Venus Express
Venus Express (VEX) was the first Venus exploration mission of the European Space Agency (ESA). Launched in November 2005, it arrived at Venus in April 2006 and began continuously sending back science data from its polar orbit around Venus. Equipped with seven scientific instruments, the main objective of the mission was the long term observation of the Venusian atmosphere. The observation over such long periods of time had never been done in previous missions to Venus, and was key to a better understanding of the atmospheric dynamics. ESA concluded the mission in December 2014.<ref name="esa20141216">Template:Cite web</ref><ref>Template:Cite web</ref><ref>Template:Cite web</ref><ref>Template:Cite web</ref>
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Objectives
Starting out in the early planetary system with similar sizes and chemical compositions, the histories of Venus and Earth have diverged in spectacular fashion. The Venus Express data were intended to contribute not only to in-depth understanding of how the Venusian atmosphere is structured today, but also to understanding of the changes that led to the current greenhouse atmospheric conditions. Such investigations contribute to the study of climate change on Earth.<ref>Template:Cite web</ref><ref>Template:Cite web</ref><ref>Template:Cite web</ref><ref>Template:Cite web</ref>
Instruments
ASPERA-4: An acronym for "Analyzer of Space Plasmas and Energetic Atoms," ASPERA-4 investigated the interaction between the solar wind and the Venusian atmosphere, determine the impact of plasma processes on the atmosphere, determine global distribution of plasma and neutral gas, study energetic neutral atoms, ions and electrons, and analyze other aspects of the near Venus environment. ASPERA-4 is a re-use of the ASPERA-3 design used on Mars Express, but adapted for the harsher near-Venus environment.<ref>Template:Cite web</ref><ref>ASPERA-4: Analyser of Space Plasmas and Energetic Atoms</ref>
MAG: The magnetometer was designed to measure the strength of Venus's magnetic field and the direction of it as affected by the solar wind and Venus itself. It mapped the magnetosheath, magnetotail, ionosphere, and magnetic barrier in high resolution in three-dimensions, aid ASPERA-4 in the study of the interaction of the solar wind with the atmosphere of Venus, identify the boundaries between plasma regions, and carry planetary observations as well (such as the search for and characterization of Venus lightning). MAG was derived from the Rosetta lander's ROMAP instrument.<ref name=":1">MAG: The Fluxgate Magnetometer of Venus Express</ref><ref name=":2">Template:Cite web</ref>
One measuring device was placed on the body of the craft. The identical second of the pair was placed the necessary distance away from the body by unfolding a Template:Convert boom (carbon composite tube). Two redundant pyrotechnical cutters cut one loop of thin rope to free the power of metal springs. The driven knee lever rotated the boom perpendicularly outwards and latched it in place. Only the use of a pair of sensors together with the rotation of the probe allowed the spacecraft to resolve the small natural magnetic field beneath the disturbing fields of the probe itself.<ref name=":1" /><ref name=":2" />
The measurements to identify the fields produced by the craft took place on the route from Earth to Venus.<ref>Template:Cite web</ref><ref name="pope639">Template:Cite journal</ref> The lack of magnetic cleanness was due to the reuse of the Mars Express spacecraft bus, which did not carry a magnetometer.<ref name="pope639" /> By combining the data from two-point simultaneous measurements and using software to identify and remove interference generated by Venus Express itself, it was possible to obtain results of a quality comparable to those produced by a magnetically clean craft.<ref name="pope639" />
VMC: The Venus Monitoring Camera is a wide-angle, multi-channel CCD. The VMC is designed for global imaging of the planet.<ref>Template:Cite web</ref> It operated in the visible (VIS), ultraviolet (UV), and near infrared (NIR1 and NIR2) spectral ranges, and maps surface brightness distribution searching for volcanic activity, monitoring airglow, studying the distribution of unknown ultraviolet absorbing phenomenon at the cloud-tops, and making other science observations.<ref>Template:Cite journal</ref><ref>Template:Cite web</ref><ref>Template:Cite web</ref>
It was derived in part from the Mars Express High Resolution Stereo Camera (HRSC) and the Rosetta Optical, Spectroscopic and Infrared Remote Imaging System (OSIRIS). The camera is based on a Kodak KAI-1010 Series, 1024 x 1024 pixel interline CCD, and included an FPGA to pre-process image data, reducing the amount transmitted to Earth.<ref name=":0" /><ref>Template:Cite web</ref>
The consortium of institutions responsible for the VMC included the Max Planck Institute for Solar System Research, the Institute of Planetary Research at the German Aerospace Center and the Institute of Computer and Communication Network Engineering at Technische Universität Braunschweig.<ref>Template:Cite web</ref> It is not to be confused with Visual Monitoring Camera mounted on Mars Express, of which it is an evolution.<ref name=":0">Template:Cite web</ref><ref>Template:Cite web</ref>
| VMC Channel | Central Wavelength | Spectral Range |
|---|---|---|
