NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
Magma reservoirs and neutral buoyancy zones on Venus - Implications for the formation and evolution of volcanic landformsThe 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.
Document ID
19920048475
Document Type
Reprint (Version printed in journal)
Authors
Head, James W. (NASA Headquarters Washington, DC United States)
Wilson, Lionel (Brown University Providence, RI, United States)
Date Acquired
August 15, 2013
Publication Date
March 25, 1992
Publication Information
Publication: Journal of Geophysical Research
Volume: 97
Issue: E3 M
ISSN: 0148-0227
Subject Category
LUNAR AND PLANETARY EXPLORATION
Funding Number(s)
CONTRACT_GRANT: NGR-40-002-088
CONTRACT_GRANT: NAGW-713
Distribution Limits
Public
Copyright
Other