Magma reservoirs and neutral buoyancy zones on Venus - Implications for the formation and evolution of volcanic landforms

Details Magma reservoirs and neutral buoyancy zones on Venus - Implications for the formation and evolution of volcanic landforms Magma reservoirs and neutral buoyancy zones on Venus - Implications for the formation and evolution of volcanic landforms

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....97.3877h&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 97, no. E3, March 25, 1992, p. 3877-3903. Research supported by William F

Physics

69

Landforms, Magma, Venus Surface, Volcanoes, Planetary Evolution, Venus Atmosphere

Scientific paper

The production of magma reservoirs and neutral buoyancy zones (NBZs) on Venus and the implications of their development for the formation and evolution of volcanic landforms are examined. The high atmospheric pressure on Venus reduces volatile exsolution and generally serves to inhibit the formation of NBZs and shallow magma reservoirs. For a range of common terrestrial magma-volatile contents, magma ascending and erupting near or below mean planetary radius (MPR) should not stall at shallow magma reservoirs; such eruptions are characterized by relatively high total volumes and effusion rates. For the same range of volatile contents at 2 km above MPR, about half of the cases result in the direct ascent of magma to the surface and half in the production of neutral buoyancy zones. NBZs and shallow magma reservoirs begin to appear as gas content increases and are nominally shallower on Venus than on earth. For a fixed volatile content, NBZs become deeper with increasing elevation: over the range of elevations treated in this study (-1 km to +4.4 km) depths differ by a factor of 2-4. Factors that may account for the low height of volcanoes on Venus are discussed.

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