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Origin of Fluvial Channels in the Walls of Juventae Chasma: Evidences of Groundwater Sapping? P

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Origin of Fluvial Channels in the Walls of Juventae Chasma: Evidences of Groundwater Sapping? P 47th Lunar and Planetary Science Conference (2016) 1878.pdf ORIGIN OF FLUVIAL CHANNELS IN THE WALLS OF JUVENTAE CHASMA: EVIDENCES OF GROUNDWATER SAPPING? P. Singh1, R. Sarkar1, I. Ganesh1 and A. Porwal1, 1Geology and Mineral Resources Group, CSRE, Indian Institute of Technology, Bombay, India ([email protected]) Introduction: Juventae Chasma is a deep box- Type IV: This type includes channels emanating from canyon located to the north of Valles Marineris. The gullies between the spurs on the chasma wall (Fig. 1d). main geological units of the chasma are chaotic terrain, They are mainly found in the southern wall of the four mounds of interior layered deposits (ILDs) and an chasma. These channels have shorter lengths ranging outflow channel. The presence of the outflow channel from 1-6 km and at places converge into a single chan- indicates that water played an important role in the nel. geological and geomorphological evolution of the Age determination: We estimated the ages of the chasma. In this paper, we report ground-water sapping geological units containing Type 1 and Type III chan- features from the wall of Juventae Chasma. We also delineate and characterize fluvial channels originating nels using crater size-frequency distributions. The re- from the chasma wall. This study was carried out using sults indicate that Type 1 channels are younger than panchromatic data from the CTX and digital terrain 790+- 200 Ma and Type III channels are younger than models from the HRSC onboard the MRO and MEX 620+-300 Ma. Type II and IV were left out because of respectively. considerable degradation of the containing units. Morphology of the Canyon Wall: The wall of Ju- Discussion: The presence of amphitheatre headed vantae Chasma is characterized by spur-and-gully fea- tributary canyons without upstream water sources tures. The absence of straight segments along the wall along the chasma wall indicate that groundwater sap- indicates a lack of structural/tectonic control. The ping is the possible mechanism for their formation [1]. south wall is characterized by curvilinear outlines with We observe different types of water-cut channels from the mean slope ranging between 20ᵒ and 30ᵒ. The different portions of the walls. These channels do not south-western part of the chasma wall shows amphithe- link to external sources of water and are associated ater-headed channels with V-shaped profiles, possibly formed by groundwater sapping [1]. The south-eastern with amphitheatre-headed canyons, pits or gullies. part of the wall contains relatively short and much These observations suggest the channels to have broader tributary canyons. A hook-shaped tributary formed due to local ground water sapping. canyon is present in the northern part of the chasma Large valley networks formed in the early history of wall. Mars [2, 3] indicate warm and wet climate; however Types of fluvial channels: We identify the follow- smaller fluvial features formed in the later age of the ing four types of fluvial channels indicating the pres- planet were possibly carved by subsurface water or ence of flowing water in the wall of Juventae chasma at melt of snow or permafrost. Such features reveal finer some stage in its geological history. details of the subsequent evolution of the Martian hy- Type I: They are relatively broad and long, single flow drology and climatic condition [4, 5]. The geomor- channels with a few short channels (4-5 km) flowing phology of the fluvial channels and sapping features into them. They occur on a collapse pit inside a crater present in the walls of Juventae Chasma point to the in the eastern wall of the chasma (Fig. 1a). presence of water either in the pore spaces or in the Type II: These fluvial channels are associated with the form of a confined aquifer. tributary canyons. They comprise broad channels that Crater-size-frequency distribution shows that these emerge from groundwater sapping and show headward channels have formed in the middle Amazonian- a time erosion on the chasma wall, sometimes cutting into the when the cryosphere became sufficient thick (~2 km) basalt plateau (Fig. 1b). to sustain a confined aquifer [6]. Presence of these Type III: This type of channel include dense networks channels would indicate recent water activity in the last of small branching channels, often mimicking the den- 1 Ga. The presence of rampart craters in the surround- dritic pattern. These channels are mostly found on the ing plateau also support occurrence of fluid in the sub- western wall of the chasma near the ILD Mound B surface [7]. (Fig. 1c). At places they are cut across by a younger network of broad channels. 47th Lunar and Planetary Science Conference (2016) 1878.pdf References: P.R. (2003) Nature 422, 45–48. [6] Clifford and Parker [1] Marra et al. (2014) Icarus, 232, 97-117 [2] Milton, (2001) Icarus, 154(1), 40-79. [7] Peulvast et al. (2001) D. J. (1973) J. Geophys. Res., 78, 4037–4047 [3] Carr, Geomorphology, 37(3), 329-352. M. H. (1996) Water on Mars, 229 pp., Oxford Univ. Acknowledgement: We thank Centre for Studies Press, New York. [4] Hanna, J.C. and Phillips, R.J. in Resources Engineering, IIT Bombay for their assis- (2005) J. Geophys. Res., 110, E01004. [5] Christensen, tance and financial support. Figure 1. Context mosaic image of Juventae chasma: (a) black continuous line shows the main channel, small discontinuous lines show other small channels joining the main channel; (b) channels coming out of a tributary; (c) arrows indicating dense networks of small branching channels and continuous lines are the younger network of broad channels (d) channels emerging from the gullies between the spurs. (All the images used in the figures are from CTX mosaic of Google Mars) .
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