Latitudinal variations of CO and OCS in the lower atmosphere of Venus from near-infrared nightside spectro-imaging

Icarus ◽  
2005 ◽  
Vol 179 (2) ◽  
pp. 375-386 ◽  
Author(s):  
E MARCQ ◽  
B BEZARD ◽  
T ENCRENAZ ◽  
M BIRLAN
Keyword(s):  
Near Infrared ◽  
Lower Atmosphere ◽  
Latitudinal Variations ◽  
Spectro Imaging ◽  
Atmosphere Of Venus

The deep atmosphere of Venus

1994 ◽  
Vol 349 (1690) ◽  
pp. 273-283 ◽  
Keyword(s):  
Carbon Monoxide ◽  
Near Infrared ◽  
Thermal Structure ◽  
Extreme Case ◽  
Lower Atmosphere ◽  
The Earth ◽  
Northern Latitudes ◽  
Low Latitudes ◽  
Remote Measurements ◽  
Atmosphere Of Venus

Venus as a planet resembles the Earth, but has a much hotter and denser atmosphere due to an extreme case of the greenhouse effect, caused by compositional differences and the thick cloud cover. Studies of the lower atmosphere are inhibited by the cloud opacity, which makes remote measurements at most frequencies short of the radio range quite difficult. Progress in understanding of the composition and thermal structure below the clouds has been made by the Pioneer and Venera entry probes of the 1970s, and more recently with results from the Galileo fly-by in 1990. The latter exploited the newly discovered near-infrared ‘windows’ to achieve measurements of carbon monoxide and water vapour abundances in the deep atmosphere, and provided the first detailed view of the global cloud structure. The morphology and spatial variations seen in the main mass of clouds are remarkable, and suggest a powerful and diverse meteorology dominated by convection. Carbon monoxide is significantly more abundant at high northern latitudes than at low latitudes in either hemisphere.

Sulfuric acid vapor and sulfur dioxide in the atmosphere of Venus as observed by the Venus Express Radio Science Experiment VeRa

2021 ◽  
Author(s):  
Janusz Oschlisniok ◽  
Bernd Häusler ◽  
Martin Pätzold ◽  
Silvia Tellmann ◽  
Michael Bird
Keyword(s):  
Sulfuric Acid ◽  
Transport Model ◽  
Lower Atmosphere ◽  
Local Times ◽  
Acid Vapor ◽  
Radio Science ◽  
X Band ◽  
Wide Range ◽  
Venus Express ◽  
Atmosphere Of Venus

<p>The main cloud deck within Venus' atmosphere, which covers the entire planet between approx. 50 and 70 km altitude, is believed to consist mostly of liquid sulfuric acid. The temperature below the main clouds is high enough to evaporate the H2SO4 droplets into gaseous sulfuric acid forming a haze layer which extends to altitudes as deep as 35 km. Gaseous sulfuric acid in Venus’ lower atmosphere is responsible for a strong absorption of radio waves as seen in Mariner, Pioneer Venus, Magellan and Venera radio science observations. Radio wave absorption measurements can be used to derive the amount of H2SO4 in Venus’ atmosphere. The radio science experiment VeRa onboard Venus Express probed the atmosphere of Venus between 2006 and 2014 with radio signals at 13 cm (S-band) and 3.6 cm (X-band) wavelengths. The orbit of the Venus Express spacecraft allowed to sound the atmosphere over a wide range of latitudes and local times providing a global picture of the sulfuric acid vapor distribution. We present the global H2SO4(g) distribution derived from the X-band radio signal attenuation for the time of the entire Venus Express mission. The observation is compared with results obtained from a 2-D transport model. The VeRa observations were additionally used to estimate the abundance of SO2 near the cloud bottom. The global distribution of SO2 at these altitudes is presented and compared with results obtained from other experiments. Eight years of VEX observation allow to study the long-term evolution of H2SO4 and SO2. The latter is presented for the northern polar region.</p>

scholarly journals Structure of the Lower Atmosphere of Venus.

1962 ◽  
Vol 67 ◽  
pp. 281 ◽  
Author(s):  
Carl Sagan
Keyword(s):  
Lower Atmosphere ◽  
Atmosphere Of Venus

scholarly journals Near-Infrared Spectroscopy of the Surface of Mars Derived from TIGER Spectro-Imaging Data

1995 ◽  
Vol 149 ◽  
pp. 298-299
Author(s):  
P. Martin ◽  
P.C. Pinet ◽  
R. Bacon ◽  
A. Rousset
Keyword(s):  
Infrared Spectroscopy ◽  
Spatial Resolution ◽  
Near Infrared Spectroscopy ◽  
Near Infrared ◽  
Western Hemisphere ◽  
Imaging Data ◽  
Integral Field Spectrograph ◽  
Integral Field ◽  
Spectro Imaging

AbstractHigh spectral and spatial resolution telescopic observations of the western hemisphere of Mars, using the integral field spectrograph TIGER at 0.8-1.1 µm, are described.

Dust in the Lower Atmosphere of Venus

Science ◽  
1969 ◽  
Vol 163 (3864) ◽  
pp. 275-276 ◽  
Author(s):  
A. D. Anderson
Keyword(s):  
Lower Atmosphere ◽  
Atmosphere Of Venus

scholarly journals Evidence for carbonyl sulfide (OCS) conversion to CO in the lower atmosphere of Venus

2009 ◽  
Vol 114 ◽  
Author(s):  
Yuk L. Yung ◽  
M. C. Liang ◽  
X. Jiang ◽  
R. L. Shia ◽  
C. Lee ◽  
...  
Keyword(s):  
Carbonyl Sulfide ◽  
Lower Atmosphere ◽  
Atmosphere Of Venus

scholarly journals The near-infrared nitric oxide nightglow in the upper atmosphere of Venus

2009 ◽  
Vol 106 (4) ◽  
pp. 985-988 ◽  
Author(s):  
A. Garcia Munoz ◽  
F. P. Mills ◽  
G. Piccioni ◽  
P. Drossart
Keyword(s):  
Nitric Oxide ◽  
Near Infrared ◽  
Upper Atmosphere ◽  
Atmosphere Of Venus

Sulfur trioxide in the lower atmosphere of Venus?

Icarus ◽  
1983 ◽  
Vol 53 (1) ◽  
pp. 1-9 ◽  
Author(s):  
R.A. Craig ◽  
R.T. Reynolds ◽  
B. Ragent ◽  
G.C. Carle ◽  
F. Woeller ◽  
...  
Keyword(s):  
Sulfur Trioxide ◽  
Lower Atmosphere ◽  
Atmosphere Of Venus

Structure of the lower atmosphere of Venus

Icarus ◽  
1962 ◽  
Vol 1 (1-6) ◽  
pp. 151-169 ◽  
Author(s):  
Carl Sagan
Keyword(s):  
Lower Atmosphere ◽  
Atmosphere Of Venus
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