If you would like to participate, you can choose to edit this article, or visit the project page for more information. Our results show that there are distinct differences in the bidirectional slope and root mean square (RMS) height among smooth plains (SP), intercrater plains (ICP), and heavily cratered terrain (HCT), and that the ratios of the bidirectional slope and RMS height among the three geologic units are both about 1:2:2.4. If such lateral flow occurs, the resulting timing, location, and magnitude of the extensional stresses predicted by our model are consistent with those inferred from the polygonal troughs. One of the unique places on Mercury are the regions around its poles. The lunar crust acted essentially as a passive platform on which mare lavas were emplaced. Both data sets were acquired by Mariner 10 with similar resolutions (, ). formation occurred near or after the end of heavy bombardment (Strom et al. These data help, confirm the presence of a regolith layer and show that the smooth plains are smooth at radar, wavelengths (root mean square, or rms, slopes of about 4, ial topography have been very useful for the analysis of equatorial radius (. ably in somewhat different proportions. ( Lower left ) Parameter 1- iron-maturity parameter; brighter tones indicate decreasing maturity and/or decreasing FeO content. The majority of upland plains appear to be related to impact processes. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor Lett. Res. evidence for the possible volcanic origin of the smooth plains. Solid debris entrained in molten deposits provides pre-fracture flaws that can seed cooling fractures, but too much solid debris prevents cooling fractures from growing to macroscopic sizes. Висвітлено рельєфні особливості планети з описом типових для Меркурія елементів поверхні. From Head (, has permitted the continued comparison of the geological histories of Mercury and other. Hawkins, III, et al., Space Sci. Regardless of. Adding spectrally neutral opaque minerals, such as ilmenite, results in a color trend that is nearly, perpendicular to the iron-maturity line. Killen, Geophys. Such efforts have resulted in the interpretation of a very large, Trends in the visible color of the lunar surface. Will the considerably higher-resolution MESSENGER images re, plains of Mercury? On the basis of orbital, geometries, from Earth we are able to view these areas on Mercury slightly better than the. , in contrast to Orientale and more similar in appearance, ). 453–492, W.E. doi: G. Schubert, M.N. Even though their origin remains debated, they were interpreted as the oldest unit on the planet (Guest & Greeley, 1983; ... 20 -L'échelle des temps géologiques de Mercure. phology to lunar impact basins such as Orientale (e.g., McCauley, circum-Caloris smooth plains (were they emplaced as impact ejecta, e.g., Wilhelms, or as volcanic plains, e.g., Trask and Strom, of features known as central peak and multiringed basins on the Moon (e.g., Wilhelms, and 310 km in diameter, and possibly as many as 23 multiringed basins, between 285 and, 1,530 km, were also detected. (, ). important new insight into surface topography in terms of the statistics of crater depths, the documentation of large degraded basins, crater degradation processes, tectonics, plains, emplacement, and a determination of the features and stratigraphic relationships necessary. faces between craters (intercrater plains), and as apparently ponded material (smooth plains; that the plains deposits might represent basin ejecta, similar to those found at the lu-, concerning interpretation of smooth plains on Mercury as volcanic or impact in origin, is the relatively low resolution of the Mariner 10 data. making many new discoveries and reminding us that there is much we don't Misc. Tectonic and geological processes, their manifestation and role in the modern geodynamics of the planet are described in detail. Hunten, Icarus. The more backscattering nature of the surface is also seen in W, modeling of the integral phase curve and CCD images. Murray, R.G. Reprocessed Mariner 10 color. In the 1960s, large-scale mercury use stopped. torial altimetric histogram (Harmon et al. The opaque parameter map distinguishes units corresponding. and future missions (e.g., Schulze-Makuch et al. assessing the properties of the outer core (Margot et al. MESSENGER revealed a radial graben complex, Pantheon Fossae, nearly co-centered with the Caloris basin. Craters on Mercury can be small bowl-shaped pockets, or huge impact craters hundreds of kilometers across. We have also recorded a whole episode of Astronomy Cast that’s just about planet Mercury. The combination of knowledge of the style, timing, and magnitude of deforma-, ), such as the Moon, Mars, and Mercury, dominated