| タイトル | Characterizing Volcanic Eruptions on Venus: Some Realistic (?) Scenarios |
| 本文（外部サイト） | http://hdl.handle.net/2060/20120011799 |
| 著者（英） | Glaze, L. S.; Stofan, E. R.; Grinspoon, D. H. |
| 著者所属（英） | NASA Goddard Space Flight Center |
| 発行日 | 2011-03-07 |
| 言語 | eng |
| 内容記述 | When Pioneer Venus arrived at Venus in 1978, it detected anomalously high concentrations of SO2 at the top of the troposphere, which subsequently declined over the next five years. This decline in SO2 was linked to some sort of dynamic process, possibly a volcanic eruption. Observations of SO2 variability have persisted since Pioneer Venus. More recently, scientists from the Venus Express mission announced that the SPICAV (Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus) instrument had measured varying amounts of SO2 in the upper atmosphere; VIRTIS (Visible and Infrared Thermal Imaging Spectrometer) measured no similar variations in the lower atmosphere (ESA, 4 April, 2008). In addition, Fegley and Prinn stated that venusian volcanoes must replenish SO2 to the atmosphere, or it would react with calcite and disappear within 1.9 my. Fegley and Tremain suggested an eruption rate on the order of approx 1 cubic km/year to maintain atmospheric SO2; Bullock and Grinspoon posit that volcanism must have occurred within the last 20-50 my to maintain the sulfuric acid/water clouds on Venus. The abundance of volcanic deposits on Venus and the likely thermal history of the planet suggest that it is still geologically active, although at rates lower than Earth. Current estimates of resurfacing rates range from approx 0.01 cubic km/yr to approx 2 cubic km/yr. Demonstrating definitively that Venus is still volcanically active, and at what rate, would help to constrain models of evolution of the surface and interior, and help to focus future exploration of Venus. |
| NASA分類 | Lunar and Planetary Science and Exploration |
| レポートNO | GSFC.CPR.01191.2012 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
|
