Baerbel K. Lucchitta

Mars and Earth: Comparison of cold-climate features

Abstract On Earth, glacial and periglacial features are common in areas of cold climate. On Mars, the temperature of the present-day surface is appropriate for permafrost, and the presence of water is suspected from data relating to the outgassing of the planet, from remote-sensing measurements over the polar caps and elsewhere on the Martian surface, and from recognition of fluvial morphological features such as channels. These observations and the possibility that ice could be in equilibrium with the atmosphere in the high latitudes north and south of ±40° latitude suggest that glacial and periglacial features should exist on the planet. Morphological studies based mainly on Viking pictures indicate many features that can be attributed to the action of ice. Among these features are extensive talus aprons; debris avalanches; flows that resemble glaciers or rock glaciers; ridges that look like moraines; various types of patterned ground, scalloped scarps, and chaotically collapsed terrain that could be attributed to thermokarst processes; and landforms that may reflect the interaction of volcanism and ice.

Valles Marineris, Mars: Wet debris flows and ground ice

Abstract Detailed study of the Valles Marineris equatorial troughs suggests that the landslides in that area contained water and probably were gigantic wet debris flows: one landslide complex generated a channel that has several bends and extends for 250 km. Further support for water or ice in debris masses includes rounded flow lobes and transport of some slide masses in the direction of the local topographic slope. Differences in speed and emplacement efficiency between Martian and terrestrial landslides can be attributed to the entrainment of volatiles on Mars, but they can also be explained by other mechanisms. Support that the wall rock contained water comes from the following observations: (1) the water within the landslide debris must have been derived from wall rock; (2) debris appears to have been transported through tributary canyons; (3) locally, channels emerged from the canyons; (4) the wall rock apprarently disintegrated and flowed easily; and (5) fault zones within the troughs are unusually resistant to erosion. The study further suggests that, in the equatorial region of Mars, material below depths of 400–800 m was not desiccated during the time of landslide activity (within the last billion years of Martian history). Therefore the Martian ground-water or groundice reservoir, if not a relic from ancient times, must have been replenished.

Young volcanic deposits in the Valles Marineris, Mars?

Abstract A study of the interior deposits of the central Valles Marineris has led to the discovery of a sequence of deposits that cover the chasma floors and range in thickness from that of thin dust to several kilometers. The emplacement of the deposits was the last major event in the history of the Valles Marineris, following deposition of older layered interior beds, warping, faulting, erosion, and landslide emplacement. The young deposits are of three major types: (1) dark patches typically occurring along faults; (2) light-colored deposits locally associated with craters; and (3) rugged, mottled deposits with, in places, light-colored lobate fronts. These young materials may be of volcanic origin, as suggested by the low albedo and spectrally gray colors of some, their association with faults and possible volcanic craters and calderas, and their embayment relations and lobate margins. No other mechanism explains all the observed features and relations as well as volcanism. If these deposits are volcanic, implications are that (1) volcanism was associated with rifting in the Valles Marineris, (2) the volcanism was explosive in places, and (3) the volcanism may be as young as the late Tharsis volcanism and, locally, may well be recent.

Crater clusters and light mantle at the Apollo 17 site - A result of secondary impact from Tycho

Abstract The morphologies of Tycho secondary craters and their ejecta deposits were studied using full-Moon, Lunar-Orbiter, and Apollo panoramic photographs. These data were compared with similar data for the secondary craters and light mantle of the Apollo 17 landing site. The results indicate that (1) the central crater cluster and the light mantle can be attributed to Tycho, (2) the dominant mechanism for emplacement of the light mantle was impact by secondary craters that threw material across the valley floor, and (3) level sheets of material may be emplaced locally by secondary impact. Analysis of returned samples confirms that secondary impacts rework mostly local material.

Antarctic ice streams and outflow channels on Mars

New sonar images of the Antarctic sea floor reveal mega-scale glacial lineations that are strikingly similar to longitudinal flutes in martian outflow channels. The analogs suggest that ice moved through the martian channels in places and carved the flutes. The ice in martian channels may have moved like Antarctic ice streams on deformable debris saturated with water under high pore pressure. On Mars, water at the base of ice-filled channels may have come from residual water or melt water liberated during past warmer climates or higher heat flows.