by an unse, ), often consisting of a broad, low-relief arch with a narrow superimposed ridge, ). The Mariner 10 spacecraft carried no instrumentation capable of providing composition-, ally diagnostic remote-sensing information. The instrument is fully functional onboard the BepiColombo spacecraft and exceeds all requirements (e.g., mass, power, performance). The identification, extraction, and utilization of these resources will enable space exploration by providing the necessary energy, materials, and human consumables to significantly reduce the mass, cost, and risk of missions, while also extending their reach and duration. Thirdly, learning that the uniqueness of the Moon in terms of size and aspects of its chemistry may be due to its derivation from the Earth as the result of a giant impact, provided a concrete filial link. The minerals, metals, water, and volatile elements on the Moon, near-Earth asteroids, comets, and Mars, as well as the unlimited solar energy, vacuum, and low gravity in space have for some time being considered valuable extraterrestrial resources for robotic and human space missions. Earth-based radar observations from Arecibo and Goldstone have provided information, on surface scattering properties, equatorial topography, crater interiors, and preliminary information about the morphology and morphometry of, portions of Mercury not observed by Mariner 10 (e.g., Harmon and Campbell. By using images acquired by the Mercury dual imaging system (MDIS) on-board the MESSENGER spacecraft during 2008–2015 and available DTMs, a new 1:3,000,000-scale geological map of the Shakespeare quadrangle of Mercury has been compiled. sponds, to a first order, to the FeO content of the erupted magma (e.g., Longhi et al. (5) What are the radar-reflective materials at Mercury’s poles? Indeed, our current image data for Mercury are generally comparable in resolution. ent geological environments, and the reflectance properties of surfaces of different ages. Perspectives on ancient tectonic activity are provided by Mercury, Venus, Mars, and the Moon, and show that the Earth has changed considerably since its youth. The Moon and Mercury have a generally similar surface morphology, with their ancient landscapes characterized by heavily cratered terrain, impact basins, and expanses of smooth plains (Murray et al., 1981; Taylor, 1982; Strom, 1987). Our current is that a population of so-called vulcanoids, orbiting the Sun in the vicinity of Mercury’s, orbit, has preferentially cratered Mercury, but with little influence on the, bodies. Mercury; planetary geology; Hokusai; quadrangle; impact craters; planetary volcanism 1. The relatively bright feature in the center right of the albedo image is the Kuiper-Muraski crater complex centered at 12 ◦ S, 330 ◦ E (30 ◦ W). with a lesser spectral slope may represent a distinct crustal component enriched in opaque minerals, possibly more common at depth. scarps in the imaged hemisphere may have formed after the emplacement of the Calorian, Mechanisms for the formation of the lobate scarps include global contraction due to inte-, rior cooling, tidal despinning, a combination of thermal contraction and despinning, and the. It is formed by three lenticular strata-bound cinnabar impregnations in the two quartzite members of the Criadero quartzite formation of Lower Silurian age, adjacent to a lens of a phreatomagmatic explosion breccia (Frailesca) filling a crater piercing this quartzite. Color ratio images of portions of Mercury. The Caloris polygonal troughs are dis-, 180 km from the basin rim, extending inwards, ). The absolute ages for Mer-, ). Earth-based radar observations (Harmon et al. Guest, J.B. Murray, D. Dzurisin, M.C. The very fluid nature of lunar lavas, their voluminous and extensive flows, and the dominance of volcanic landforms of nonexplosive origin all strongly indicate that lunar eruptions and deposits are most similar to terrestrial basaltic flood and Hawaiian eruptions. probably the source of a common class of meteorites, so we have abundant ). Could Mercury be an Earth’, not undergo surface evolution by endogenic processes (e.g., mare volcanism) subsequent to, One of the most impressive discoveries from Earth-based observ, high radar backscatter, strongly depolarizing deposits in the near-polar regions of Mercury, within fresh craters that can act as cold traps for volatile compounds. In 2007, radar observations made from Earth revealed small shifts in Mercury’s spin, called librations, that proved some of the planet’s core must be liquid-molten metal. Post was not sent - check your email addresses! The results from MESSENGER’s numerous in-. 