Geology of the Shakespeare quadrangle (H03), Mercury

Guzzetta, L.; Galluzzi, V.; Ferranti, Luigi; Palumbo, P.

doi:10.1080/17445647.2017.1290556

Cited by 24 publications

(40 citation statements)

References 52 publications

(94 reference statements)

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“…As described in the latter references, digital compositing at this scale of published geologic maps is an ongoing project in support of the upcoming BepiColombo mission jointly conducted by the European Space Agency and the Japan Aerospace Agency. Figure b is a superposition of an updated version of the previous field magnitude map of H16 onto a similar composited geologic map of the Caloris side of Mercury (Guzzetta et al, ; Mancinelli et al, ). The updated version was produced from MESSENGER data after further editing to minimize downward continuation errors near the southern edge of the map, especially in and around Sobkou Planitia.…”

Section: Resultsmentioning

confidence: 99%

Investigating Sources of Mercury's Crustal Magnetic Field: Further Mapping of MESSENGER Magnetometer Data

et al. 2018

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One hundred six low‐altitude passes of magnetometer data from the last 2 months of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging mission have been applied to produce a map of the crustal magnetic field at a constant altitude of 40 km covering latitudes of 35–75∘ N and longitudes of 270–90∘ E. Some anomalies correlate significantly with impact basins/craters (e.g., Rustaveli and Vyasa), while other basins/craters have no obvious anomalies. A possible interpretation that is consistent with lunar evidence is that some impactors delivered more ferromagnetic Fe–Ni metal to the interior subsurfaces and ejecta fields of the craters/basins that they produced. The amount of metallic iron that could plausibly be delivered is limited by the diameter and mass of an impactor that would yield a crater with observed diameters (e.g., 200 km for Rustaveli). This in turn limits the maximum amplitude of anomalies that could be induced by impactor‐added iron in the present‐day Mercury global field to relatively low values. It is therefore concluded that if impactor‐added iron is the source of the observed crater‐associated anomalies, then they must be almost entirely a consequence of ancient remanent magnetization. A broad magnetic anomaly occurs over the northern rise, a topographically high region with an associated strong free air gravity anomaly. A possible interpretation of the latter anomaly is that an early major impact preconditioned the region for a later mantle uplift event.

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Section: Resultsmentioning

confidence: 99%

Investigating Sources of Mercury's Crustal Magnetic Field: Further Mapping of MESSENGER Magnetometer Data

et al. 2018

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“…[] and Guzzetta et al . [] show the exterior plains here as smooth plains passing outward into Odin Formation after about 100 km. At 176.5°W, 26°N, approximately where the buried rim (or a gap if it was originally discontinuous) must lie, there is a slightly fan‐shaped array of about eight 3 km wide, steep‐sided, flat‐bottomed fractures (Figure ) reminiscent of those occurring more abundantly in locations 1 and 3.…”

Section: The Critical Locationsmentioning

confidence: 99%

Mercury's Caloris basin: Continuity between the interior and exterior plains

et al. 2017

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The smooth plains on the floor of Mercury's Caloris basin and those almost entirely surrounding it beyond its rim are usually accepted to be younger than the rim materials and to be lava flows rather than impact melt. High‐resolution imaging shows that the emplacement of interior and exterior plains was concurrent, with evidence of both inward and outward flow while they were being emplaced. The Caloris rim is breached in two places by continuous smooth plains that seamlessly connect interior and exterior plains. The gross‐scale spectral and compositional distinctiveness of interior and exterior plains is blurred on a scale of several tens of kilometers, which could reflect interfingering of flow units less than a few hundred kilometers long that tapped melt sources of different composition and/or depth inside and outside the basin followed by local mixing of regolith. Flows occurring both inside and outside the basin should be included in estimates of the total erupted volume.

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“…In particular, we saw that the floor of Degas is covered by a bluish material, which is observed nowhere else, at least in the Shakespeare quadrangle. However, (Guzzetta et al, ) mapped Degas with the same geological unit than the surrounding craters (e.g., Erté) which do not present such kind of deposits on their floors. This discrepancy between the geological map of Guzzetta et al () and our color map can justify to define a spectral (or lithological) subunit, to combine both morphological and compositional information given by the two maps.…”

Section: Discussionmentioning

confidence: 99%

“…The Shakespeare quadrangle extends from 22.5°N to 65°N in latitude and from 180°E to 270°E in longitude and covers an area of about 5 × 10 6 km 2 . The 1:3M‐scale geological map of the quadrangle (Guzzetta et al, , and Figure ) shows the distribution of the terrain units and of the impact craters in this region of the planet. In particular, the main units occurring in Shakespeare are the SP and the IcP, whereas the ImP occur only as small patches (Guzzetta et al, ; Spudis & Guest, ; Trask & Guest, ).…”

Section: Data Set and Data Processingmentioning

confidence: 99%

“…The 1:3M‐scale geological map of the quadrangle (Guzzetta et al, , and Figure ) shows the distribution of the terrain units and of the impact craters in this region of the planet. In particular, the main units occurring in Shakespeare are the SP and the IcP, whereas the ImP occur only as small patches (Guzzetta et al, ; Spudis & Guest, ; Trask & Guest, ). The impact craters are more abundant in the eastern part of the quadrangle, which thus seems to be older than the western area, dominated by the Caloris ejecta (McCauley et al, ).…”

Section: Data Set and Data Processingmentioning

confidence: 99%

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Global Spectral Properties and Lithology of Mercury: The Example of the Shakespeare (H‐03) Quadrangle

et al. 2019

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The MErcury Surface, Space ENvironment, GEochemistry and Ranging mission showed the surface of Mercury with an accuracy never reached before. The morphological and spectral analyses performed thanks to the data collected between 2008 and 2015 revealed that the Mercurian surface differs from the surface of the Moon, although they look visually very similar. The surface of Mercury is characterized by a high morphological and spectral variability, suggesting that its stratigraphy is also heterogeneous. Here, we focused on the Shakespeare (H‐03) quadrangle, which is located in the northern hemisphere of Mercury. We produced an 8‐color cube of this quadrangle at 450‐m per pixel spatial resolution and with a complete coverage. Various selected color maps based on this eight‐color cube were used to analyze the spectral properties of this region to define its compositional variability and identify some clear units constrained by relevant spectral parameters: for example, we identified a higher concentration of low reflectance material around three main craters of Shakespeare (Degas, Akutagawa, and Sholem Aleichem) and in the area to the south of Sobkou Planitia delimited by 24.4°N to 28.4°N and −140°W to −125°W. Moreover, we selected some regions of interest, which can be proposed as particularly interesting targets for the Visual and Infrared Hyper‐spectral Imager and Mercury Radiometer and Thermal Imaging Spectrometer instruments onboard the BepiColombo spacecraft. This work can help for the geological analysis of this quadrangle, by integrating information that are usually not derived with a single morphostratigraphic analysis.

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Geology of the Shakespeare quadrangle (H03), Mercury

Cited by 24 publications

References 52 publications

Investigating Sources of Mercury's Crustal Magnetic Field: Further Mapping of MESSENGER Magnetometer Data

Investigating Sources of Mercury's Crustal Magnetic Field: Further Mapping of MESSENGER Magnetometer Data

Mercury's Caloris basin: Continuity between the interior and exterior plains

Global Spectral Properties and Lithology of Mercury: The Example of the Shakespeare (H‐03) Quadrangle

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