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"Rothery, David A"
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Geology of the Michelangelo quadrangle (H12), Mercury
The Michelangelo quadrangle of Mercury (H12) encompasses the area between latitudes 22.5°S-65°S and longitudes 180°E-270°E. The quadrangle covers almost 6.5% of the planet's surface with a total area of almost 5 million km
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. Geologic contacts and linear features were drawn at a mapping scale between 1:300,000 and 1:600,000, based on photointerpretation of MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) Mercury Dual Imaging System (MDIS) imagery. We distinguish three geomorphological plains units (smooth, intermediate, and intercrater plains) and, based on their degradation state, three morpho-stratigraphic classes of craters with diameter ≥ 20 km. The surface of this quadrangle is dominated by intermediate plains and by degraded crater materials of class c2. The geological map at 1:3,000,000 scale improves the existing 1:5,000,000 map based on Mariner-10 data. This work is a contribution to the Mercury geological map series planned to foster observational strategies of the ESA-JAXA BepiColombo mission.
Journal Article
Geology of the Derain quadrangle (H10), Mercury
We present the results of geological mapping of Mercury's Derain (H10) quadrangle (0°-72°E and 22.5°N-22.5°S) using data from the MESSENGER spacecraft. The map is presented on a scale of 1:3,000,000, for which linework was drawn at 1:300,000. We distinguish three major morphological plains units: Smooth, Intermediate, and Intercrater Plains. We produced two versions of the map, with craters classified according to a 3- and 5-class degradation system. This allows compatibility with other MESSENGER-era maps and Mariner 10-era maps. This map will help provide science context for the ESA-JAXA BepiColombo mission to Mercury.
Journal Article
Moons : a very short introduction
\"Proving to be both varied and fascinating, moons are far more common than planets in our Solar System. Our own Moon has had a profound influence on Earth, not only through tidal effects, but even on the behaviour of some marine animals. Many remarkable things have been discovered about the moons of the giant outer planets from Voyager, Galileo, Cassini, and other spacecraft. Scientists have glimpsed volcanic activity on Io, found oceans of water on Titan, and captured photos of icy geysers bursting from Enceladus. It looks likely that microbial life beyond the Earth may be discovered on a moon rather than a planet.\"-- --Provided by publisher.
Book
An Integrated Geologic Map of the Rembrandt Basin, on Mercury, as a Starting Point for Stratigraphic Analysis
Planetary geologic maps are usually carried out following a morpho-stratigraphic approach where morphology is the dominant character guiding the remote sensing image interpretation. On the other hand, on Earth a more comprehensive stratigraphic approach is preferred, using lithology, overlapping relationship, genetic source, and ages as the main discriminants among the different geologic units. In this work we produced two different geologic maps of the Rembrandt basin of Mercury, following the morpho-stratigraphic methods and symbology adopted by many authors while mapping quadrangles on Mercury, and an integrated geo-stratigraphic approach, where geologic units were distinguished also on the basis of their false colors (derived by multispectral image data of the NASA MESSENGER mission), subsurface stratigraphic position (inferred by crater excavation) and model ages. We distinguished two different resurfacing events within the Rembrandt basin, after the impact event, and four other smooth plains units outside the basin itself. This provided the basis to estimate thicknesses, volumes, and ages of the smooth plains inside the basin. Results from thickness estimates obtained using different methodologies confirm the presence of two distinct volcanic events inside the Rembrandt basin, with a total thickness ranging between 1–1.5 km. Furthermore, model ages suggest that the volcanic infilling of the Rembrandt basin is among the ones that extended well into the mid-Calorian period, when Mercury’s effusive volcanism was previously thought to be largely over.
