Impact craters and Venus resurfacing history

  title={Impact craters and Venus resurfacing history},
  author={Roger J. Phillips and Richard F. Raubertas and Raymond E. Arvidson and Ila C. Sarkar and Robert R. Herrick and Noam R. Izenberg and Robert Grimm},
  journal={Journal of Geophysical Research},
Venusian impact crater size-frequency distributions, locations, and preservation states were analyzed to reconstruct the history of resurfacing by tectonism and volcanism. An atmospheric transit model for meteoroids demonstrates that for craters larger than about 30 km, the size-frequency distribution is close to the atmosphere-free case. With this result, and assuming that the surface records a crater production population (a catastrophic resurfacing model, CRM), an age of cessation of rapid… 

Global Resurfacing of Venus

The impact cratering record on Venus is unique among the terrestrial planets. Fully 84% of the craters are in pristine condition, and only 12% are fractured. Remarkably, only 2.5% of the craters and

Recent volcanic resurfacing of Venusian craters

Ejecta from impact craters on Venus are a major source of fine-grained materials across the planet, and crater spatial distribution has been studied as a guide to the relative age and resurfacing

Mean age of rifting and volcanism on Venus deduced from impact crater densities

UNLIKE the extensively cratered highlands of the Moon and Mars, the surface of Venus does not preserve a record of heavy bombard-ment from the early history of the Solar System1-3. Those craters that

Dating volcanism and rifting on Venus using impact crater

Although the distribution of impact craters on Venus is indistinguishable from a completely spatially random population on the basis of crater data alone, the addition of geologic information

Venus: Crater distribution and plains resurfacing models

Detailed analysis of the distribution of craters on Venus using Mth nearest neighbor analysis, coupled with models based upon surface morphology constraints, indicates that the hypothesis of complete

Evidence for rapid regional plains emplacement on Venus from the population of volcanically embayed impact craters

We have reexamined the population of craters on Venus believed to be embayed by lava flows and discuss the reliability of criteria for determining the volcanic embayment state of a crater, presenting

Constraints on the resurfacing history of Venus from the hypsometry and distribution of volcanism, tectonism, and impact craters

Improved measurements of the target elevations of 885 impact craters on Venus indicate that they are nearly random with respect to elevation. Although a slight deficit of craters at high elevations

Floor subsidence and rebound of large Venus craters

The topography and geology of large craters on Venus reveal no evidence for floor rebound or relaxation; rather, the floors have subsided. Depressions of the floor centers relative to the margins are



On the nature and rate of resurfacing of Venus

Crater production and obliteration are modeled for the plains of Venus, using: (1 ) the observed distribution of Venus-crossing asteroids and comets, (2) viscous relaxation of crater topography, and

Limits on modes of lithospheric heat transport on Venus from impact crater density

We present a formalism by which the size-frequency distribution of impact craters on Venus may be used to estimate upper bounds on the mean global rates of volcanic resurfacing and lithospheric

Impact craters of Venus: Analysis of Venera 15 and 16 data

From description of impact craters on Venus and crater size-and-depth distributions, models are developed that analyze the size-distribution curve and radar-bright haloes around fresh craters. The

Impact Craters on Venus: What are they Telling Us?

Magellan has revealed an ensemble of impact craters on Venus that is unique in many important ways. We have compiled a data base describing the 842 craters on 89% of Venus' surface mapped through

Impact Craters on Venus: Initial Analysis from Magellan

Magellan radar images of 15 percent of the planet show 135 craters of probable impact origin, and there is apparently a spectrum of surface ages on Venus ranging approximately from 0 to 800 million years, and therefore Venus must be a geologically active planet.

Atmospheric effects on ejecta emplacement and crater formation on Venus from Magellan

The Venus cratering record provides a unique environment for assessing the effects of both gravity and an atmosphere on impact crater formation. This contribution uses surface signatures of energy

Surface modification of Venus as inferred from Magellan observations of plains

In Sedna Planitia, clear stratigraphic relations can be discerned among volcanic flow units. Young flows exhibit SAR specific cross section values similar to fresh terrestrial basalt flows, whereas

Impact craters of Venus: A continuation of the analysis of data from the Venera 15 and 16 spacecraft

Additional studies of Venusian impact craters have been made based on an analysis of Venera 15/16 radar imagery and altimetry. The crater population on Venus has been subdivided into groups

Mechanisms for lithospheric heat transport on Venus: Implications for tectonic style and volcanism

The tectonic and volcanic characteristics of the surface of Venus are poorly known, but these characteristics must be closely related to the mechanism by which Venus rids itself of internal heat. On

Venus volcanism: Classification of volcanic features and structures, associations, and global distribution from Magellan data

A preliminary analysis of a global survey of Magellan data covering over 90% of the surface and designed to document the characteristics, location, and dimensions of all major volcanic features on