas of low thermal inertia and at low latitudes [1,2]. They first emerge as bold, elongated streaks, which

Present-Day Impact Cratering Rate and Contemporary Gully Activity on Mars

The Mars Global Surveyor Mars Orbiter Camera has acquired data that establish the present-day impact cratering rate and document new deposits formed by downslope movement of material in mid-latitude gullies on Mars, suggesting that liquid water flowed on the surface of Mars during the past decade.

Seasonal Erosion and Restoration of Mars’ Northern Polar Dunes

It is shown that martian dunes are subject to an additional modification process not found on Earth: springtime sublimation of Mars’ CO2 seasonal polar caps.

Subsurface ice on Mars with rough topography

High-latitude ground ice on Mars discovered by the Gamma Ray Spectrometer suite is thought to be thermally stable owing to the presence of vapor in the Martian atmosphere. However, local slopes can

Examination of gully sites on Mars with the shallow radar

[1] Martian gullies, found on steep slopes along broad mid-latitudinal bands, have morphologies resembling those of water-carved gullies on Earth and have been dated to <10 Ma. As such, one of the

Dynamic temperature fields under Mars landing sites and implications for supporting microbial life.

Thermal modeling has shown that 253 K is reached beneath the surface at diurnal peak heating for at least some parts of the year at each of these landing sites, which corresponds to the minimum found for specific terrestrial microorganisms.

New and recent gully activity on Mars as seen by HiRISE

Fresh‐appearing gully deposits are found at tens of sites in the southern hemisphere of Mars. These deposits have latitudinal and azimuthal dependences similar to the overall preferences of