Statistics – Computation
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..635m&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Statistics
Computation
Scientific paper
Introduction The outflow channels Dao and Niger Valles are located at the eastern rim of the 2000-km diameter Hellas Planitia impact basin, in a transition zone with ancient cratered terrain and the volcanoes Hadriaca and Tyrrhena Patera (Hesperia Planum) on the one hand and fluvial, mass-wasting and aeolian deposits on the other hand [1]. Dao and Niger have alcove-shaped source regions similar to the chaotic terrains found in the Margaritifer Terra region, with flat floors, landslide morphologies and small, chaotically distributed isolated mounds. As [2] pointed out, the intrusion of volcanic material could be responsible for the release of pressurized water that can carry loose material away. This process could than have created a depression and an associated outflow channel. In contrast to [2] who made their calculations for Aromatum Chaos and Ravi Vallis, we have focused on Dao and Niger Valles for investigation, since they are spatially related to the nearby Hadriaca Patera. Heat-triggered outflow events seem likely. We follow the generally accepted assumption that water was the main erosional agent [3]. Furthermore we take into account that multiple floods with different volumes are more likely than a single event because of repressurization of an aquifer [4]. Background Hadriaca Patera Hadriaca Patera is among the oldest central-vent volcanoes on Mars, a low-relief volcano with a central caldera complex which consists predominantly of pyroclastic material. The erosional structure of degraded valleys on its flanks is indicative of dissection by a combination of groundwater sapping and surface runoff, attributed to a hydromagmatic eruption scenario [5]. Dao Vallis Dao Vallis is interpreted as collapse region of volcanic and sedimentary plains that have been eroded by surface and subsurface flow [5]. The approximately radial alignment to Hellas is interpreted as following deep-seated structural weakness zones generated by the impact. Small grabens and fractures parallel to the channel margins are considered to be the result of extensional deformation. Two smoothfloored collapse depressions, representing source areas, cut into the flanks of Hadriaca Patera (Ausonia and Peraea Cavus) and are connected to Dao Vallis by a region of irregular valley floor materials. These regions are all bounded by steep scarps and are interpreted to be collapse depressions in water- or ice-rich materials. Linear and curvilinear features that are approximately parallel to the channel walls are seen in some parts of the channel floors. The channel walls show typical spur-and-gully morphology. It has been suggested that gullies can be exposed by a removal of semi-competent mantling deposits along the walls of Dao Vallis. The walls could either be a source of volatiles or provide an insulating layer [6]. A possible sedimentary deposit is observed on the floor of Hellas near the terminus of Dao Vallis [1]. Geologic evolution of the eastern rim of Hellas The oldest geologic materials result from the basin-forming impact and consist of the Noachian basin rim unit and mountainous materials. Volcanism began in the late Noachian or Early Hesperian epoch with the formation of the highland paterae. The low shields of Hadriaca and Tyrrhena Patera are interpreted to be composed primarily of pyroclastic flows. The distribution of flank materials at Hadriaca Patera can be attributed to the emplacement of gravity-driven pyroclastic flow, which is in contrast to the caldera-filling material and implies a transition from explosive to effusive volcanism at the highland paterae [5]. Substantial modification of the cratered highlands characterizes the Hesperian Period, with the formation of the smooth plateau materials, predominantly sedimentary plains-infilling low-lying intermontane areas. Continuation of this style of erosion extended into the Amazonian Period with the emplacement of debris aprons. The channels on the flanks of Hadriaca Patera are clearly truncated by Dao Vallis and appear to be truncated by the channeled plains, indicating that the erosion of Hadriaca Patera preceded erosion on the plains [1]. Data sets and additional information For the eastern-Hellas region a sufficient HRSC coverage exists. In addition, age estimates for the channel floors and the surrounding plains are available [7]. For detailed studies we processed MOC and HIRISE images also. Moreover, a detailed geologic map of the Hellas region has been made [8] which was utilized to constrain the channel boundaries and the main branches. Computations are actually done with MOLA data, but will be further improved by a high resolution mosaic DTM created out of HRSC stereo data of the eastern Hellas area. Water flow experiments within a Mars Simulation Chamber conducted at the Open University London, Department of Earth and Environmental Sciences (pers. comm.), suggest a complex interaction of phase changes (boiling and freezing) which have to be kept in mind when modeling the discharge of water from the subsurface. Such experiments will be improved in further investigations to give a better input to numerical modeling. Work plan The objective of the ongoing work is to make a quantitative comparison between the amount of water that could be melted by volcano-permafrost interaction and the outflow volume derived from channel and chaotic terrain morphology. The melted water is supposed to be initially stored as ice in a subsurface porous medium, so that the quested volume depends on the pore space and drainage area to be reached by a heat supplier. To find an approach to this problem, we want to reconstruct the outflow event by computing the discharge and sediment transport rate for Dao and Niger Valles under consideration of flow and transport processes in martian channels reviewed by [9]. The theoretical background of this work is used to derive model parameters. Channel width and water depth were obtained using individual MOLA tracks. Together with an assumed flow velocity based upon energy slope of the flow we calculate the discharge. Unlike previous calculations we will use the nondimensionalized Darcy- Weisbach equation for depth- and width-averaged flow velocity which has a depth-dependent roughness coefficient [9]. In order to investigate the history of the channel genesis we need a timescale, which can be derived from the discharge and volume of the removed material. Rather than utilizing individual MOLA profiles we base our estimates of channel dimensions on high-resolution DTM data obtained from HRSC stereo information. This process includes determination of overall volume by digitizing the channel area, creating TIN (triangulated irregular network) elements with individual height values (rather than assuming a flat cover) in order to obtain the surface before channel formation. The overall volume of removed material can be derived from height differences in combination with cellsize. Our first results show that a volume of 11400 km3 has been removed from the Dao source region. This can be compared to the volumes computed for some chaos regions as cited by [10]: Iani Chaos 32000 km3, Aram Chaos 28000 km3 and Margaritifer Chaos 23000 km3. These were determined from a combination of shadow and stereo measurements. The volume for Dao will be much better constrained. Further work, based on the conditions on the surface of Mars today, will include the significant but still open question of water phase changes and the timescale of these processes, compared to the derived timescale for the channel formation. References [1] Crown, D. A. et al. (1992) Icarus, 100, 1-25. [2] Leask, H. J. et al. (2006) JGR, 111, E08071. [3] Coleman, N. M. (2003), JGR, 108, E5-1-E5-15. [4] Andrews-Hanna, J. C. and Phillips, R. J. (2007) JGR, 112, E08001. [5] Crown, D. A. and Greeley, R. (1993) JGR, 98, 3431- 3451. [6] Bleamaster, L. F. III and Crown, D. A. (2005) GRL, 32, L20203. [7] Zuschneid, W. et al. (2005) EGU05-A-08664 / Zuschneid, W. (2005) diploma thesis FU Berlin. [8] Leonard, G. J. and Tanaka, K. L. (2001) Geol. Invest. Ser. I-2694. [9] Kleinhans, M. G. (2005
Gerhard Neukum
Musiol Stefanie
van Gasselt Stefan
No associations
LandOfFree
Channel geometry and discharge estimates for Dao and Niger Valles, Mars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Channel geometry and discharge estimates for Dao and Niger Valles, Mars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Channel geometry and discharge estimates for Dao and Niger Valles, Mars will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1793911