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

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

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sosyr..29..189i&link_type=abstract

Solar System Research, Vol. 29, No. 3, p. 189 - 209

Computer Science

Venus: Surface Structure

Scientific paper

Magellan synthetic aperture radar images serve as the basis for a global overview of tessera distribution, characterization of tessera boundaries, and tentative establishment of typical sequences of events in tessera terrains. 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 million km2. The total area of the entire tessera population is approximately 36 million km2, 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 and Beta-Phoebe and Alpha-Lada Terrae. Tesserae 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 reveals that essentially everywhere (about 97% of the total boundary length), the material of lava plains overlaps onto tessera margins. This indicates, first, that tesserae are the oldest stratigraphic unit on Venus and, second, allows one to suggest that the tesserae extend beneath the plain covers and form their basements. Computer simulation of tessera lava flooding shows that the thickness of this mantle may range from a few hundred m to several km.

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