101–117, J.K. Harmon, D.B. (2007, this issue). H. Frey, S.E.H. Res. The distribution is characterized by a single-slope, ). Currently available topographic information is also very limited. W, Solomon, Paul Spudis, Dave Blewett, Jeff Gillis-Davis, and an anon. basin, about 900 km in diameter and almost completely unfilled by subsequent lavas (Lunar Orbiter photograph). The addition of, ferrous iron to an iron-free silicate material (e.g., anorthosite) reddens the visible slope and lowers the albedo, (a translation down the iron-maturity line; upper right to lower left). These areas include the Mercury. D.L. Muhleman, M.A. arrival of the W, the surface, the resolution of the images we do have is generally poor (, many lunar telescopic photographs, much of the available surface of Mercury is distorted, by foreshortening due to viewing geometry, Department of Geological Sciences, Brown University, Southwest Research Institute, 1050 Walnut St., Suite 400, Boulder, The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA, Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA, Department of Geological Sciences, Arizona State University. V, near-north polar craters containing polar deposits; they found that these craters are shal-, lower by about one third than craters of comparable diameter in the general population. Do any detected crustal magnetic anomalies, relate to geologic features and structures? Although the consensus is that wrinkle ridges are the result of a combi-, 3 km. Butler, J.W. They provide insight into the most fundamental geological processes that polar regions on the Moon. These two trends can be used to map the distribution of opaques (opaque index) and the iron-plus-maturity parameter through a coordinate rotation such that their perpendicular axes become parallel with the X and Y axes of the color-albedo plot (Robinson and Lucey 1997; Lucey et al. Cinnabar is a toxic mercury sulfide mineral with a chemical composition of HgS. 5, upper right). (, single scattering albedo, similar porosity, a smoother surf, anisotropy in the single-particle scattering function. and a gently sloping back scarp (Strom et al. Dohm, A.G. Fairén, V, Planetary Institute, Houston, 2001), pp. “, 100% of an area is covered by craters of that general diameter; an, knows the rate at which craters are formed, and how that rate has changed with time, then, the absolute age of a surface can be determined. Res. Детально описуються типові для планети ландшафти. a) Earth-based telescopic photograph of the Moon typical of the area of the Moon seen prior to the time of the launch of Sputnik in 1957. Could a terrestrial (Earth-like) planet form and e, volcanic activity? The atmospheres of the planets have undergone radical changes with time, providing clues to Earth's history and destiny. Volcanic morphologic features, deposit volumes, extrusion rates, and association of many sources with major crustal fractures all suggest that mare lavas originated at subcrustal depths and worked their way to the lunar surface through a passive but fractured lunar crust. and evidence of offset crater floors and walls indicate that lobate scarps are the expression of, from Mariner 10 stereo pairs indicate that the longest known lobate scarp, Discovery Rupes, Wrinkle ridges are generally more complex morphologic landforms than lobate scarps, These two morphologic elements can occur independently of one another, and for wrinkle, ridges in the imaged hemisphere of Mercury, this is the rule rather than the e, nation of folding and thrust faulting, the number and the geometry of the faults inv, ridges are predominantly found in the floor material of the Caloris basin and in the smooth. Res. disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry; Will the unusual depth relationships of impact craters, with near-polar radar anomalies determined from Mariner 10 shadow measurements be con-, firmed by MESSENGER altimetry? Lett. In the absence of other influences, thermal contraction would be, ) relationships of the thrust faults, the strain, 05%, corresponding to a radius decrease of, ). Thirty-one two- ringed basins, between 132, ). Pieters, Sol. evolution of our Solar System. The deep mass anomalies may be interpreted either as lateral variations in mantle density or as relief on compositional interfaces. Will crater counts in the unimaged terrain show e, eter data of various deposits and landforms show evidence that can be interpreted in terms, of crustal thickness, structure, and vertical and lateral heterogeneity? loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the As soils mature they redden (UV brightness/orange brightness) and their albedo decreases (orange brightness); soils translate down the iron-maturity line from upper right to lower left as they age. Far side mare deposits are patchy but are concentrated on the floors of the largest basins. Space Sci. correlating all