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• W45752571 abstract "Introduction: Slope streaks are ubiquitous albedo features in the tropical latitudes of Mars, typically occurring as elongated dark streaks below point sources and with narrow, fan-shaped morphologies [1,2]. Slope streaks represent one of the most active surface processes observed on Mars, with new streaks forming at a rate of up to 7% per Martian year per existing streak [3,4], yet their formation mechanism and their significance in the context of the present day nearsurface environment of Mars remain uncertain. The common interpretation for slope streaks is dry mass wasting in the form of ‘dust avalanches’, e.g., [1,5], although competing hypotheses involving aqueous processes have also been postulated based on the fluvial appearance of some streaks [6], their geomorphic relation with the slopes they occur on [7] and their morphological resemblance with Earth analogs in the form of liquid seepages in Antarctica [8]. In this study we use HiRISE [9] images, HRSC [10] multispectral data and CRISM [11] hyperspectral measurements to test these hypotheses, and to propose a new diagenetic model for slope streak formation on Mars as the precipitated solid residue left behind by short-term seepages of a brine. Results: HiRISE images of dark slope streaks in multiple locations (Fig. 1) reveal adjacent erosional scarps that expose a light-toned substrate beneath an apparently smooth thin dust mantle. These observations are not consistent with an erosional model such as dust avalanching, which would require exposure of a dark-toned rather than light-toned substrate. Furthermore, the HiRISE images also reveal that slope streaks crossing terrain boundaries typically maintain constant albedo and textural characteristics (Fig. 1c), which is more consistent with their formation through depositional rather than erosional processes. HRSC multispectral images show that the dark slope streaks lie outside the spectral mixing volume defined by adjacent unaffected dusty slopes, bedrock outcrops and shadow (Fig. 2), thus indicating that slope streaks represent a compositionally distinct scene element that cannot be explained as a linear mixture of the other scene elements described above. Sub-pixel roughness measurements obtained from HRSC stereo data (Fig. 3a) also reveal that dark streaks are rougher at <30-cm scales than their surrounding unaffected slopes. Nonetheless, HiRISE images of slope streaks in the shadow of large cliffs (Fig. 3b) reveal a similar albedo contrast between streaks and slope inside and outside the shadowed areas, indicating that the roughness differences between streaks and their surrounding are only a 2-order effect and that compositional differences are the primary reason for the observed albedo contrast. The HRSC roughness map (Fig. 3a) also suggests that streaks become smoother over time as the albedo contrast with their surrounding is reduced." @default.
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• W45752571 date "2008-03-01" @default.
• W45752571 modified "2023-09-23" @default.
• W45752571 title "New Observational Constraints on the Nature of Slope Streaks on Mars" @default.
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