Lakes in Valles Marineris

The Valles Marineris is a large system of troughs extending just south of the Martian equator from about longitude 250° E to 320° E. They trend approximately N 75° W for a distance of about 4000 km, equivalent to nearly the entire width of the United States. The troughs opened about 3.5 Ga ago. Initial collapse along structural planes of weakness formed ancestral troughs, littered with chaotic hills, which filled rapidly with water from ground ice, subterranean aquifers, or nearby valley networks. Ancestral outflow channels spilled out of these troughs and flowed across the adjacent plateaus. Sediments may have filled the troughs gradually, as the basins sank, or were deposited into deep lakes after rapid basin collapse. The major lakes within the Valles Marineris dried up, except for a few late shallow lakes on the trough floors that were locally fed by tributary canyons or lingering valleys. Spur-and-gully erosion, which carved the early walls, apparently also stopped. It is nearly inevitable that lakes or playas with varying levels of surface or ground water existed at some time inside the Valles Marineris. It is difficult to envision the formation of or alteration to hydrated evaporite and iron oxide deposits without some aqueous activity. Ongoing investigations, especially with hyperspectral data, may eventually shed more light on the origin of the ILD and perhaps clarify the still ongoing debate over the extent to which the original ILD were of sedimentary, volcanic, or mixed provenance.

A Miocene river in northern Arizona and its implications for the Colorado River and Grand Canyon

The southwesterly course of the pre–late Miocene Crooked Ridge River can be traced continuously for 48 km and discontinuously for 91 km in northern Arizona. It is visible today in inverted relief. Pebbles in the river gravel came from at least as far northeast as the San Juan Mountains. The river valley was carved out of easily eroded Jurassic and Cretaceous rocks, whose debris overloaded the river with abundant detritus, possibly steepening the gradient. After the river became inactive, the regional drainage network was rearranged twice, and the Four Corners region was lowered by erosion 1–2 km. The river provides constraints on the history of the Colorado River and Grand Canyon; its continuation into lakes in Arizona or Utah is unlikely, as is integration of the Colorado River through Grand Canyon by lake spillover. The downstream course of the river was probably across the Kaibab Arch in a valley roughly coincident with the present eastern Grand Canyon.

Geomorphologic Evidence for Ground Ice on Mars

For ground ice to exist on Mars, two conditions have to be met. One is the presence of permafrost; the second is the availability of water. Because the mean temperature of Mars’surface is − 80 C., permafrost 1–3 km thick occurs over the entire planet. Remote-sensing measurements suggest that water presently exists in the atmosphere and in the polar caps; frost has been observed at the Viking landing sites. Landforms that support the contention that ground ice exists on Mars include lobate ejecta from craters, small valley networks, and numerous features that may be attributed to thermokarst. Chaotically collapsed terrain, chain craters, irregular depressions, and valleys tributary to canyons all appear to be related to loss of ground ice. Patterned ground has dimensions similar to that on Earth as well as dimensions of giant size. Masswasting features are common on scarps Even though individual features may be explained as results of other processes, the combined evidence indicates that a large reservoir of ground ice has existed on Mars.

Implications of the Miocene(?) Crooked Ridge River of northern Arizona for the evolution of the Colorado River and Grand Canyon

The southwesterly course of the probably pre–early Miocene and possibly Oligocene Crooked Ridge River can be traced continuously for 48 km and discontinuously for 91 km in northern Arizona (United States). The course is visible today in inverted relief. Pebbles in the river gravel came from at least as far northeast as the San Juan Mountains (Colorado). The river valley was carved out of easily eroded Jurassic and Cretaceous rocks whose debris overloaded the river with abundant detritus, probably steepening the gradient. After the river became inactive, the regional drainage network was rearranged three times, and the nearby Four Corners region was lowered 1–2 km by erosion. The river provides constraints on the early evolution of the Colorado River and Grand Canyon. Continuation of this river into lakes in Arizona or Utah is unlikely, as is integration through Grand Canyon by lake spillover. The downstream course of the river probably was across the Kaibab arch in a valley roughly coincident with the present eastern Grand Canyon. Beyond this point, the course may have continued to the drainage basin of the Sacramento River, or to the proto–Snake River drainage. Crooked Ridge River was beheaded by the developing San Juan River, which pirated its waters and probably was tributary to a proto–Colorado River, flowing roughly along its present course west of the Monument upwarp.

Relative age of Camelot crater and crater clusters near the Apollo 17 landing site

Topographic profiles and depth-diameter ratios from the crater Camelot and craters of the central cluster in the Apollo 17 landing area suggest that these craters are of the same age. Therefore, layers that can be recognized in the deep-drill core and that can be identified as ejecta deposits from Camelot or from the cluster craters should yield similar emplacement ages.