Tessera terrains on Venus: global overview of their distribution, specific features, and relationships with other terrains based on the Magellan spacecraft data.

Details Tessera terrains on Venus: global overview of their distribution, specific features, and relationships with other terrains based on the Magellan spacecraft data. Tessera terrains on Venus: global overview of their distribution, specific features, and relationships with other terrains based on the Magellan spacecraft data.

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995avest..29..219i&link_type=abstract

Astronomicheskii Vestnik, Tom 29, No. 3, p. 219 - 242

Astronomy and Astrophysics

Astrophysics

Venus: Surface Structure

Scientific paper

The total number of tesserae mapped on the surveyed surface of Venus (98% of the total planetary surface) is 609. Their areas vary from 400 km2 to about 9 Mkm2. The total area of the whole tessera population is approximately 36 Mkm2, or about of 8% of the surface of Venus. The main part of the tessera population (69%) is concentrated in 11 regions, which are restricted to the Aphrodite and Ishtar Regions, Beta-Phoebe and Alpha-Lada Terrae. Tessera areas are unevenly distributed over the surface of Venus; they are mostly concentrated within the equatorial belt and the northern hemisphere and occur relatively rarely south of 30°S. Thorough examination of tessera boundaries with the adjacent plains indicates, first, that tesserae are the oldest stratigraphic unit on Venus and, second, allows one to suggest that the tessera extend beneath the plain covers and from their basements. The first tectonic stage in tesserae possibly predated the formation of vast Venusian lava plains, whose age is estimated at approximately 500 Ma. The second tectonic stage seemed to follow directly after the first and probably was nearly contemporaneous to the intratessera plains and the oldest units of surrounding plains. Specific size-frequency and areal distributions of tesserae, the morphology of their boundaries, and typical sequences of events are best described by a model of the catastrophic resurfacing of Venus (Saunders et al., 1992).

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