The Memnonia quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Memnonia quadrangle is also referred to as MC-16 (Mars Chart-16).
Map of Memnonia quadrangle from Mars Orbiter Laser Altimeter (MOLA) data. The highest elevations are red and the lowest are blue.
The quadrangle is a region of Mars that covers latitude -30° to 0° and longitude 135° to 180°. The western part of Memnonia is a highly cratered highland region that exhibits a large range of crater degradation.
Memnonia includes these topographical regions of Mars:
Recently, evidence of water was found in the area. Layered sedimentary rocks were found in the wall and floor of Columbus Crater. These rocks could have been deposited by water or by wind. Hydrated minerals were found in some of the layers, so water may have been involved.
Many ancient river valleys Vallis including Mangala Vallis, have been found in the Memnonia quadrangle. Mangala appears to have begun with the formation of a graben, a set of faults that may have exposed an aquifer. Dark slope streaks and troughts (fossae) are present in this quadrangle. Part of the Medusae Fossae Formation is found in the Memnonia quadrangle.
Columbus Crater contains layers, also called strata. Many places on Mars show rocks arranged in layers. Sometimes the layers are of different colors. Light-toned rocks on Mars have been associated with hydrated minerals like sulfates. The Mars Rover Opportunity examined such layers close-up with several instruments. Some layers are probably made up of fine particles because they seem to break up into find dust. Other layers break up into large boulders so they are probably much harder. Basalt, a volcanic rock, is thought to in the layers that form boulders. Basalt has been identified on Mars in many places. Instruments on orbiting spacecraft have detected clay (also called phyllosilicate) in some layers. Recent research with an orbiting near-infrared spectrometer, which reveals the types of minerals present based on the wavelengths of light they absorb, found evidence of layers of both clay and sulfates in Columbus crater. This is exactly what would appear if a large lake had slowly evaporated. Moreover, because some layers contained gypsum, a sulfate which forms in relatively fresh water, life could have formed in the crater.
Scientists are excited about finding hydrated minerals such as sulfates and clays on Mars because they are usually formed in the presence of water. Places that contain clays and/or other hydrated minerals would be good places to look for evidence of life.
Rock can form layers in a variety of ways. Volcanoes, wind, or water can produce layers.
Layers in crater wall, as seen by HiRISE under HiWish program
Layers exposed at the base of a group of buttes in Mangala Valles in Memnonia quadrangle, as seen by HiRISE under HiWish program. Arrows point to boulders sitting in pits. The pits may have formed by winds, heat from the boulders melting ground ice, or some other process.
Mangala Vallis is a major channel system that contains several basins which filled, then the overflow went through a series of spillways. One source of waters for the system was Memonia Fossae, but water also probably came from a large basin centered at 40 degrees S.
Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak. The peak is caused by a rebound of the crater floor following the impact. Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed unto the surface. Hence, craters can show us what lies deep under the surface. At times, bright rays surround craters because the impact has gone down to a bright layer of rocks, then thrown out the bright rocks on the darker surface. An image below from Mars Global Surveyor shows this.
Close-up of Columbus (Martian crater), as seen by HiRISE.
Nicholson Crater Central Mound, as seen by HiRISE. Click on image to see dark slope streak being diverted by an obstacle.
Bernard Crater Floor, as seen by HiRISE. Large cracks are visible on floor.
Troughs on the floor of Bernard Crater showing many boulders, as seen by HiRISE under HiWish program
Troughs on the floor of Bernard Crater, as seen by HiRISE under HiWish program
Dejnev Crater Floor, as seen by HiRISE. Scale bar is 500 meters long. Click on image to see large pits.
Middle section of Burton Crater, showing central mound, as seen by CTX camera (on Mars Reconnaissance Orbiter).
Central mound of Burton Crater, showing dark slope streaks, as seen by CTX camera (on[Mars Reconnaissance Orbiter). Note: this is an enlargement of the previous image of Burton Crater.
East side of Ejriksson Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).
