Circumferential depressions enclosing mesas and plateaus in the northern Kasei Valles and in the Tartarus Colles regions of Mars are interpreted as indicators of the former extent of lobate debris aprons, thought to be mixtures of ice and clastic particles. These former lobate debris aprons existed about 1 Ga ago and were embayed by lavas or other flow deposits. After the lobate debris aprons had been removed by sublimation and deflation, topographic depressions with a depth of 50 m and a width of several kilometers were left behind between the mesa or plateau scarp and the solidified flow materials. These depressions or moats are located equatorward of ±30° at significantly lower latitudes than generally observed for occurrences of modern, intact lobate debris aprons. This observation provides evidence that the paleoclimate at that time was different than today, probably due to a higher averaged obliquity of the planet's rotational axis.
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 Lobate debris aprons (LDA) are distinctive geomorphic landforms showing possible evidence for the creep and deformation of ice-rich debris in Martian midlatitudes [e.g., Carr and Schaber, 1977; Squyres, 1978, 1979; Lucchitta, 1984]. They occur predominantly at and near the northern hemispheric dichotomy escarpment and at margins of the southern hemispheric impact basins of Mars. LDA typically extend for up to 20 km from mesas or plateau scarps and show distinct flow lobes in plan view and convex upward profiles in cross section with steep termini [Mangold and Allemand, 2001; Pierce and Crown, 2003; Li et al., 2005; Chuang and Crown, 2005; Crown et al., 2006]. Where LDA are confined in broad and narrow valleys, they are termed lineated valley fill and show a particular surface texture characterized by generally valley-parallel lineations [e.g., Kress et al., 2006; Head et al., 2006b, 2006a]. A third type of landform which is genetically connected to creep of ice and debris is termed concentric crater fill and is characterized by creep of material downward along the inner slopes of impact craters. LDA were first described in detail by Carr and Schaber  and Squyres [1978, 1979], who ascribed them to downslope transport of erosional debris mixed with ice, analogous to terrestrial rock glaciers [e.g., Wahrhaftig and Cox, 1959; Barsch, 1996; Whalley and Azizi, 2003]. Squyres  and Squyres and Carr  mapped the global distribution of LDA and found a strong concentration in two latitudinal bands with a width of 25°, centered at 40°N and 45°S. They concluded that this latitudinal dependence implies a climatic influence on the formation of lobate debris aprons. Beside these macroscale landforms, a concentration of small-scale viscous flow features in the same latitudinal belts was later observed by Milliken et al.  on high-resolution Mars Orbiter Camera (MOC) data. Virtually no viscous flow features were reported equatorward of 30°, although possible glacial landforms were reported from tropical regions on Mars. These are mainly located westward of the Tharsis Montes and Olympus Mons [e.g., Lucchitta, 1981; Head and Marchant, 2003; Head et al., 2005; Shean et al., 2005; Milkovich et al., 2006; Shean et al., 2007], and are morphologically distinct from LDA. They seem rather to be the result of orographically induced accumulation of ice [Forget et al., 2006] and are not widespread phenomena like LDA. It has been shown first by Squyres  on the basis of photoclinometry and later by Mangold and Allemand  as well as Li et al.  on the basis of MOLA topographic profiles that the cross section shape of LDA can be approximated by the flow law of polycrystalline ice [Glen, 1953] and the flow relation of ice [Vialov, 1958] as done by Paterson  for terrestrial ice sheets. Colaprete and Jakosky  modeled flow of ice under Martian conditions and found that (1) temperatures 20 to 40 K higher than present average midlatitude temperatures (∼210 K), (2) ice contents ≥80%, and (3) net accumulation rates of ≥1 cm a−1 are required to create LDA of the observed size.
 In this study, we analyze unusual moats around mesas and along topographic scarps which resemble the shapes of lobate debris aprons in plan view, using image data (MOC, THEMIS, HRSC) and PEDR (Precision Data Experiment Record) MOLA topographic profiles (Figures 1 and 2). We present morphological evidence for the existence of former LDA, which emplaced equatorward of 30°N more than 1 Ga ago, and draw conclusions for the paleoclimate at that time.
