109 research outputs found
MARS 2020/PERSEVERANCE IN SITU GEOLOGIC CONTEXT MAPPING (GXM) INITIAL RESULTS ALONG THE TRAVERSE WITHIN JEZERO CRATER
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Birmingham News sleeve BN0028772
No full textMiss Alabama rehearsal / Suggested pictures / James Hatcher pointing out something to a couple of girls / Janice Walker fixing contestant's costume / Action shot of 24 finalists being presented / Town and Gown people and Ann Fowler in opening number / Anything you think of or think is better / Birmingham-Southern theater / Connie Durham - Fort Payne / Betsy Bryant - Bay Minette / Janice Walker / Nancy Williams - Andalusia / Anna Fay - Sylacauga / Kathy Wesson - Alexander City / Jeanie Edwards - Tuscaloosa / Freida Crumpler - Montgomery / Jim Holland / Suzanne Donnie - Mobile / Deedy Thompson - Birmingham / Larry McMillian / Jane McKinnon - Sylacauga / Cindy Winters / [Work order included
Chryse Planitia as a Mars Pathfinder landing site: The imperative of building on previous ground truth
No full textBased on consideration of the geological characteristics of Chryse Planitia, the requirements for Mars Pathfinder landing sites, the nature of the mission, the scale of the observations to be made, and the need to build outward from previous experience, a new mission to Chryse Planitia offers several advantages that are difficult to ignore as well as offering a low-gamble/high-return mission scenario. Considering the need to ensure a successful mission, and to ensure the continued health of planetary exploration, the reasons for a new mission to Chryse Planitia are compelling. Results of 1:500,000 mapping, operational benefits of Chryse Planitia, science benefits of Chryse Planitia, and conclusions and site recommendations are discussed
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IO: MODELS OF VOLCANISM AND INTERIOR STRUCTURE (JUPITER, MOON, CALDERAS, HEAT FLOW, LACCOLITHS).
No full textThe silicate "magma trigger" model of volcanism on Io has been evaluated numerically with finite element methods by considering the one-dimensional heat transfer between hot silicate magma and initially cold sulfur. It is found that for the probable range of initial magma temperatures and sulfur temperatures, the contact between silicate magma and a sulfur crust will be 700 (+OR-) 100 K, or approximately the vapor point of elemental sulfur. A silicate magma sill or laccolith on the order of 10 m thick will yield energetic vapor for a period of several weeks to several months depending on the vapor temperature and the amount of convective cooling of the silicate magma that occurs at the silicate-sulfur interface. This model may account for the origin of plumes and possible sulfur flows, as well as for their observed temperatures ((TURN) 600-700K) and lifetimes (several days to a few months). If the conducted heat flow is similar in high and low latitudes, then the low latitude occurrence of plumes may be explained as a result of lower temperatures at higher latitudes. Because the contact temperature of sulfur and silicate magma depends on the pre-existing sulfur temperature, a system in which sulfur vapor temperature is just reached at the equator would not generate sulfur vapor under lower initial sulfur temperatures existing at high latitudes. If the heat flow is higher in high latitudes, then the sulfur crust must be thinner than it is in low latitudes for the model to work as described above. Most of the heat flow from Io may be moved by convection from the interior to the surface, not by conduction. Heat flow may be modulated by the efficient transfer of silicate melts from 40 to 300 km depth, and emplaced as laccoliths at the sulfur-silicate crustal interfaces at a depth of 5-10 km. Sulfur flows, plumes, calderas and other areas of massive radiant heat dissipation continue the convective cycle to the surface. The temperature at the base of the sulfur crust may be less than the melting point of sulfur, and the silicate magma temperature can be as low as 1200 K. Low silicate magma temperatures will occur if the crust of Io is as differentiated as terrestrial rhyolites and trachytes. High alkalies in the Io plasma torus suggest the possibility that the Ionian crust is a highly differentiated silicate
Water alteration of rocks and soils on Mars at the Spirit rover site in Gusev crater
No full textGusev crater was selected as the landing site for the Spirit rover because of the possibility that it once held a lake. Thus one of the rover’s tasks was to search for evidence of lake sediments. However, the plains at the landing site were found to be covered by a regolith composed of olivine-rich basaltic rock and windblown ‘global’ dust. The analyses of three rock interiors exposed by the rock abrasion tool showed that they are similar to one another, consistent with having originated from a common lava flow.Here we report the investigation of soils, rock coatings and rock interiors by the Spirit rover from sol (martian day) 1 to sol 156, from its landing site to the base of the Columbia hills. The physical and chemical characteristics of the materials analysed provide evidence for limited but unequivocal interaction between water and the volcanic rocks of the Gusev plains. This evidence includes the softness of rock interiors that contain anomalously high concentrations of sulphur, chlorine and bromine relative to terrestrial basalts and martian meteorites; sulphur, chlorine and ferric iron enrichments in multilayer coatings on the light-toned rockMazatzal; high bromine concentration in filled vugs and veins within the plains basalts; positive correlations between magnesium, sulphur and other salt components in trench soils; and decoupling of sulphur, chlorine and bromine concentrations in trench soils compared to Gusev surface soils, indicating chemical mobility and separation.Additional co-authors: Paulo A de Souza, Jr, Douglas W Ming, Ralf Gellert, Jutta Zipfel, Johannes Brückner, James F Bell, III, Kenneth Herkenhoff, Phil R Christensen, Steve Ruff, Diana Blaney, Steven Gorevan, Nathalie A Cabrol, Larry Crumpler, John Grant, Lawrence Soderblo
Geologic map of the MTM 25047 and 20047 quadrangles, Central Chryse Planitia, Viking 1 lander site, Mars
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