The Venus geologic mappers' handbook

Tanaka, Kenneth L.; Moore, H. J.; Shaber, G.G.; Chapman, M. G.; Stofan, ER; Campbell, D. B.; Davis, Philip A.; Guest, J. E.; McGill, G. E.; Rogers, P. G.; Saunders, R. S.; Zimbelman, J. R.

doi:10.3133/ofr94438

Cited by 54 publications

(20 citation statements)

References 133 publications

(14 reference statements)

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“…Considering their small size, we mapped only the brighter and larger clusters (>10 km long), consistent with the larger hollow groups collected in the database of Thomas et al (2014a). Following USGS recommendations (Tanaka et al, 2011), our mapping scale led us to avoid digitising outcrops (e.g. central peaks) smaller than 4 km.…”

Section: Geodatabase Structure and Line Drawingmentioning

confidence: 99%

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Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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Mercury's quadrangle H02 'Victoria' is located in the planet's northern hemisphere and lies between latitudes 22.5°N and 65°N, and between longitudes 270°E and 360°E. This quadrangle covers 6.5% of the planet's surface with a total area of almost 5 million km 2 . Our 1:3,000,000-scale geologic map of the quadrangle was produced by photo-interpretation of remotely sensed orbital images captured by the MESSENGER spacecraft. Geologic contacts were drawn between 1:300,000 and 1:600,000 mapping scale and constitute the boundaries of intercrater, intermediate and smooth plains units; in addition, three morpho-stratigraphic classes of craters larger than 20 km were mapped. The geologic map reveals that this area is dominated by Intercrater Plains encompassing some almost-coeval, probably younger, Intermediate Plains patches and interrupted to the north-west, north-east and east by the Calorian Northern Smooth Plains. This map represents the first complete geologic survey of the Victoria quadrangle at this scale, and an improvement of the existing 1:5,000,000 Mariner 10-based map, which covers only 36% of the quadrangle. ARTICLE HISTORY

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Section: Geodatabase Structure and Line Drawingmentioning

confidence: 99%

“…The mapping scale is the scale at which it is recommended to draw lines. USGS guidelines suggest drawing contacts at a scale two to five times larger than the final output scale (Tanaka, Skinner, & Hare, 2011). Generally, drawing contacts at a scale five times larger generates cleaner and smoother linework.…”

Section: Mapping and Final Output Scalesmentioning

confidence: 99%

Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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“…In distinguishing our units we followed the recommendations of The Venus Geologic Mappers' Handbook (Tanaka, 1994), which, in turn, inherits experience of the geologic mapping of the Solar System planets and satellites summarized in Wilhelms (1990). Mapping Venus (or other planets) is based on photogeologic analysis of images of the planets.…”

Section: Description Of Geologic Unitsmentioning

confidence: 99%

“…In the case of Venus this work began with available local (e.g., Campbell et al, 1990) and regional (e.g., Kotelnikov et al, 1989) coverage, but global analyses were not possible until global SAR images with a resolution of 120± 220 m of almost the entire surface of Venus were acquired by the Magellan mission . Beginning in the early 1990s this work started partly as initiatives of individual researchers and groups, and as part of the NASA-funded Venus Geological Mapping Program coordinated by the US Geological Survey (Tanaka, 1994). This paper is derived from a presentation made at the Chapman Conference on Geodynamics of Venus on 4±6 September 1997, in Snowmass at Aspen, Colorado.…”

Section: Introductionmentioning

confidence: 99%

Geologic units on Venus: evidence for their global correlation

Basilevsky

Head

2000

Planetary and Space Science

116

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“…Some alternate criteria are needed in order to assemble different local areas into global stratigraphic units. As is the case on other planets and satellites, these criteria can be developed through photogeologic mapping and stratigraphic studies, which are a goal of numerous ongoing mapping projects for Venus [Tanaka, 1994; The first goal of this paper is to consider the published age estimates in the context of this global stratigraphic model in order to further test the model. The second goal is to use the stratigraphy as a tool to summarize a scenario for the geologic history of Venus that is consistent with crater density esimates and other crater-based evidence for the duration of various geologic processes and events.…”

mentioning

confidence: 99%

The geologic history of Venus: A stratigraphic view

Basilevsky¹,

Head²

1998

J. Geophys. Res.

173

139

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Abstract. On the basis of regional and global stratigraphic analyses, we outline the major events in the geologic history of Venus determined by photogeological study of surface features. Because the morphological signatures of terrain emplaced prior to the time of tessera formation are not preserved, the stratigraphic record presented comprises only the last 10-20% of the total history of Venus. The estimated range of the mean crater retention age of the surface (from -200 to 1600 million years) leads us to describe the timing and duration of different events in terms of fractions of the mean surface age T. The beginning of the observed history of Venus was characterized by intensive tectonic deformation of global or semi-global scale which formed the tessera terrain. Termination of the compressional stage is estimated to have occurred at about 1.4T while the tensional stage lasted for another 0.1-0.2T. After tessera formation, several stages of extensive volcanism occurred, burying vast areas of tessera and forming what are now observed as regional plains. The combined duration of the emplacement of these plains is estimated to be about 0.2-0.3T, with an implied average global rate of volcanism of a few cubic kilometers per year. Regional plains-forming matedhals can be subdivided and are separated from each other, and from underlying and overlying units, by unconformities. These unconformities are formed, from oldest to youngest, by tessera-forming deformation, dense fracturing, broad ridging, and, finally, wrinkle ridging. These tectonic episodes are interpreted to be generally globally synchronous and to represent successive episodes characterized by the dominance of compression, then tension, then again compression, and, finally, tension. The last global-scale tectonic episode, extensive wrinkle ridging, happened at about time T, which was very close in time to the emplacement of the most areally abundant plains unit. This marked the transition to the present stage of the history of Venus, which is characterized by a predominance of regional rifting and related volcanism. This stage appears to have lasted from about time T to the present, making it the longest time duration among the stratigraphic units considered, although the resulting tectonic and volcanic features and deposits cover only 10-20% of the surface of Venus. These observations mean that the general intensity of tectonics and the flux of volcanism (a few tenths of a cubic kilometer per year) in this latest period were much lower than those in earlier times. In summary, the morphologically observable part of the history of Venus was characterized by two key characteristics that stand in contrast to the comparable period of Earth history (approximately the Phanerozoic) when global geodynamic processes were dominated by plate tectonics: (1) Venus shows no signature of plate tectonics; instead, its global tectonic environment passed from an initial dominance of compression, through tension, then again compression, and finally tension, with the de...

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The Venus geologic mappers' handbook

Cited by 54 publications

References 133 publications

Geology of the Victoria quadrangle (H02), Mercury

Geology of the Victoria quadrangle (H02), Mercury

Geologic units on Venus: evidence for their global correlation

The geologic history of Venus: A stratigraphic view

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