Ridges on Mars may be due to different causes. Long straight ridges are thought to be dikes. Curved and branched ridges may be examples of inverted topography, and groups of straight ridges that cross each other may be the result of impacts. These intersecting box-like ridges are called linear ridge networks. Linear ridge networks are found in various places on Mars in and around craters. Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind.
Yardangs are common in some regions on Mars, especially in what's called the "Medusae Fossae Formation." They are formed by the action of wind on sand sized particles; hence they often point in the direction that the winds were blowing when they were formed.
Wide view of yardangs in Lucus Planum, as seen by HiRISE under HiWish program
Dark slope streaksEdit
Many places on Mars show dark slope streaks on steep slopes like crater walls. It seems that the youngest streaks are dark; they become lighter with age. Often they begin as a small narrow spot then widen and extend downhill for hundreds of meters. Several ideas have been advanced to explain the streaks. Some involve water. or even the growth of organisms. The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust. Fine dust settles out of the atmosphere covering everything. We know a lot about this dust because the solar panels of Mars Rovers get covered with dust. The power of the Rovers has been saved many times by the wind, in the form of dust devils, that have cleared the panels and boosted the power. From these observations with the Rovers, we know that the process of dust coming out of the atmosphere then returning happens over and over.
It is most generally accepted that the streaks represent avalanches of dust. The streaks appear in areas covered with dust. When a thin layer of dust is removed, the underlying surface is dark. Much of the Martian surface is covered with dust. Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the sun. The orbit of Mars is much more elliptical then the Earth's. That is the difference between the farthest point from the sun and the closest point to the sun is very great for Mars, but only slight for the Earth. Also, every few years, the entire planet is engulfed in a global dust storm. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm. Other global dust storms have also been observed, since that time. Dark streaks can be seen in the image below taken with HiRISE of the central mound in Nicholson Crater. At least one streak in the image splits into two when encountering an obstacle.
Research, published in January 2012 in Icarus, found that dark streaks were initiated by airblasts from meteorites traveling at supersonic speeds. The team of scientists was led by Kaylan Burleigh, an undergraduate at the University of Arizona. After counting some 65,000 dark streaks around the impact site of a group of 5 new craters, patterns emerged. The number of streaks was greatest closer to the impact site. So, the impact somehow probably caused the streaks. Also, the distribution of the streaks formed a pattern with two wings extending from the impact site. The curved wings resembled scimitars, curved knives. This pattern suggests that an interaction of airblasts from the group of meteorites shook dust loose enough to start dust avalanches that formed the many dark streaks. At first it was thought that the shaking of the ground from the impact caused the dust avalanches, but if that was the case the dark streaks would have been arranged symmetrically around the impacts, rather than being concentrated into curved shapes.
Fossa on MarsEdit
Large troughs (long narrow depressions) are called fossae in the geographical language used for Mars. This term is derived from Latin; therefore fossa is singular and fossae is plural. Troughs form when the crust is stretched until it breaks. The stretching can be due to the large weight of a nearby volcano. A trough often has two breaks with a middle section moving down, leaving steep cliffs along the sides; such a trough is called a graben. Lake George, in northern New York State, is a lake that sits in a graben.
Other ideas have been suggested for the formation of fossae. There is evidence that they are associated with dikes of magma. Magma might move along, under the surface, breaking the rock and more importantly melting ice. The resulting action would cause a crack to form at the surface. Dikes caused both by tectonic stretching (extension) and by dikes are found in Iceland. An example of a graben caused by a dike is shown below in the image Memnonia Fossae, as seen by HiRISE.
Large pits in Sirenum Fossae, as seen by HiRISE under HiWish program
There is enormous evidence that water once flowed in river valleys on Mars. Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter.Vallis (plural valles) is the Latin word for valley. It is used in planetary geology for the naming of landform features on other planets, including what could be old river valleys that were discovered on Mars, when probes were first sent to Mars. The Viking Orbiters caused a revolution in our ideas about water on Mars; huge river valleys were found in many areas. Space craft cameras showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers. Some valles on Mars (Mangala Vallis, Athabasca Vallis, Granicus Vallis, and Tinjar Valles) clearly begin at graben. On the other hand, some of the large outflow channels begin in rubble-filled low areas called chaos or chaotic terrain. It has been suggested that massive amounts of water were trapped under pressure beneath a thick cryosphere (layer of frozen ground), then the water was suddenly released, perhaps when the cryosphere was broken by a fault.
