Mathematics – Logic
Scientific paper
Nov 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982icar...52..365g&link_type=abstract
(International Conference on the Venus Environment, Palo Alto, CA, Nov. 1-6, 1981.) Icarus, vol. 52, Nov. 1982, p. 365-372.
Mathematics
Logic
23
Magma, Planetary Geology, Venus (Planet), Volcanology, Basalt, Bubbles, Carbon Dioxide, Effusives, Venus Atmosphere
Scientific paper
Theoretical consideration of the magma vesiculation process under observed and inferred venusian surface conditions suggests that vesicles should form in basaltic melts, especially if CO2 is the primary magmatic volatile. However, the high surface atmospheric pressure (about 90 bars) and density on Venus retard bubble coalescence and disruption sufficiently to make explosive volcanism unlikely. The products of explosive volcanism (fire fountains, convecting eruption clouds, pyroclastic flows, and topography-mantling deposits of ash, spatter, and scoria) should be rare on Venus, and effusive eruptions should dominate. The volume fraction of vesicles in basaltic rocks on Venus are predicted to be less than in chemically similar rocks on earth. Detection of pyroclastic landforms or eruption products on Venus would indicate either abnormally high volatile contents of Venus magmas (2.5-4 wt%) or different environmental conditions (e.g., lower atmospheric pressure) in previous geologic history.
Garvin James B.
Head James W.
Wilson Leslie
No associations
LandOfFree
Magma vesiculation and pyroclastic volcanism on Venus does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Magma vesiculation and pyroclastic volcanism on Venus, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magma vesiculation and pyroclastic volcanism on Venus will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1757571