| VIS | 513 nm | 503 – 523 nm |
| NIR1 | 935 nm | 900 – 970 nm |
| NIR2 | 1.01 μm | 990 – 1030 nm |
| UV | 365 nm | 345 – 385 nm |
PFS: The "Planetary Fourier Spectrometer" (PFS) should have operated in the infrared between the 0.9 μm and 45 μm wavelength range and was designed to perform vertical optical sounding of the Venus atmosphere. It should have performed global, long-term monitoring of the three-dimensional temperature field in the lower atmosphere (cloud level up to 100 kilometers).<ref>Template:Cite web</ref>
Furthermore, it should have searched for minor atmospheric constituents that may be present, but had not yet been detected, analyzed atmospheric aerosols, and investigated surface to atmosphere exchange processes. The design was based on a spectrometer on Mars Express, but modified for optimal performance for the Venus Express mission. However PFS failed during its deployment and no useful data was transmitted.<ref name="Lakdawalla2007">Template:Cite news</ref>
SPICAV: The "SPectroscopy for Investigation of Characteristics of the Atmosphere of Venus" (SPICAV) is an imaging spectrometer that was used for analyzing radiation in the infrared and ultraviolet wavelengths. It was derived from the SPICAM instrument flown on Mars Express. However, SPICAV had an additional channel known as SOIR (Solar Occultation at Infrared) that was used to observe the Sun through Venus's atmosphere in the infrared.<ref>Template:Cite journal</ref><ref>Template:Cite web</ref>
VIRTIS: The "Visible and Infrared Thermal Imaging Spectrometer" (VIRTIS) was an imaging spectrometer that observed in the near-ultraviolet, visible, and infrared parts of the electromagnetic spectrum. It analyzed all layers of the atmosphere, surface temperature and surface/atmosphere interaction phenomena.<ref>Template:Cite web</ref><ref>VIRTIS for Venus Express</ref><ref>Template:Cite web</ref>
VeRa: Venus Radio Science was a radio sounding experiment that transmitted radio waves from the spacecraft and passed them through the atmosphere or reflected them off the surface. These radio waves were received by a ground station on Earth for analysis of the ionosphere, atmosphere and surface of Venus. It was derived from the Radio Science Investigation instrument flown on Rosetta.<ref>Template:Cite web</ref><ref>Template:Cite journal</ref>
Mission history
Background
The mission was proposed in 2001 to reuse the design of the Mars Express mission. However, some mission characteristics led to design changes: primarily in the areas of thermal control, communications and electrical power. For example, since Mars is approximately twice as far from the Sun as Venus, the radiant heating of the spacecraft was four times greater for Venus Express than Mars Express. Also, the ionizing radiation environment was harsher. On the other hand, the more intense illumination of the solar panels resulted in more generated photovoltaic power. The Venus Express mission also used some spare instruments developed for the Rosetta spacecraft. The mission was proposed by a consortium led by D. Titov (Germany), E. Lellouch (France), and F. Taylor (United Kingdom).<ref>Template:Cite journal</ref>
Launch campaign
Venus Express completed its final phase of testing at Astrium Intespace facility in Toulouse, France on 3 August 2005 and arrived at the airport of the Baikonur Cosmodrome on 7 August 2005. First flight verification test was completed on 16 August 2005. Integrated System Test-3 was completed on 22 August 2005. Last major system test successfully started on 30 August 2005. Electrical testing was completed on 5 September 2005. The Fuelling Readiness Review was completed on 21 September 2005. The spacecraft was mated to the Fregat upper stage on 12 October 2005.<ref>Template:Cite web</ref>
The launch window for Venus Express was open from 26 October to 23 November 2005, with the launch initially set for 26 October 4:43 UTC. However, problems with the insulation from the Fregat upper stage (detected on 21 October 2005) led to a two-week launch delay to inspect and clear out the small insulation debris that migrated on the spacecraft.<ref>Template:Cite web</ref> The spacecarft arrived at launch pad on 5 November 2005 and it was launched by a Soyuz-FG/Fregat rocket on 9 November 2005 at 03:33:34 UTC into a parking Earth orbit and 1 h 36 min after launch put into its transfer orbit to Venus. <ref>Template:Cite web</ref><ref>Template:Cite web</ref><ref>Template:Cite journal</ref>
In space
Three trajectory correction maneuvers were successfully performed on 11 November 2005, 24 February 2006, and 29 March 2006. The main engine was fired successfully on 17 February 2006 in a dress rehearsal for the arrival maneuver.<ref>Template:Cite web</ref> The command stack for orbit insertion maneuver was loaded on the spacecraft on 7 April 2006. The spacecraft arrived at Venus on 11 April 2006, after 153 days of journey, and fired its main engine between 07:10:29 and 08:00:42 UTC SCET to reduce its velocity so that it could be captured by Venusian gravity into an orbit of Template:Convert.<ref name="nssdc">Template:Cite web</ref> The burn was monitored from ESA's Control Centre ESOC in Darmstadt, Germany. Period of this initial orbit was nine days.<ref name="nssdc" />
| Event | Spacecraft event time (UTC) | Ground receive time (UTC) |
|---|---|---|
| Liquid Settling Phase start | 07:07:56 | 07:14:41 |
