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Density of impact craters on tessera, venus
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Ivanov, M. A. Basilevsky, A. T. |
| Copyright Year | 1993 |
| Description | After the plains, tessera is the most abundant terrain on Venus. It occupies about 10 percent of the Venusian surface, forming the continent-like blocks and small islands above the adjacent plains. Tessera is a result of tectonic deformations of some precursor terrain. However, the nature of that precursor, as well as the causes and mechanisms of its formations, are under debate. Any models considering tessera terrain involve estimation of tessera age, either relative or absolute. It is well known that the important information on the age of a planetary surface comes from impact crater statistics. The Magellan global overview of Venus with improved resolution provides an opportunity to gather data on impact craters in amounts large enough for statistically reliable estimations of crater density for different terrains. Our study of impact crater density on tesserae compared to the surrounding terrains has a goal to determine whether it is higher, lower, or the same and to interpret it in terms of the tessera age and processes involved. |
| File Size | 160022 |
| Page Count | 2 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_19940011790 |
| Archival Resource Key | ark:/13960/t5p896d88 |
| Language | English |
| Publisher Date | 1993-01-01 |
| Access Restriction | Open |
| Subject Keyword | Lunar And Planetary Exploration Venus Planet Deformation Planetary Geology Terrain Meteorite Craters Topography Venus Surface Tectonics Estimates Planetary Crusts Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
