What We Learned From the Venus Surface in-situ Exploration And What Looks Promising to do Next

Details What We Learned From the Venus Surface in-situ Exploration And What Looks Promising to do Next What We Learned From the Venus Surface in-situ Exploration And What Looks Promising to do Next

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p23e..08b&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #P23E-08

Computer Science

Sound

6295 Venus

Scientific paper

The in-situ study of Venus surface started on Dec 15, 1970 with the landing of the Soviet Venera 7 probe, which sent back to Earth data on the surface temperature and atmosphere pressure. Then, since 1972 till 1985 there were successful landings of the Soviet Venera 9 to 14 and Vega 1-2 probes. The Day probe, part of the US Pioneer Venus Multiprobe (1978), also sent the data from the Venus surface. Gained by these missions we have the results of gamma-spectrometry measurements of K, U, and Th contents in the surface material in five sites and the X-ray fluorescence measurements of major elements contents in three sites as well as TV panoramas of four landing sites. In addition, in some of these sites there have been measured the surface material density, bearing capacity and electro conductivity as well as albedo and color. The results of the geochemical measurements, all characterizing Venusian plains, are consistent with basaltic composition of the surface material in all seven sampled sites. Recent comparisons of the Venusian compositions with those of the extended database of terrestrial magmatic rocks from different geodynamic environments within the oceanic crust showed that except one (Venera 14) all other measurements suggest enrichment in LIL elements and differ from N-MORB compositions. The surface in the imaged landing sites was found to consist of very dark finely layered and mechanically weak rock and even darker soil. Recent joint analysis of the Veneras' and Magellan data showed that the layered rock most likely is thermally sintered airborn sediment of fine debris derived from ejecta of impact craters. This sediment, although of small thickness, seems to be widespread on the Venus surface that should be taken into account in planning new missions. The future landings have to provide more compositional knowledge on Venus surface by significantly improving the analyses accuracies and detection limits and extending sampled geologic formations beyond the already sampled plains. Determination of mineralogic composition of the surface material as well as the redox-controlling components of the atmosphere are of a key value. Seismic and other geophysical sounding of Venus interior should be also planned. Sample return mission(s) as distant but necessary step in Venus studies should be considered too.

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