2. Geologic Settings
 The main focus of our study is on topographic depressions, henceforth called moats, which enclose mesas or are parallel to steep topographic scarps (Figure 1). These moats are located in northern Kasei Valles, the largest outflow channel on Mars [e.g., Baker and Kochel, 1979]. The study area was geologically mapped at global scale by Scott and Tanaka , at regional scale by Rotto and Tanaka , and partly at local scale by Chapman et al. . Moats occur on a flat-lying terrace, which is situated north of Kasei Valles' main channels and south of the Hesperian ridged plains of Tempe Terra. The surface of the western part of this terrace was mapped as Amazonian-aged lava flows associated with Tharsis volcanism (unit At4), while the eastern part was interpreted as eroded channel floor (unit Hchh) [Rotto and Tanaka, 1995]. A geomorphologic map depicting some of the moats in their geologic context is shown in Figure 3. A distinct, step-like topographic scarp with a height of more than 1000 m separates the terrace from the plateau of Tempe Terra in the north (ridged plains material; units Hr and Hrd). Several mesas (inselberge, e.g., Labeatis Mensa) with heights of several 100 m to 1000 m are distributed on this terrace, mainly in its western part. These mesa surfaces also consist of Hesperian ridged plains material. The terrace itself slopes very gently (∼0.13°) toward the northeast (western part) and east (eastern part).
3. Morphology and Distribution
 Image data show a topographic scarp facing steep and high topographic walls of mesas or plateau margins (Figure 4a). The outlines of these depressions have shapes and sizes in plan view that are identical to the outlines of intact lobate debris aprons (Figure 4b) as confirmed by area measurements on isolated remnants and aprons which show a mean size ratio of 2.5 (ranging from 1.5 to 3.5), closely comparing to values obtained for intact remnants and debris aprons in Tempe Terra [Gasselt et al., 2003]. The topographic depression between the scarp and the mesa walls typically has a depth of more than 50 m (Figures 4c–4d). The floor of this depression is almost flat, and the topographic slope rising toward the mesa walls is less than 0.4°. In contrast, the surfaces of intact lobate debris aprons have slopes of around 1° to >12° [Pierce and Crown, 2003; Carr, 2001; Gasselt et al., 2003] (Figure 4e). At several locations, the scarps display a lobate morphology. At least at one moat around a mesa centered at 28.02°N and 286.32°E, a high-resolution MOC image (M12-01407) shows that the scarp has an elevated margin.
 Topographic depressions very similar to the examples shown in Figure 1 exist around mesas and parallel to the southern plateau margins of Tempe Terra. They occur at latitudes between 25°N and 31°N, and between 281°E and 301°E (Figure 5). These locations are distinctively south of the locations of modern and intact LDA previously mapped by Squyres  and Squyres and Carr  (Figure 6). They are also south of the latitude belts at which Kreslavsky and Head  and Mustard et al.  found evidence for young mantling deposits indicative of a recent climate change. Both studies give a lower latitude limit of 30°N for these mantling deposits in the northern hemisphere, although Mustard et al.  note that such deposits can be found at 25°S in the southern hemisphere.
 In order to find out if this phenomenon is global, we searched for comparable moats at similar or even lower latitudes, where relatively young lava or sediment has embayed mesas and topographic scarps (e.g., in Elysium Planitia or at the southern parts of the Phlegra Montes). Several examples, though less developed than in Kasei Valles, were found around small knobs and mesas in the Tartarus Colles region, east of the Elysium volcanic rise (Figure 7). They are embayed by Early Amazonian lava flows of the Elysium volcanic region (unit AHEe by Tanaka et al. ) and by Late Amazonian lava flows in Marte Vallis (unit AEc3 by Tanaka et al. ). The locations of these samples are between 24°N and 29°N latitude (Figure 6). These moats are different from moats around knobs in the flood tract of Grjotá Valles, also in roughly the same region east of Elysium, but located more southward (at latitudes of 14°S to 16°S). The moats there have different shapes in plan view, are smaller, and are ascribed to erosion by floodwaters [Burr and Parker, 2006].