Asopus Vallis, as seen by HiRISE.
Samara Valles, as seen by HiRISE. Scale bar is 500 meters long.
Minio Vallis, as seen by HiRISE under HiWish program Many dark slope streaks are present.
Sabis Vallis, as seen by THEMIS. The small channels are joining to form Sabis Vallis.
Channel with dark slope streaks as seen by HiRISE under HiWish program
Lava is common on Mars, as it is on many other planetary bodies.
Fifty Years of Mars Imaging: from Mariner 4 to HiRISEEdit
On October 3, 2017, HiRISE acquired a picture of Mars in the Memnonia quadrangle of a spot that has been imaged by 7 different cameras on different spacecraft over the past 50 years. The pictures from the Red Planet started with one of the pictures from Mariner 4 in the summer of 1965. The following pictures show these pictures with their increasing resolution over the years. The resolution in the first image by Mariner 4 was 1.25 Km/pixel; that compares to the approximate 50 cm/pixel resolution of HiRISE.
Composite demonstrating relative resolution of 7 different cameras that imaged Mars: HiRISE (Mars Reconnaissance Orbiter), THEMIS VIS (Mars Odyssey), MOC-WAC (Mars Global Surveyor), HRSC (Mars Express), CTX (Mars Reconnaissance Orbiter), Viking, Mariner 4. Location is Memnonia quadrangle. Blue arrow on some pictures points to same location at with different cameras. Red box with CTX image shows location of the next frame from HiRISE.
More features of Memnonia quadrangleEdit
Other Mars quadranglesEdit
Interactive Mars mapEdit
- Climate of Mars
- Dark slope streaks
- Fossa (geology)
- Geology of Mars
- Groundwater on Mars
- High Resolution Stereo Camera - HRSC
- HiWish program
- Impact crater
- Lakes on Mars
- List of quadrangles on Mars
- Linear ridge networks
- Lucus Planum
- Mariner 4
- Mars Express
- Mars Global Surveyor
- Mars Orbiter Camera
- Mars Orbiter Mission
- 2001 Mars Odyssey
- Thermal Emission Imaging System- THEMIS
- Viking program
- Valley networks (Mars)
- Water on Mars
- Yardangs on Mars
- Davies, M.E.; Batson, R.M.; Wu, S.S.C. "Geodesy and Cartography" in Kieffer, H.H.; Jakosky, B.M.; Snyder, C.W.; Matthews, M.S., Eds. Mars. University of Arizona Press: Tucson, 1992.
- USGS Astrogeology: Planetary Map Listing
- "HiRISE | Sedimentary Layers in Columbus Crater (PSP_010281_1510)". Hirise.lpl.arizona.edu. Retrieved 2012-08-04.
- "Mars Channels and Valleys". Msss.com. Retrieved 2012-08-04.
- Cabrol, N. and E. Grin (eds.). 2010. Lakes on Mars. Elsevier.NY.
- Wray, J. et al. 2009. Columbus Crater and other possible plaelakes in Terra Sirenum, Mars. Lunar and Planetary Science Conference. 40: 1896.
- "Martian "Lake Michigan" Filled Crater, Minerals Hint". News.nationalgeographic.com. 2010-10-28. Retrieved 2012-08-04.
- "Target Zone: Nilosyrtis? | Mars Odyssey Mission THEMIS". Themis.asu.edu. Retrieved 2012-08-04.
- "HiRISE | Craters and Valleys in the Elysium Fossae (PSP_004046_2080)". Hirise.lpl.arizona.edu. Retrieved 2012-08-04.
- "HiRISE | High Resolution Imaging Science Experiment". Hirise.lpl.arizona.edu?psp_008437_1750. Retrieved 2012-08-04.
- Cabrol, N. and E. Grin (eds.). 2010. Lakes on Mars. Elsevier. NY.
