HiRISE | Science in Motion: Recurring Slope Lineae in Equatorial Regions of Mars

Recurring Slope Lineae in Equatorial Regions of Mars

Alfred S. McEwen, Colin M. Dundas, Sarah S. Mattson, Anthony D. Toigo, Lujendra Ojha, James J. Wray, Matthew Chojnacki, Shane Byrne, Scott L. Murchie and Nicolas Thomas

ABSTRACT
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. These recurring slope lineae are narrow, dark markings on steep slopes that appear and incrementally lengthen during warm seasons on low-albedo surfaces. The lineae fade in cooler seasons and recur over multiple Mars years. Recurring slope lineae were initially reported to appear and lengthen at mid-latitudes in the late southern spring and summer and are more common on equator-facing slopes where and when the peak surface temperatures are higher. Here we report extensive recurring slope linea activity in equatorial regions of Mars, particularly in the deep canyons of Valles Marineris, from analysis of data acquired by the Mars Reconnaissance Orbiter. We observe the lineae to be most active in seasons when the slopes often face the sun. Expected peak temperatures suggest that activity may not depend solely on temperature. Although the origin of the recurring slope lineae remains an open question, our observations are consistent with intermittent flow of briny water. Such an origin suggests surprisingly abundant liquid water in some near-surface equatorial regions of Mars.

Nature Geoscience
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ANIMATED GIFS OF RSLs (Please note the animations may take a moment to load fully)
Heavily dissected hill in Juventae Chasm

Sequence of 5 HiRISE images of a heavily-dissected (eroded) hill in southern Juventae Chasm, Mars (latitude 4.7 degrees S, longitude 298.6 degrees E). This sequence is from the recently completed Mars Year (31), and RSL were also seen here in Mars Year 28, so they have recurred. The season of these images is late spring to early summer in the southern hemisphere, and include perihelion (Mars closest to the sun in its orbit). Activity is strongly concentrated on the south-facing slopes, which are the warmest slopes this time of year. The RSL are closely associated with “small” (for Mars) gullies. Images reduced to 1 m/pixel scale. (31MB)

RSL and darkening fans in East Coprates Chasm

Sequence of 6 images showing a small area of steep slopes with RSL activity (latitude 14.7 degrees S, longitude 304.6 degrees E). The sequence is in Mars Year 31, southern spring. Note that some of the fans that RSL flow over became darker and brighter over time (see also figure S2 of the supplementary material of the Nature Geoscience paper). There are many other such fans in this region that darkened and brightened at the same times. Image 0.25 m/pixel scale; scene 480 meters wide. (18MB)

RSL follow the sun in crater on Melas Chasm floor

Sequence of 8 images showing RSL forming first on the north-facing slope (bottom), then switching to the south-facing slope (top). This change occurred close to when the subsolar latitude moved from the north to the south of the latitude of this crater. In other words, RSL are most active on the slopes that receive more direct sunlight. There was also an episode of inactivity and fading of RSL on the south-facing slope, when the air over this region was especially dusty (Ls 235-246). Dusty air makes the daytime temperatures cooler, which may have temporarily stopped the RSL activity. (42MB)

RSL activity on complex topography in East Coprates Chasm

The use of digital terrain maps (DTMs), constructed from HiRISE stereo images, helps characterize the RSL phenomena. The images in other sequences have been DTM-projected to looking straight down on the surface, but here that have been projected to a view a person or rover on the surface could observe. This sequence of 6 DTM-projected images shows RSL forming and fading on west-facing slopes in east Coprates Chasma (latitude 14.7 degrees S, longitude 304.6 degrees E). North is to the left, and most slopes face south. Flows appear to form from the upper-most 100 meters along this ridge, suggesting very concentrated sources, possibly from the light- and mid-toned bedrock. Activity here is observed on all slope aspects and for the majority of the year, but RSL generally favor Sun-facing slopes. (13MB)

RSL and colorful fans along Coprates ridge

This site along Coprates ridge shows RSL on generally north-facing slopes in northern summer/southern winter (latitude 12.9 degrees S, longitude 295.5 degrees E). South is down, and most slopes face northwest. IRB color (near-infrared, red, and blue-green bandpasses displayed as red, green, and blue, respectively) with a min-max stretch illustrates the “greenish” fans and deposits associated with RSL. Two of these fans transition downslope into ripples (see also figure 2 of the Nature Geoscience paper). All of the lineae here and in the larger scene appear to originate from relatively bright bedrock outcrops. Note that some of the fans that RSL flow over became darker and brighter over time. Image is approximately 950 meters wide. (33MB)

Animated GIF captions by: Matt Chojnacki and Alfred McEwen

Image credit: NASA/JPL/University of Arizona