scholarly journals Circulation of Venusian Atmosphere at 90–110 km Based on Apparent Motions of the O 2 1.27 μm Nightglow From VIRTIS‐M (Venus Express) Data

2018 ◽  
Vol 45 (5) ◽  
pp. 2554-2562 ◽  
Author(s):  
D. A. Gorinov ◽  
I. V. Khatuntsev ◽  
L. V. Zasova ◽  
A. V. Turin ◽  
G. Piccioni
Keyword(s):  
Venus Express ◽  
Venusian Atmosphere

Vertical Wavenumber Spectra of Gravity Waves in the Venus Atmosphere Obtained from Venus Express Radio Occultation Data: Evidence for Saturation

2015 ◽  
Vol 72 (6) ◽  
pp. 2318-2329 ◽  
Author(s):  
Hiroki Ando ◽  
Takeshi Imamura ◽  
Toshitaka Tsuda ◽  
Silvia Tellmann ◽  
Martin Pätzold ◽  
...  
Keyword(s):  
Diffusion Coefficient ◽  
Power Law ◽  
Gravity Waves ◽  
Radio Occultation ◽  
Spectral Power ◽  
European Space Agency ◽  
Small Scale ◽  
Turbulent Diffusion Coefficient ◽  
Venus Express ◽  
Venusian Atmosphere

Abstract By using the vertical temperature profiles obtained by the radio occultation measurements on the European Space Agency (ESA)’s Venus Express, the vertical wavenumber spectra of small-scale temperature fluctuations that are thought to be manifestations of gravity waves are studied. Wavenumber spectra covering wavelengths of 1.4–7.5 km were obtained for two altitude regions (65–80 and 75–90 km) and seven latitude bands. The spectra show a power-law dependence on the high-wavenumber side with the logarithmic spectral slope ranging from −3 to −4, which is similar to the features seen in Earth’s and Martian atmospheres. The power-law portion of the spectrum tends to follow the semiempirical spectrum of saturated gravity waves, suggesting that the gravity waves are dissipated by saturation as well as radiative damping. The spectral power is larger at 75–90 km than at 65–80 km at low wavenumbers, suggesting amplitude growth with height of unsaturated waves. It was also found that the wave amplitude is larger at higher latitudes and that the amplitude is maximized in the northern high latitudes. On the assumption that gravity waves are saturated in the Venusian atmosphere, the turbulent diffusion coefficient was estimated. The diffusion coefficient in the Venusian atmosphere is larger than those in Earth’s atmosphere because of the longer characteristic vertical wavelength of the saturated waves.

Investigation of the surface of Venus with VIRTIS on Venus Express

2006 ◽  
Author(s):  
Mr. Nils Müller ◽  
Dr. Jorn Helbert ◽  
Dr. Lucia Marinangeli ◽  
Prof. George Hashimoto ◽  
Mr. Kevin Baines ◽  
...  
Keyword(s):  
Venus Express

Sulfuric acid vapor and sulfur dioxide in the atmosphere of Venus as observed by the Venus Express radio science experiment VeRa

Icarus ◽  
2021 ◽  
Vol 362 ◽  
pp. 114405
Author(s):  
J. Oschlisniok ◽  
B. Häusler ◽  
M. Pätzold ◽  
S. Tellmann ◽  
M.K. Bird ◽  
...  
Keyword(s):  
Sulfuric Acid ◽  
Sulfur Dioxide ◽  
Acid Vapor ◽  
Radio Science ◽  
Venus Express ◽  
Atmosphere Of Venus

scholarly journals The Case (or Not) for Life in the Venusian Clouds

Life ◽  
2021 ◽  
Vol 11 (3) ◽  
pp. 255
Author(s):  
Dirk Schulze-Makuch
Keyword(s):  
Natural Selection ◽  
Environmental Conditions ◽  
Cloud Layer ◽  
Harsh Conditions ◽  
Venusian Atmosphere

The possible detection of the biomarker of phosphine as reported by Greaves et al. in the Venusian atmosphere stirred much excitement in the astrobiology community. While many in the community are adamant that the environmental conditions in the Venusian atmosphere are too extreme for life to exist, others point to the claimed detection of a convincing biomarker, the conjecture that early Venus was doubtlessly habitable, and any Venusian life might have adapted by natural selection to the harsh conditions in the Venusian clouds after the surface became uninhabitable. Here, I first briefly characterize the environmental conditions in the lower Venusian atmosphere and outline what challenges a biosphere would face to thrive there, and how some of these obstacles for life could possibly have been overcome. Then, I discuss the significance of the possible detection of phosphine and what it means (and does not mean) and provide an assessment on whether life may exist in the temperate cloud layer of the Venusian atmosphere or not.

scholarly journals Venus surface data extraction from VIRTIS/Venus Express measurements: Estimation of a quantitative approach

2008 ◽  
Vol 113 ◽  
Author(s):  
Gabriele Arnold ◽  
Rainer Haus ◽  
David Kappel ◽  
Pierre Drossart ◽  
Giuseppe Piccioni
Keyword(s):  
Data Extraction ◽  
Quantitative Approach ◽  
Surface Data ◽  
Venus Express

scholarly journals Did Lomonosov see the Venusian atmosphere?

Physics Today ◽  
2012 ◽  
Vol 65 (11) ◽  
pp. 11-12 ◽  
Author(s):  
Jay M. Pasachoff ◽  
William Sheehan
Keyword(s):  
Venusian Atmosphere

Calibration of Hyperspectral Imaging Data: VIRTIS-M Onboard Venus Express

2010 ◽  
Author(s):  
Alejandro Cardesin Moinelo ◽  
Giuseppe Piccioni ◽  
Eleonora Ammannito ◽  
Gianrico Filacchione ◽  
Pierre Drossart
Keyword(s):  
Hyperspectral Imaging ◽  
Imaging Data ◽  
Venus Express

Venus Express In-Flight Experience

2006 ◽  
Author(s):  
Andrea Accomazzo ◽  
Peter Schmitz ◽  
Ignacio Tanco
Keyword(s):  
Flight Experience ◽  
Venus Express
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