A warm layer in Venus' cryosphere and high-altitude measurements of HF, HCl, H2O and HDO

  title={A warm layer in Venus' cryosphere and high-altitude measurements of HF, HCl, H2O and HDO},
  author={J L Bertaux and Ann Carine Vandaele and Oleg I. Korablev and Eric Villard and Anna A. Fedorova and Didier Fussen and Eric Qu{\'e}merais and D. A. Belyaev and Arnaud Mahieux and Franck Montmessin and Christine H. Muller and Eddy Neefs and Dennis Nevejans and Valérie Wilquet and Jean-Pierre Dubois and Alain Hauchecorne and Alexander V. Stepanov and Imant I. Vinogradov and Alexander V. Rodin},
Venus has thick clouds of H2SO4 aerosol particles extending from altitudes of 40 to 60 km. The 60–100 km region (the mesosphere) is a transition region between the 4 day retrograde superrotation at the top of the thick clouds and the solar–antisolar circulation in the thermosphere (above 100 km), which has upwelling over the subsolar point and transport to the nightside. The mesosphere has a light haze of variable optical thickness, with CO, SO2, HCl, HF, H2O and HDO as the most important minor… 

HDO and H2O vertical distributions and isotopic ratio in the Venus mesosphere by Solar Occultation at Infrared spectrometer on board Venus Express

[1] Vertical distributions of the molecular density and mixing ratios of H2O and HDO in the Venus mesosphere have been obtained using Solar Occultation at Infrared (SOIR), a high-resolution (with

Ozone on Mars and Venus

Cross-hemispheric circulation of the atmosphere is a major feature of the Martian troposphere and Venusian thermosphere. On Mars, it is driven by the latitudinal gradient of insolation at the

Direct observations of Venus upper mesospheric temperatures from ground based spectroscopy of CO2

We report direct observations of temperatures in the Venus upper mesosphere around 110 km altitude (0.15 Pa). Information about temperatures at these altitude regions are sparse especially for the

Densities and temperatures in the Venus mesosphere and lower thermosphere retrieved from SOIR on board Venus Express: Carbon dioxide measurements at the Venus terminator

[1] SOIR is a high-resolution spectrometer flying on board the ESA Venus Express mission. It performs solar occultations of the Venus high atmosphere, and so defines unique vertical profiles of many



Morphology of the Venus ultraviolet night airglow

Images of the nightside of Venus in the (0,1)delta band of nitric oxide have been obtained by the Pioneer Venus orbiter ultraviolet spectrometer (OUVS). The emission, which is produced by radiative

The altitude distribution of the Venus ultraviolet nightglow and implications on vertical transport

The altitude distribution of the nitric oxide nightglow was measured with an ultraviolet spectrometer on board Pioneer Venus, in order to study the effects of the distribution on the Venus nightside

The deep atmosphere of Venus revealed by high-resolution nightside spectra

THE night side of Venus is anomalously bright in two narrow spectral windows centred at 1.74 and 2.3 µm (ref. 1). The source of this emission has been identified recently as thermal radiation from

The Venus nitric oxide night airglow: Model calculations based on the Venus thermospheric general circulation model

Pioneer Venus (PV) orbiter ultraviolet spectrometer (OUVS) images of the nightside airglow in the (0, 1) δ band of nitric oxide showed a maximum whose average location was at 0200 local solar time

Global circulation, thermal structure, and carbon monoxide distribution in Venus' mesosphere in 1991

Abstract Millimeter-wave observations of CO lines have provided a detailed picture of Venus' mesosphere dynamics in 1991 from simultaneous measurements of absolute wind velocities in two layers and

Isotopic fractionation through water vapor condensation: The Deuteropause, a cold trap for deuterium in the atmosphere of Mars

Recent observations of deuterium atoms at Lyman alpha with the Hubble Space Telescope have shown the puzzling result of a D/H ratio in the upper atmosphere of Mars to be 11 times smaller than the D/H

Radio Occultation Studies of the Venus Atmosphere with the Magellan Spacecraft: 2. Results from the October 1991 Experiments

On October 5 and 6, 1991, three dual-frequency ingress radio occultation experiments were conducted at Venus during consecutive orbits of the Magellan spacecraft. The radio signals probed a region of