 The basement of the study area consists of Hesperian-aged ridged plains [Rotto and Tanaka, 1995] (units ps and epm in Figure 3). The events that incised Kasei Valles eroded these plains down to the grooved valley floor (unit gvf in Figure 3). The material that flooded the valley floor in northern Kasei Valles and embayed the ancient lobate debris aprons (unit fm in Figure 3) is stratigraphically higher than the valley floor and therefore younger. Its age was determined by Lanz [2003, p. 137], as 1.1 Ga on the basis of crater counts, using the production function of Ivanov  and the cratering model of Hartmann and Neukum  to derive absolute model ages. We performed own crater counts (see Figure 3 for location of counting area), using the same techniques, and obtain an absolute crater model age of 1 Ga to 1.6 Ga (Figure 8). The lava emplacement in the Tartarus Colles region was determined to be of Early Amazonian age in the western parts and Late Amazonian age in the eastern parts (Marte Vallis) [Tanaka et al., 2005].
 On the basis of the striking morphological similarity with modern LDA, we interpret the moats around the mesas and along the plateau scarps as an indication of the extents of former lobate debris aprons. Several scenarios could explain the current-day existence of moats at the sites of former debris aprons: Material flowing down from the Tharsis rise in the southwest could have flooded the floor of northern Kasei Valles no later than 1 Ga ago. This material could have consisted of lava flows [Rotto and Tanaka, 1995] and/or debris flows like lahars. Lahars have been proposed by several authors in the Elysium [e.g., Christiansen, 1989; Russell and Head, 2003] and Tharsis [e.g., Tanaka, 1990a] regions, and they have also been suggested to account for deposits in several outflow channels, including Kasei Valles [Tanaka, 1990b]. The study area in northern Kasei Valles is located far away from volcanic source regions, but a runout distance of more than 1000 km has been reported from suggested megalahars on the northwestern slope of the Elysium volcanic rise [Christiansen, 1989]. Where the flooding material terminated against lobate debris aprons and solidified, it formed a steep scarp. This phenomenon is well known for lava flows on the Earth. Examples can be found in (1) the Garibaldi Volcanic Belt in British Columbia (Canada), where lavas from high-altitude vents flowed downhill to be impounded against ice [Matthews, 1952], (2) at the Llangorse volcanic field in northern British Columbia (Canada) [Harder and Russell, 2007], or (3) at Mount Rainier (Washington), where lava flows were emplaced between valley glaciers and remain as topographic ridges after the glaciers retreated [Lescinsky and Sisson, 1998]. The phenomenon has also been observed for the case of Mars: In a similar way, lava flows seem to have banked against the glacier that might have been present at Pavonis Mons [see Shean et al., 2005, Figure 23]. Indeed, typical lobate terminations of possible lava flows can be observed in new image data (Figure 9a). An origin of the flooding material as lahars might be supported by the observation of several channels in the immediate vicinity of the moats (Figure 9b), which might have been formed by dewatering of water-rich lahar deposits. However, it cannot be excluded that the channels were carved by the latest and very minor stages of Kasei Valles outflow activity. Finally, erosion beneath the former lobate debris aprons might also have contributed to the formation of the moats, and the elevated margins of the scarps at several locations (e.g., Figure 1e) might be interpreted as push moraines. On the basis of the strong evidence for lobate lava flow terminations (Figure 9a) we favor lava flows as the most likely material to preserve the moats, although we cannot rule out other hypotheses.
 We conclude that the combination of relatively young lava (and/or debris flows) and the occurrence of topographic relief is particularly suitable to create these depressions. Lobate debris aprons might have formed in the past at other places in low latitudes as well, but were not preserved by embaying lava flows or other deposits like mudflows.
