A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express

@article{Drossart2007ADU,
  title={A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express},
  author={Pierre Drossart and Giuseppe Piccioni and J.‐C. G{\'e}rard and Miguel Angel Lopez‐Valverde and Agust{\'i}n S{\'a}nchez‐Lavega and L. V. Zasova and Ricardo Hueso and Fredric W. Taylor and Bruno B{\'e}zard and Alberto Adriani and Francesco Angrilli and Gabriele Arnold and Kevin H. Baines and Giancarlo Bellucci and Johannes Benkhoff and J. P. Bibring and Armando Blanco and Maria I. Blecka and Robert W. Carlson and Angioletta Coradini and Andrea Maria di Lellis and Thérèse Encrenaz and St{\'e}phane Erard and Sergio Fonti and Vittorio Formisano and Thierry Fouchet and R. Garc{\'i}a and R. Haus and J. Helbert and Nikolay I. Ignatiev and P.G.J. Irwin and Y. Langevin and S{\'e}bastien Lebonnois and David Luz and Lucia Marinangeli and Vincenzo Orofino and Alexander V. Rodin and Maarten C. Roos-Serote and Bortolino Saggin and Daphne M. Stam and D. V. Titov and Guido Visconti and Massimo Zambelli and Constantine C. C. Tsang},
  journal={Nature},
  year={2007},
  volume={450},
  pages={641-645}
}
The upper atmosphere of a planet is a transition region in which energy is transferred between the deeper atmosphere and outer space. Molecular emissions from the upper atmosphere (90–120 km altitude) of Venus can be used to investigate the energetics and to trace the circulation of this hitherto little-studied region. Previous spacecraft and ground-based observations of infrared emission from CO2, O2 and NO have established that photochemical and dynamic activity controls the structure of the… 

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References

SHOWING 1-10 OF 19 REFERENCES

Non-LTE Infrared Emissions of CO2 in the Atmosphere of Venus

Abstract A non-local thermodynamic equilibrium (non-LTE) radiative transfer model previously developed for the martian atmosphere has been applied to the venusian atmosphere to study the CO2 infrared

Ground‐based near‐infrared observations of the Venus nightside: 1.27‐μm O2(a 1Δ g ) airglow from the upper atmosphere

Near-infrared spectroscopic observations of Venus taken in 1975 revealed O2(a1Δg) airglow from both the dayside and nightside of the planet with emission rates exceeding 1 mega-Rayleigh (1 MR = 1012

Venus II--geology, geophysics, atmosphere, and solar wind environment

The final orbit of Venus by the Magellan spacecraft in October 1994 brought to a close an exciting period of Venus reconnaissance and exploration. The scientific studies resulting from data collected

South-polar features on Venus similar to those near the north pole

Observations of Venus’ south-polar region are reported, where clouds with morphology much like those around the north pole, but rotating somewhat faster than the northern dipole are seen.

O2/1 Delta/ emission in the day and night airglow of Venus

We have detected an intense airglow from O/sub 2/(/sup 1/..delta..) at 1.27 ..mu..m on both the light and the dark sides of Venus, using a ground-based, high-resolution Fourier transform