Seasonal Flows in Asimov Crater
NASA/JPL/University of Arizona
Seasonal Flows in Asimov Crater
ESP_040485_1330  Science Theme: Mass Wasting Processes
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Seasonal flows called recurring slope lineae (RSL) grow down warm slopes in the summer, fade when they become inactive, then re-form the following year when the slopes warm up again from the Sun.

We see many of these RSL over the steep equator-facing slopes of the troughs within Asimov Crater, as illustrated in this cutout. However, just a few days later HiRISE imaged another steep equator-facing slope in Asimov crater, and no RSL are visible at all (ESP_040551_1330). These two slopes are very similar in slope angle, rockiness, and other properties seen by HiRISE.

Why are RSL present in one place but not another that appears so similar? RSL activity must be controlled by something that HiRISE can't detect, such as the presence of salts or groundwater. It is also possible that in future years, the RSL activity will appear or disappear on each slope.

Written by: Alfred McEwen (audio: Tre Gibbs)  (20 May 2015)
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Acquisition date
17 March 2015

Local Mars time:
14:26

Latitude (centered)
-46.840°

Longitude (East)
5.144°

Range to target site
256.9 km (160.6 miles)

Original image scale range
25.7 cm/pixel (with 1 x 1 binning) so objects ~77 cm across are resolved

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25 cm/pixel and North is up

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Equirectangular

Emission angle:
11.2°

Phase angle:
50.4°

Solar incidence angle
41°, with the Sun about 49° above the horizon

Solar longitude
309.5°, Northern Winter

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North azimuth:  96°
Sub-solar azimuth:  35.4°
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POSTSCRIPT
NASA’s Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, Calif., manages the Mars Reconnaissance Orbiter for NASA’s Science Mission Directorate, Washington. The HiRISE camera was built by Ball Aerospace and Technology Corporation and is operated by the University of Arizona.