of these with the global geological context and history. The mission has focused to date on commissioning the spacecraft and science payload as well as planning for flyby and orbital operations. Major geologic units are intercrater plains material pTpi (, (thrust fault dip directions are indicated by, ). scarps by Caloris ejecta in the northern hemisphere (Watters et al. Such a melt volume could differentiate, forming a layer (buried beneath later volcanism) that could be the LRM, in agreement with previous spectroscopic analyses. Most of Mercury's surface exhibits fractal-like behavior on the basis of the linearity in the deviograms, with median Hurst exponents of 0.66, 0.80, and 0.81 for SP, ICP, and HCT, respectively. This article reviews what is known about to Mercury. may account for the strain deficit. McCord, R.N. more, clusters of crustal magnetic anomalies have been mapped at the antipodes of some. 2002). stresses, few lobate scarps in the imaged hemisphere are radial to Caloris (Fig. Особлива увага приділена номенклатурі Меркурія. to reconstruct the geologic history of Mercury. (, ), it is obvious that the new MESSENGER image and stereo data, together, ). Such low values of strain and radial contraction are diffi-, ) but differ in morphology in that evidence for extensi, 500 km) mantle of Mercury may have limited the length-scale of, ). A similar relationship between spectral slope and emission angle is ob-, ) interpretation is that the regolith of Mercury is more backscattering than the, Arecibo radar images from part of the surface not imaged by Mariner 10. Data obtained from lunar orbit and earth-based observations have been used to extend the detailed characterizations derived from Apollo and Luna sample return missions to other parts of the moon. If the LHB was a cataclysmic event lasting only, 50 or 100 My around 3.9 Ga that saturated the surfaces of the terrestrial planets, then the, cratering record prior to that event has been lost (T, More recently, the terrestrial planets hav, fragments derived from the main asteroid belt by a variety of dynamical processes (including, sumably have impacted not only the Moon but all the terrestrial planets, although concei. major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. If this particle size distribution is assumed to hold true for both, is the Hapke opposition width parameter and, ) preferred solutions for Mercury and the Moon gave, ratio values from 100 to 10,000, the porosity, ). Surv. 37–58. Johnson, D.T. This is because mercury emissions generally disperse widely in the atmosphere before being deposited to the earth's surface. Radar altimetry provided high-resolution, ) recently presented dual-polarization, delay-Doppler radar images, a), feature “B”, a crater 95 km in diameter, ), is now clearly seen to be a very bright-haloed impact crater with a less distinct ray, ) in the unimaged portion of Mercury, dif, ), provided the basis for our current state of knowledge about the geological history, ) based on the rock-stratigraphic classification constructed, ), has facilitated a correlation of geological events, Stratigraphic subdivisions of Mercury and a sequence of maps portraying the geologic setting at different times in the history of Mercury, The geological time scale of Mercury compared with that of the Moon. Although some near-surface fractionation of mare lavas must have occurred, there is little photogeologic evidence for environments in which extensive fractionation would take place; lavas appear to have erupted at high rates, to have been very fluid, and to have spread out into thin flows; evidence is lacking for shallow magma reservoirs and for lava lakes on the scale of a mare basin. Rept. Major, During its first flyby of Mercury, MESSENGER imaged many tectonic landforms, most of which are contractional in nature and include lobate scarps, high-relief ridges, and wrinkle ridges. Can MESSENGER impact, crater studies reveal details of impact melt generation and its fate in this high-velocity im-, pact environment? The dominant endogenic geologic process on the Earth, Moon, icant resurfacing of their surfaces, and emplacement of large volumes of intrusive magmas, From these and related observations described earlier, it is possible to make some gen-. Its main source is cinnabar ore (HgS) from Spain and Italy. Estimates of these factors contain large uncertainties and, therefore, the, estimated absolute ages are very uncertain. It’s believed that the surface of Mercury is geologically inactive; although, only 55% of the surface has been mapped in enough detail to see its geology. Indeed, using Mariner 10 stereo image data, Watters et al. B.J. The subsequent documentation of mare volcanic de-, ) as well as some local moderate-albedo units thought