 After LDA were removed by thermokarstic degradation through the sublimation of ice and deflation of detritus [Mangold, 2003; Crown et al., 2003; Pierce and Crown, 2003; see also Head et al., 2005, Figure 1], which shows fretted pits and depressions that suggest the former presence of ice), the solidified lava front remains as a free-standing topographic cliff (Figure 10). The same moats were first mentioned by Lucchitta and Chapman  and later described by Chapman and Scott  and Chapman et al. , who used photoclinometric profiles to measure a depth of the moats of about 40 m and noted that the moats have flat floors. They ascribed the moats to lava flows that “terminated upward against former slopes at the base of talus material,” and suggest that the talus might have consisted of fine detritus and ice, which was subsequently deflated and melted, respectively. This interpretation does not explicitly mention LDA, but is in line with our hypothesis. If this schematic model is correct, it would also imply that modern LDA are indeed ice-rich deposits analogous to rock glaciers [Barsch, 1996]. Since the use of the term rock glacier on Mars is problematic, because of the difficulty that rock glaciers on Earth can form in several ways [Whalley and Azizi, 2003], we note here that by using this term we do not intend to favor a specific origin. Rather, we use it as a nongeneric term to refer to a tongue-like or lobate body resembling a small glacier, a definition that is derived from, but more general than, the definitions given by, e.g., Washburn  or Barsch , and would for this purpose also include debris-covered glaciers [e.g., Head et al., 2006b].
 The almost flat floor of the moats suggests that the entire amount of the material originally constituting the LDA has been removed. This fact has one or more of the following implications: Either the LDA had a very high percentage of ice that sublimated away, Kasei floodwaters eroded the friable materials, or the clastic fraction of the LDA consisted mainly of very fine material, i.e., dust-sized particles (comparable to loess), which could be easily removed by wind. If coarse clastic particles (coarser than sand-sized) had made up a significant fraction of the former LDA, relics of that material should still be seen on the floor since the fine material is more effectively removed by wind [e.g., Armstrong and Leovy, 2005]. Mangold and Allemand  have pointed out that the volumes of some LDA are too large to have been derived from rockfalls from the associated mesas. A high ice content and/or a significant content of atmospheric dust in the total volumes of these LDA would not only explain their relatively large volume with respect to the associated mesa. The small particle sizes implied by atmospheric dust would also explain the almost complete loss of material and the remaining flat floors, since these small-sized particles would be more easily eroded by wind than coarser-grained materials.
 A very high ice content is consistent with the modeling results of Colaprete and Jakosky  and Li et al. , which show that a high content of solid particles in rock glaciers prevents flow. Since the former lobate debris aprons seem to have flowed from the mesa radially outward, a high ice content might have facilitated this flow. If modern LDA have a comparable morphology to the ancient LDA in northern Kasei Valles, the contact between the LDA and the underlying bedrock should also be flat. This could be tested with the Shallow Subsurface Radar (SHARAD) on the Mars Reconnaissance Orbiter (MRO) [Seu et al., 2004], which has a horizontal resolution between 0.3 km and 3 km and a vertical resolution of 15 m in free space (better than 10 m in Mars' subsurface), sufficient to resolve the dimensions of LDA.
 Virtually all modern and intact LDA are located poleward of ±30°. This distribution is thought to reflect the influence of climatic conditions on the formation of features indicative of creep of ice and debris. The climate on Mars is controlled by the obliquity of the planet's rotational axis and by the orbital parameters eccentricity and precession [e.g., Murray et al., 1973; Pollack, 1979; Toon et al., 1980; Jakosky et al., 1995; Laskar et al., 2004]. At higher obliquities than today (∼25°), ground ice becomes stable even in equatorial latitudes [e.g., Mellon and Jakosky, 1995]. It was also shown by climate modeling that prolonged periods of higher obliquity lead to a mobilization of volatiles at the poles and to precipitation at low latitudes [Levrard et al., 2004; Forget et al., 2006]. The obliquity of Mars is variable but cannot be reliably predicted backward in time for more than about 107 years due to its chaotic behavior [Touma and Wisdom, 1993; Laskar and Robutel, 1993]. However, recent calculations suggest that the averaged obliquity over 5 Ga was probably almost 40° [Laskar et al., 2004], a value that would allow ground ice to be stable globally. Our results indicate the formation of LDA and the stability of ground ice equatorward of ±30° more than 1 Ga ago and are therefore consistent with such models of the evolution of Mars' obliquity that predict an averaged higher obliquity [Laskar et al., 2004]. Higher obliquities in the past could have lead to precipitation of snow at low latitudes, where LDA formed because ground ice would have been stable. After the embayment of LDA by lava flows, the disappearance of the LDA would have been triggered by a decrease in the obliquity and the associated instability of ground ice at low latitudes. Periodic variations of the obliquity in the past might have caused the formation and entire removal by wind of LDA many times in the past, as suggested earlier by Lucchitta . New image data suggest that climate change may have occurred (and LDA were removed) during emplacement of lava flows or sedimentary materials like lahars (unit At4 as mapped by Rotto and Tanaka ), as some younger lava flows can be observed that flow into the topographic depressions of the moats (Figure 9a).