- Emrick, C. and R. De Hon. 1999. Flood discharge through Labou Vallis, Mars. Lunar Planet. Sci. Conf. XXX: Abstract #1893.
- Zimbelman, J. et al. 1992. Volatile history of Mangala Valles, Mars. J. Geophys. Res. 97: 18309-18317
- De Hon, R. 1994. Lacustrine sedimentation in lower Mangals Valles. Mars Lunar Planet. Sci. Conf. XXVII: 295-296
- "Stones, Wind, and Ice: A Guide to Martian Impact Craters". Lpi.usra.edu. Retrieved 2012-08-04.
- Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved 7 March 2011.
- Head, J., J. Mustard. 2006. Breccia dikes and crater-related faults in impact craters on Mars: Erosion and exposure on the floor of a crater 75 km in diameter at the dichotomy boundary, Meteorit. Planet Science: 41, 1675-1690.
- SAO/NASA ADS Astronomy Abstract Service: Yardangs on Mars
- Schorghofer, N, et al. 2007. Three decades of slope streak activity on Mars. Icarus. 191:132-140.
- [dead link]
-  Archived February 21, 2015, at the Wayback Machine
- [dead link]
- "Mars Spirit Rover Gets Energy Boost From Cleaner Solar Panels". Sciencedaily.com. 2009-02-19. Retrieved 2012-08-04.
- Ferris, J. C.; Dohm, J.M.; Baker, V.R.; Maddock III, T. (2002). Dark Slope Streaks on Mars: Are Aqueous Processes Involved? Geophys. Res. Lett., 29(10), 1490, doi:10.1029/2002GL014936
- ISBN 0-517-00192-6
- Kaylan J. Burleigh, Henry J. Melosh, Livio L. Tornabene, Boris Ivanov, Alfred S. McEwen, Ingrid J. Daubar. Impact air blast triggers dust avalanches on Mars. Icarus, 2012; 217 (1): 194 doi:10.1016/j.icarus.2011.10.026
- "Red Planet Report | What's up with Mars". Redplanet.asu.edu. Retrieved 2012-08-04.
- "Mars Art Gallery Martian Feature Name Nomenclature". Marsartgallery.com. Retrieved 2012-08-04.
- "HiRISE | Craters and Pit Crater Chains in Chryse Planitia (PSP_008641_2105)". Hirise.lpl.arizona.edu. Retrieved 2012-08-04.
- "HiRISE | Graben in Memnonia Fossae (PSP_005376_1575)". Hirise.lpl.arizona.edu. Retrieved 2012-08-04.
- Michael H. Carr (2006). The surface of Mars. Cambridge University Press. ISBN 978-0-521-87201-0. Retrieved 21 March 2011.
- Baker, V. 1982. The Channels of Mars. Univ. of Tex. Press, Austin, TX
- Baker, V., R. Strom, R., V. Gulick, J. Kargel, G. Komatsu, V. Kale. 1991. Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature 352, 589–594.
- Carr, M. 1979. Formation of Martian flood features by release of water from confined aquifers. J. Geophys. Res. 84, 2995–300.
- Komar, P. 1979. Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth. Icarus 37, 156–181.
- Raeburn, P. 1998. Uncovering the Secrets of the Red Planet Mars. National Geographic Society. Washington D.C.
- Moore, P. et al. 1990. The Atlas of the Solar System. Mitchell Beazley Publishers NY, NY.
- Carr, M. 1979. Formation of martian flood features by release of water from confined aquifers. J. Geophys. Res. 84: 2995-3007.
- Hanna, J. and R. Phillips. 2005. Tectonic pressurization of aquifers in the formation of Mangala and Athabasca Valles on Mars. LPSC XXXVI. Abstract 2261.
- Morton, Oliver (2002). Mapping Mars: Science, Imagination, and the Birth of a World. New York: Picador USA. p. 98. ISBN 0-312-24551-3.
- "Online Atlas of Mars". Ralphaeschliman.com. Retrieved December 16, 2012.
- "PIA03467: The MGS MOC Wide Angle Map of Mars". Photojournal. NASA / Jet Propulsion Laboratory. February 16, 2002. Retrieved December 16, 2012.