Penetrating an impenetrable world

Penetrating the atmosphere of Venus

Penetrating the mysteries of Venus with a precision never before achieved is the goal of Venus Express.

With respect to the previous missions to Venus, the scientific instrumentation on board Venus Express is enormously improved.

This will allow studying in great detail the atmosphere of Venus, to understand its complex dynamics and its tight relationship with the surface and with the planetary space environment around it.

Venus Express data will answer some of the open questions about Venus and will allow definition of new objectives for future missions to the planet. ESA will achieve this by largely inheriting instruments from the scientific packages already developed for the Mars Express and Rosetta missions.

The ‘eyes’ of Venus Express are extremely sensitive to a wide range of electromagnetic wavelengths, from ultraviolet to infrared. They will be able to dig down through the atmosphere by exploiting for the first time the so-called ‘spectroscopic windows’, discovered in the late 1980s thanks to ground observations.

The radiation leaking from the deep atmosphere through these ‘windows’ can be observed on Venus’s night side. Infrared radiation from the lower atmosphere and even the surface can surprisingly escape to space, carrying precious information that Venus Express will collect from orbit.

Synergy is the strength of Venus Express

The underlying philosophy of Venus Express investigations is to observe the same target with different instruments at the same time. This provides a comprehensive, versatile and complete view of the different phenomena taking place on Venus.

  • Monitoring the temperatures: - PFS, VIRTIS, VeRa and SPICAV

  • Chemical composition: - VIRTIS, SPICAV and PFS

  • Climate, weather and global atmospheric dynamics: - VIRTIS and VMC, complemented by temperatures retrieved by PFS, VeRa and VIRTIS

  • Atmospheric escape into space: - ASPERA, in combination with SPICAV to assess how this process evolves in time

  • Interaction of solar wind with atmosphere: - ASPERA, MAG and VeRa

  • Surface roughness, temperature and other properties: - VeRa, together with VIRTIS, PFS and SPICAV

  • Volcanic activity: - VIRTIS, PFS and VMC, VIRTIS and PFS will also look for signs of seismic activity
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