Mercury: A post-Mariner 10 assessment

  title={Mercury: A post-Mariner 10 assessment},
  author={R. Strom},
  journal={Space Science Reviews},
  • R. Strom
  • Published 1979
  • Geology
  • Space Science Reviews
Our knowledge of Mercury has improved dramatically since the flight of Mariner 10. The planet is probably differentiated into a large iron-rich core (∼75% of the total radius) and a relatively thin (∼600 km) silicate mantle. Although the surface of Mercury superficially resembles the Moon, there are three main differences: (1) large areas of relatively old intercrater plains, (2) a widespread (probably global) distribution of lobate scarps, and (3) a similar albedo between young smooth plains… Expand
The chronology of Mercury's geological and geophysical evolution: The vulcanoid hypothesis
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Geologic evolution and cratering history of Mercury
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Did 26Al and impact‐induced heating differentiate Mercury?
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The partial volatilization of Mercury
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The Geophysics of Mercury: Current Status and Anticipated Insights from the MESSENGER Mission
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Radar altimetry of Mercury: A Preliminary analysis
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Mercury radar studies and lunar comparisons
Abstract Results from radar observations of Mercury are reviewed, the used as a basis for comparison of Mercury with its closest geologic relative, the Moon. Both bodies show very similarExpand
The Depletion of the Putative Vulcanoid Population via the Yarkovsky Effect
Abstract The geophysical history of Mercury is constrained by its crater record, its tectonics, and its magnetic field. Standard thermal models based on these constraints lead to inconsistent resultsExpand
Mercury: Radar images of the equatorial and midlatitude zones
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Tectonism and volcanism on Mercury
Mercury appears to have a tectonic framework and diastrophic history not found on other terrestrial planets explored to date (earth, Mars, and the moon). On the part of the planet viewed by MarinerExpand
Surface History of Mercury: Implications for Terrestrial Planets
A working hypothesis of Mercury's history is presented. We infer the surface of Mercury to record a sequence of events broadly similar to those recorded on the moon, implying similar histories ofExpand
Preliminary geologic terrain map of Mercury
A geologic terrain map of Mercury has been constructed by use of the photogeologic methods employed for the moon and Mars. The oldest and most widespread unit, intercrater plains, forms nearly levelExpand
Origin and relative age of lunar and Mercurian intercrater plains
Abstract Differences in the diameter/density distribution of craters in the size range 7–100 km between heavily cratered areas and areas of intercrater plains indicate the deposition of both lunarExpand
Some aspects of core formation in Mercury
Evidence for a large metallic core in Mercury is all indirect; the internal magnetic field may imply a convective dynamo; the surface geology is suggestive of large-scale differentiation; and thermalExpand
Mercury's Surface: Preliminary Description and Interpretation from Mariner 10 Pictures
The surface morphology and optical properties of Mercury resemble those of the moon in remarkable detail and record a very similar sequence of events, suggesting Mercury is probably a differentiated planet with a large iron-rich core. Expand
Global tectonics of Mercury and the moon
Lobate scarps on Mercury have been studied to determine the nature of the surface stress history and implications for the planet's early tectonic history. Morphologic and transection relationsExpand
Moon-Mercury - Relative preservation states of secondary craters
Abstract Geologic mapping of the Kuiper quadrangle of Mercury and other geologic studies of the planet indicate that secondary craters are much better preserved than those on the moon around primaryExpand
Consequences of the tidal slowing of Mercury
Abstract Mercury, currently rotating very slowly, probably rotated faster in the past. If Mercury's rotation period had been near 8 hours initially, similar to that of most solar system bodies today,Expand
Moon-Mercury: Large impact structures, isostasy and average crustal viscosity
Thirty-five craters and basins larger than 200 km in diameter are recognized on the imaged portion (45%) of Mercury. If the unimaged portion of the planet is similarly cratered, a total of 78 suchExpand