Journal Article
Map of tectonic shortening structures in Chryse Planitia and Arabia Terra, Mars
We present a 1:4,000,000 scale map of tectonic landforms in Chryse Planitia and Arabia Terra, on either side of Mars' dichotomy. Our study area is a ∼3 million km
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region, transitional between Mars' highlands and lowlands including Oxia Planum, the landing site of the ExoMars rover. Using a structural mapping approach, we digitised all kilometre-scale tectonic structures at a scale of 1:50,000 using high-resolution data (∼6 m/pixel). Although this region is represented as sparsely tectonised on global tectonic maps, we find evidence of widespread tectonic shortening structures across the region. The shortening structures have a dominant N-S orientation and occur in all globally identified geological units. The structural map contributes to a broader understanding of the geological history of the region and Mars' wider tectonic history.
Journal Article
Geology of the Neruda quadrangle (H13), Mercury
We present the first geological map of the Neruda Quadrangle (H13), Mercury. H13 is in Mercury's southern hemisphere between latitudes 22.5°S-65°S, and longitudes 90°E-180° covering a total area of just under 5 million km², equivalent to 6.5% of the planet's surface. Map digitisation was carried out at scales between 1:300,000 and 1:700,000 for final presentation at 1:3,000,0000, from end-of-mission data products from NASA's MESSENGER mission. We distinguish three main photogeologic plains units: intercrater, intermediate, and smooth plains. We also distinguish all craters and their materials ≥ 20 km in diameter based on their degradation state. We have completed two versions of the map, one using a three-class crater degradation scheme and one using a five-class crater degradation scheme. In addition, specific geological units were charted for the Rembrandt impact basin. This map has been constructed to provide context and targets for the ESA-JAXA BepiColombo mission to Mercury.
Journal Article
Geology of the Hokusai quadrangle (H05), Mercury
The Hokusai (H05) quadrangle is in Mercury's northern mid-latitudes (0-90°E, 22.5-65°N) and covers almost 5 million km
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, or 6.5%, of the planet's surface. We have used data from the MESSENGER spacecraft to make the first geological map of H05. Linework was digitized at 1:400,000-scale for final presentation at 1:3,000,000-scale, mainly using a ∼166 m/pixel monochrome basemap. Three major photogeologic units of regional extent were mapped: intercrater, intermediate, and smooth plains. Materials of craters ≥ 20 km in diameter were classified according to their degradation state. Two classification schemes were employed in parallel, one with three classes and the other with five classes, for compatibility with existing MESSENGER-era quadrangle maps and the first global geologic map. This map will provide science context and targets for the ESA-JAXA BepiColombo mission to Mercury.
Journal Article
Strombolian explosive styles and source conditions: insights from thermal (FLIR) video
Forward Looking Infrared Radiometer (FLIR) cameras offer a unique view of explosive volcanism by providing an image of calibrated temperatures. In this study, 344 eruptive events at Stromboli volcano, Italy, were imaged in 2001–2004 with a FLIR camera operating at up to 30 Hz. The FLIR was effective at revealing both ash plumes and coarse ballistic scoria, and a wide range of eruption styles was recorded. Eruptions at Stromboli can generally be classified into two groups: Type 1 eruptions, which are dominated by coarse ballistic particles, and Type 2 eruptions, which consist of an optically-thick, ash-rich plume, with (Type 2a) or without (Type 2b) large numbers of ballistic particles. Furthermore, Type 2a plumes exhibited gas thrust velocities (>15 m s−1) while Type 2b plumes were limited to buoyant velocities (<15 m s−1) above the crater rim. A given vent would normally maintain a particular gross eruption style (Type 1 vs. 2) for days to weeks, indicating stability of the uppermost conduit on these timescales. Velocities at the crater rim had a range of 3–101 m s−1, with an overall mean value of 24 m s−1. Mean crater rim velocities by eruption style were: Type 1 = 34 m s−1, Type 2a = 31 m s−1, Type 2b = 7 m s−1. Eruption durations had a range of 6–41 s, with a mean of 15 s, similar among eruption styles. The ash in Type 2 eruptions originates from either backfilled material (crater wall slumping or ejecta rollback) or rheological changes in the uppermost magma column. Type 2a and 2b behaviors are shown to be a function of the overpressure of the bursting slug. In general, our imaging data support a broadening of the current paradigm for strombolian behavior, incorporating an uppermost conduit that can be more variable than is commonly considered.
Journal Article