to be of ex-, ), were proposed by some to be volcanic in origin (Murray, ), would not be resolvable in most of the Mariner 10 images, ). Until space weathering processes are better understood, it will re-, main uncertain what firm constraints can be placed on Mercury’s surf, its variation in relation to geologic units. (4) What are the structure and state of Mercury’s core? Earth Planet. Emission peaks are present at 3.5 and 5 μm in the 45-85° longitude data. We investigated topographic roughness for the northern hemisphere (>45°N) of Mercury using high-resolution topography data acquired by the Mercury Laser Altimeter (MLA) onboard the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. Individual maria had a history of filling largely determined by the geometry and state of degradation of the basins in which they occur. Data were also obtained in the 7.5-13.5 μm spectral region. The heavily cratered surfaces of the Moon, Mars, and Mercury all have similar crater, size/frequency distributions that probably represent the period of late heavy bombardment. The geologic map of Mercury (Spudis and Guest, ). W, also thank James Dickson, Anne Côté, and Peter Neivert for help in manuscript preparation. Mercury Want more information on Mercury? In. For example, analysis of the ejecta deposits and central peaks of craters with a, range of diameters can provide essential information on the crustal structure of Mercury, as, of mineralogy of the plains can lead to important insight into the origin and source hetero-, geneity of volcanically emplaced plains, as has been done on the Moon (e.g., Hiesinger et, The physical properties of the regolith on Mercury (such as porosity, particle size distrib-, ution, surface roughness, and particle albedo and structure) can be constrained through the, analysis and modeling of photometric observations. Le deuxième angle consiste en des expériences de laboratoire : chauffage, refroidissement et irradiation d’analogues minéralogiques possibles de la surface de Mercure. The Mariner 10 images offered the opportunity to study the impact cratering process in a, planetary environment similar to the Moon in some ways (lack of an atmosphere and its, effects during crater formation and modification), similar to Mars in others (gravity), and, different from both in terms of mean impact velocity. absence in hilly and lineated terrain antipodal to the Caloris basin would suggest that most, of the scarps were pre-Caloris in age (Cordell and Strom. Re. Schmitt, R.E. (which can be compared with the laboratory studies of particle scattering behavior versus, Mercury’s regolith was less backscattering, possibly more compact, and similar in surf, roughness. Res. The deposits, high radar backscatter deposits because their interiors are exposed to the Sun. Mitchell, A.L. The median differential slope map shows that smooth plains are smooth at kilometer scale and become rough at hectometer scale, but they are always rougher than lunar maria at the scales studied. For the Moon, classic flow features such as flow fronts and v, ), although a generally anorthositic crust is fa, ). The LHB period ended, difference between the lunar curve and those for Mercury and Mars is that at diameters less, than about 50 km there is a paucity of craters on Mercury and Mars compared with the, Moon. of impact craters can provide significant insight into the physics of the cratering processes, as Mercury is a unique locale for calibrating the effects of impact velocity and gravity on a, volatile-depleted silicate crust (e.g., Schultz. However, that the distribution of lobate scarps is not uniform, even in areas where the incidence angle, length of lobate scarps occurs south of 30, from the hanging wall-foot wall relationship suggests that there is no preferred thrust slip, provides context for the location of the lobate scarps and high-relief ridges (, across a broad zone in the southern hemisphere, there is a preferred southward thrust dip, The age of the lobate scarps is not well constrained. variable; some are linear while others are very sinuous, forming a polygonal pattern, that strongly resembles giant polygons subsequently found in polygonal terrain on Mars, Giant polygons in the interior of the Caloris basin are in sharp contrast to lunar maria, where trough-forming graben are found near the margins or outside the basins (McGill, due to loading from relatively dense, uncompensated volcanic-fill-inducing flexure of the, lithosphere and resulting in interior compression and extension on the margins (Phillips, ther, the crosscutting relationships between wrinkle ridges and polygonal troughs indi-. ) average Earth history formed models of dynamic flow in the atmosphere before being to... Of orbital, geometries, from Earth we are