| VOI main engine start | 07:10:29 | 07:17:14 |
| periapsis passage | 07:36:35 | |
| eclipse start | 07:37:46 | |
| occultation start | 07:38:30 | 07:45:15 |
| occultation end | 07:48:29 | 07:55:14 |
| eclipse end | 07:55:11 | |
| VOI burn end | 08:00:42 | 08:07:28 |
Seven further orbit control maneuvers, two with the main engine and five with the thrusters, were required for Venus Express to reach its final operational 24-hour orbit around Venus.<ref name="nssdc" /> First images of Venus from Venus Express were released on 13 April 2006.<ref>Template:Cite web</ref>
| Time | Event | Result |
|---|---|---|
| 20 April 2006 | Apoapsis Lowering Manoeuvre #1 | Orbital period changed to 40 hours |
| 23 April 2006 | Apoapsis Lowering Manoeuvre #2 | Orbital period changed to 25 hours 43 minutes |
| 26 April 2006 | Apoapsis Lowering Manoeuvre #3 | slight fix to previous ALM |
In target orbit
Venus Express entered its target orbit at apoapsis on 7 May 2006 at 13:31 UTC, when the spacecraft was Template:Convert from Earth. At this point the spacecraft was running on an ellipse substantially closer to the planet than during the initial orbit. The polar orbit ranged between Template:Convert over Venus. The periapsis was located almost above the North pole (80° North latitude), and it took 24 hours for the spacecraft to travel around the planet.<ref>Template:Cite web</ref>
Venus Express studied the Venusian atmosphere and clouds in detail, the plasma environment and the surface characteristics of Venus from orbit. It also made global maps of the Venusian surface temperatures. Its nominal mission was originally planned to last for 500 Earth days (approximately two Venusian sidereal days) until 19 September 2007, but the mission was extended five times: first on 28 February 2007 until early May 2009; then on 4 February 2009 until 31 December 2009; and then on 7 October 2009 until 31 December 2012.<ref>Template:Cite web</ref> On 22 November 2010, the mission was extended to 2014.<ref>Template:Cite web</ref> On 20 June 2013, the mission was extended a final time until 2015.<ref>Template:Cite web</ref> Between 18 June and 11 July 2014, the spacecraft performed successful aerobraking experiments<ref>Template:Cite web</ref> with multiple passes at 131 to 135 km altitude.<ref>Template:Cite web</ref><ref>Template:Cite web</ref>
End of mission
On 28 November 2014, mission control lost contact with Venus Express. Intermittent contact was reestablished on 3 December 2014, though there was no control over the spacecraft, likely due to exhaustion of propellant.<ref name="SpaceDaily-2014-12-08">Template:Cite news</ref> On 16 December 2014, ESA announced that the Venus Express mission had ended.<ref name="esa20141216" /> A carrier signal was still being received from the vehicle, but no data was being transmitted. Mission manager Patrick Martin expected the spacecraft would fall below Template:Convert in early January 2015, with destruction occurring in late January or early February.<ref name="natgeo20141217">Template:Cite news</ref> The spacecraft's carrier signal was last detected by ESA on 18 January 2015.<ref name="esa20150123" />
Science results
- 14 December 2006: First temperature map of the southern hemisphere.<ref>Template:Cite web</ref>
- 27 November 2007: A series of papers was published in Nature giving the initial findings. It finds evidence for past oceans. It confirms the presence of lightning on Venus and that it is more common on Venus than it is on Earth. It also reports the discovery that a huge double atmospheric vortex exists at the south pole of the planet.<ref>Template:Cite journal</ref><ref>Template:Cite news</ref>
- 20 May 2008: The detection by the VIRTIS instrument of hydroxyl (OH) in the atmosphere of Venus is reported in the May 2008 issue of Astronomy & Astrophysics.<ref>Template:Cite web</ref>
- October 2008: Venus Express was used to observe signs of life on Earth from Venus orbit. In images acquired by the probe, Earth was less than one pixel in size, which mimics observations of Earth-sized planets in other planetary systems. These observations were then used to develop methods for habitability studies of exoplanets.<ref>Template:Cite web</ref>
- 25 August 2011: A layer of ozone was found in the upper atmosphere of Venus.<ref>Template:Cite news</ref><ref>Template:Cite journal</ref>
- 1 October 2012: A cold layer, where dry ice may exists, was found in the atmosphere of Venus.<ref>Template:Cite web</ref>
- November 2025: Analysis of data from Venus Express and Akatsuki show that diurnal thermal tides are the primary driver of transporting momentum toward the tops of Venus's clouds, contributing substantially to the atmosphere's superrotation.<ref>Template:Cite news</ref><ref>Template:Cite journal</ref>
See also
- List of ESA programmes and missions
- Uncrewed space mission
- List of planetary probes
- List of missions to Venus
- List of uncrewed spacecraft by program
- Space exploration
- Space telescope
- Space probe
- Timeline of artificial satellites and space probes
- Timeline of planetary exploration
References
Further reading
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- Venus Express mission page by the European Space Agency
- Venus Express mission page by ESA Spacecraft Operations
- Venus Express profile by NASA's Solar System Exploration
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