 1. Topographic depressions around mesas and along the base of plateau scarps in the northern Kasei Valles region are interpreted as areas previously occupied by lobate debris aprons, which are generally considered to consist of mixtures of ice and debris, analogous to terrestrial rock glaciers. Lava flows and/or debris flows (lahars) embayed former LDA, and after removal of the LDA material through the complete loss of volatiles and deflation of the debris constituents, the solidified lava front preserved the “fingerprints” of ancient LDA.
 2. Very similar landforms in the Tartarus Colles region between 24°N and 29°N are also interpreted as the relics of former lobate debris aprons. They are embayed by early Amazonian lava flows from the Elysium rise and by late Amazonian lava flows covering the Marte Vallis area.
 3. The flat floors of these moats indicate that nearly the entire material of the former LDA has been removed. This implies a very high ice content of the former LDA, or a predominance of relatively small-sized particles in the debris of the LDA, which could easily be removed by deflation, or both. This part of our hypothesis can be tested by data that will be obtained with the radar experiment SHARAD onboard NASA's Mars Reconnaissance Orbiter mission: If modern LDA are similar to the ancient LDA that were analyzed in this study, the high ice content of the LDA should only weakly attenuate the radar signals and allow them to penetrate down to the underlying substrate. Therefore the bottom of the LDA should be visible, analogous to the underlying substrate beneath the south polar caps in MARSIS data [Plaut et al., 2007].
 4. The former LDA existed around 1 Ga ago at latitudes between 25°N and 30°N, which is equatorward of the latitudinal belts where modern LDA are observed today. The occurrence of ancient rock glaciers at these latitudes can be explained by a higher than present paleo-obliquity, which is consistent with recent modeling of the obliquity evolution indicating an averaged obliquity of nearly 40° over 5 Ga [Laskar et al., 2004], in accordance to assumptions by Lucchitta  and Head et al. .
 5. Our observations suggest that the surface of Mars might have been repeatedly affected by the effects of climate changes leading to LDA formation and destruction in the past [Lucchitta, 1984] and that glacial and periglacial processes might have had a significant impact in landscape genesis even at latitudes lower than 30° over a large fraction of Mars' geologic history.
 We thank the HRSC Experiment Teams at DLR Berlin and Freie Universität Berlin as well as the Mars Express Project Teams at ESTEC and ESOC for their successful planning and acquisition of data as well as for making the processed data available to the HRSC Team. We acknowledge the effort of the HRSC Co-Investigator Team members and their associates who have contributed to this investigation in the preparatory phase and in scientific discussions within the Team. We also appreciate the efforts of the MOLA, MOC, and THEMIS teams to make their data available. We appreciate helpful comments by Baerbel Lucchitta on an earlier version of the manuscript. Detailed and insightful reviews by N. Mangold, D. Crown, and an anonymous reviewer helped to improve the manuscript. This work forms part of the HRSC Experiment of the ESA Mars Express Mission and has been supported by the German Space Agency (DLR) on behalf of the German Federal Ministry of Education and Research (BMBF).