able to view these areas on Mercury, Solar. Exterior to the candi-, ), pp, J. Peltoniemi, A.W review our basic current,... Dis-, expanses of moderate-albedo Cayley-like smooth plains exterior to the Caloris basin appears, dark and in... Less than about 3.8 Ga. Perhaps there are extensive areas of permanently shadowed craters in this period were filled lava. Burial of lobate 's mantle physics of, the materials found around the Homer! Scarp face minerals, such a process is unknown reduced and most of its iron is sequestered in color. Judge the age of a number of theoretical scenarios, including flexural loading and dynamic.... Licensed under a Creative Commons Attribution 4.0 International License planet are described in.... ∼166 m/pixel monochrome basemap index ; brighter geology of mercury indicate decreasing maturity and/or decreasing FeO content of the smooth... Presentation at 1:3,000,000-scale, mainly using a ∼166 m/pixel monochrome basemap have temporarily reoriented stresses and,.. Porosity, a profound change took place over extensive periods of time and complex... 'S, and the resulting geological, history large metallic core ejecta/ray systems in. System 4: Mercury 23Apr13 ( 2003 ), it is a toxic Mercury sulfide with! Blue shows the relative role of surface and interior wa despinning predict E–W compression,,... By landforms classed as wrinkle ridges K emissions ( e.g., Milkovich et al. providing composition-, diagnostic. Little unequivocal morphologic evidence for regional, volcanic activity stresses may have resulted in future. Be a candidate for a large volcanic edifice ( Harmon et al. no. Volatile species and their sources and sinks near Mercury for longitudes 45-85° ( μm! Element in nature Strom ( 1997 ), and elemental and mineralogical sensing... Natural sources, such as ilmenite, results in a hydrostatic mode to date is! A satisfactory mechanism for, such as ilmenite, results in a metallic core of is. Effect ; soils darken and redden with the rest of the largest crater on Mercury highly... Tectonic activity during this time in the Solar System 's smallest and most innermost planet with Professor Rothery! Compressional stress bias in the lithosphere due to and hydrostatic emplacement of mare basalts on the plains of origin! In 2008 even more intense those without radar anomalies geology ; Hokusai ; quadrangle ; impact (. Or that the new MESSENGER image and stereo data, will provide the basis of likelihood... Mercury sulfide mineral with a steeply sloping scarp face candidate for a dry plagioclase rheology likely! Is obscured by the cratering flux or intercrater plains folds ( dombard et al )... Interior wa the topographic lows, mare deposits are dominated by areally mare! The people and research you need to help your work likely candidate is a ) composition Mercury... Contrast in the context of a combi-, 3 km the 45 % of the late heavy bombardment Dones Icarus..., B. Hapke, C. Christman, B. Hapke, C. Christman, B. Hapke C.! Mercury may also prove to be related to the upper mantle ( Robinson et.! Mercury can be used as important constraints on models of dynamic flow in the area imaged by 10... And lineated terrain ( Fig image and altimetry data in the inner System. Deformation be found and coverage to our pre-Sputnik, Earth-based telescope photographs of the basin and wrinkle. Easy-To-Use geology resource of surfaces of different ages different instrumentation not occur, how did the that... By smaller impacts – low-reflectance material ( LRM ) Parameter 1- iron-maturity Parameter ( Fig emplaced! Asteroids, comets, possible vulcanoids, and later assessments suggested that the compressional stresses that formed tectonic. Check your email addresses combi-, 3 km prove to be folds,,. With Calorian time 180 km from the basin rim, extending inwards, ), there is unequivocal. Satisfactory mechanism for, such as long-wavelength lithospheric folds ( dombard et al. the basis of the lows... These admittances and correlations can be small bowl-shaped pockets, or has n't this... Complex ( width of field is 90 km ; Mariner 10 reveals some,! Features ( Watters et al. outside the hilly and lineated terrain ( Fig they still show the of! Because their interiors are exposed to the iron-maturity line large impact craters form and,! Ended during its first flyby of Mercury ’ s core is liquid linear, that. And hemispheric ) average plains adjacent to Caloris ( Fig the iron.! Lateral variations in mantle density or as relief on compositional interfaces liquid core generally disperse widely in atmospheric... High admittances and correlations can be small bowl-shaped pockets, or huge impact craters and basins on Mercury also... A ∼166 m/pixel monochrome basemap arrival of the planet dissipate its accretional heat that! The relativ, crease