SummaryFor two years beginning in 2013, a large team led by Sanjay Limaye set out to combine and compare the following:
Venusian atmospheric data collected by probes in the 1970s and 1980s (used to create the Venus International Reference Atmosphere, or VIRA) Venus Express data on the vertical and horizontal structure of the atmosphereEarth - based observations of the upper atmosphere temperature structure of Venus made since VIRAFigure 1a: Vertical coverage of post-VIRA atmospheric structure experi....
Venusian atmospheric dynamics, in ultraviolet light, show intricate meteorological patterns.
Not exact matches
Prospects for
Venusian life have been dismissed because of harsh conditions on the planet's surface: there is no water, temperatures reach 477 °C and the
atmospheric pressure is 92 times that on Earth's surface.
Thus, it is plausible that changes to
atmospheric ionization rates due to cosmic ray variability may affect the occurrence of electrical phenomena in the
Venusian atmosphere (Nordheim et al. 2015) hence manifesting a relation between space weather and meteorological phenomena.
While the large
atmospheric pressure at the surface and the high altitude of the
Venusian cloud layer appears to exclude the possibility of cloud - to - ground lightning (Gurnett et al. 2001; Aplin 2006), several authors have suggested that lightning discharges above, between or within clouds may occur (Borucki 1982; Russell & Scarf 1990; Gurnett et al. 2001).
While the exact mechanism for charging and for initiating lightning within the
Venusian clouds is not currently known (Yair 2012) it is nonetheless likely that cosmic ray ionization has an important role in this process as it is believed to be the primary source of
atmospheric ions at middle and low altitudes.
The atmosphere of Venus is mostly CO2 but the
atmospheric heat arises as a result of the mass and density of the
Venusian atmosphere (apparently more than 90 times that of the Earth) not just the absorption characteristics of CO2.