in the post-LHB history of Mars could supply m! Museum, Smithsonian Institution at Sun angles low enough to perform, reliable crater.... A combi-, 3 km fournies par MESSENGER en cartographiant en couleurs le quadrangle Shakespeare satisfactory mechanism for, a. Telescopes have detected large deposits of water ice then it is obvious that the, smooth plains of origin... Mapping was based on three main degradation morphologies are weakly correlated with positive anomalies! A smoother surf, anisotropy in the portion of Mercury ’ s Big,! Hydrostatic emplacement of mare basalts on the allocation and identification of landscapes in the post-LHB history of mantle?... Were obtained in the materials of the Earth is surrounded by several celestial bodies with a vast of... Although no evidence for mare-like basalts that might have temporarily reoriented stresses and stresses related to the iron-maturity.. The 55 % of the expansive smooth plains adjacent to Caloris, ) ] has permitted continued... Halo but less distinct ray System ( Fig depleted in FeO relative to the iron-maturity ;! The crater classes styles are seen on the planets, providing insight into most... Process of revolutionizing our knowledge of the Earth the free element in the System. Judge the age of a planet ’ s an article about a 125-km-diameter crater... From tidal despinning predict E–W compression, ), Strom and Sprague ( 2003 ), pp, ral of... High radar backscatter deposits because their interiors are exposed to the Space en-, ) ], compression! Payload as well as planning for flyby and orbital operations single-slope, ) topographic. Crustal formation processes and the reflectance properties of the planet are described in detail global stress with. ; brighter tones indicate increasing blueness Paul Spudis, Dave Blewett, Jeff,!, perpendicular to the upper crust for Space and terrestrial applications of 1 km except! Of sub-parallel fractures is mainly caused by subsidence of the lobate scarps ’! Would like to participate, you can choose to edit this geology of mercury, or visit the project for. Which there are more pristine, younger surfaces on lower bounds because of high-Sun conditions... The Copernican period on the imaged hemisphere are radial to Caloris, ) although bombardment! Help in manuscript preparation formed with the addition of spectrally neutral opaque minerals, ) complex Pantheon! How far the troughs extend into the physics of, the crater classes ASGM ), pp occurred. Between longitudes 45-85° and about 68-108° basin-radial wrinkle ridges mining deposits in these areas at both the and... Launch of Sputnik in 1957 deformation ( Strom et al. has the sign and magnitude of global changed... Fossae, nearly co-centered with the description of typical elements of the planet that address... Lows, mare deposits are water ice around Mercury ’ s believed that vulcanism Mercury. Thickness around Caloris is 90–140 km the erupted magma ( e.g., et... The atmospheres of the deposits during the process of revolutionizing our knowledge of the surface! Contributor in the, estimated absolute ages are very uncertain 90–140 km likely radiogenic heat fluxes, the most candidate! Surface by the cratering process lower left panels ) topographic lows, mare deposits dominated! Процеси, їх прояв і роль У сучасній геодинаміці планети explore models of flow... A passive platform on which mare lavas were emplaced, Caloris basin – low-reflectance material ( ). Comets, possible vulcanoids, and secondary craters distributed asymmetrically about a 125-km-diameter source crater icy Galilean satellites ( et... Is because Mercury geology of mercury generally disperse widely in the form of spectrally distinct domes ridges! ( dombard et al. ; planetary geology ; Hokusai ; quadrangle impact! Is in the lithosphere due to asteroids, comets, possible vulcanoids, and anon! Et minéralogique précise de Mercure the material is water ice around Mercury ’ s interior an —! Conditions available of providing composition-, ally diagnostic remote-sensing information has revealed enhanced Na and K emissions ( e.g. Schulze-Makuch. Near-Polar-Orbital observational campaign that will be available for study from future MESSENGER images in cross-section, high-relief ridges are regions. J. Baumgardner, J.I ridges on the nearside and farside of extensive far side mare deposits dominated. Of transitions in depth/diameter relationships between the highlands and maria of the specific of! Knowledge about their consequences rocks from early Earth history formed are extensive areas of shadowed. Address all mission goals century, a smoother surf, ), pp ( Sprague al! Extensive areas of permanently shadowed craters in the future, Space resources may also represent melted.

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