Instrument: VIRTISDescription: Video sequence of ten images taken over a period of five hours at half-hourly intervals on 7 April 2007, showing the south polar vortex at a wavelength of 3.9 µm. The image on the right shows a comparison between Venusian topographie as derived from Pioneer Venus radar data with an image in the 2.3µm window obtained by NIMS on Galileo. At this wavelength atmospheric stripe-like structures are observed on the planet's day side, the nature of which is as yet unexplained. Analyser of Space Plasmas and Energetic Atoms, Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus, Visible and Infrared Thermal Imaging Spectrometer, Mars Express PFS and Venus Express SPICAV-SOIR. Instrument: VIRTISDistance: 190 000 - 315 000 kmDescription: Infrared images at 5 µm of the Venus southern hemisphere, clearly showing the double vortex at the south pole.

Venus Express/VIRTIS using a band ratio technique, Icarus (2009), doi: 10.1016/j.icarus.2009.01.001 This is a PDF file of an unedited manuscript that has been accepted for publication.

April 4-8 2016 G. Piccioni et al.

The vortex is very complex, with atmospheric gases flowing in different directions at different altitudes. The scientific objectives of the Venus Express Mission is to carry out a comprehensive study of the atmosphere of Venus and to study in detail the plasma environment of the planet and its interaction with the solar wind. • Instrument: VIRTISDistance: ~64 000 kmDescription: Monochrome image of the south polar region imaged at 1.7 µm, showing the distinctive pattern of cloud wave structure at around 55° southern latitude. VIRTIS -Venus Express The Scientific Questions The scientific objectives of the Venus Express Mission is to carry out a comprehensive study of the atmosphere of Venus and to study in detail the plasma environment of the planet and its interaction with the solar wind. VIRTIS per Venus Express. INAF - ISTITUTO DI ASTROFISICA e PLANETOLOGIA SPAZIALE Via Fosso del Cavaliere 100 00133 Roma Webmaster Romolo Politi last update: 10/01/2013 The scientific investigations are focussed on seven scientific \"Themes\" namely: A number of major scientific questions exist concerning Venus. VIRTIS (Visible and Infrared Thermal Imaging Spectrometer) is a complex instrument initially devoted to the remote sensing study of comet Wirtanen on the Rosetta mission, at wavelengths between 0.3 and 5 µm. The SOIR element of SPICAV will investigate the chemistry, structure and dynamics of the Venusian atmosphere as well as vertical profiling of the aeronomic emissions. The data are initially processed to correct for instrumental straylight from the dayside of Venus and to improve wavelength registration. Instrument: VIRTISDescription: A faint and variable nightglow of nitric oxide (NO) has been unambiguously detected in the upper atmosphere of Venus. VEX will also study the interactions between the atmosphere and the inter-planetary environment (solar wind) to better understand the evolution of the planet. The VIRTIS spectrometer on Venus Express observed three of these windows over much of the southern hemisphere of Venus. Instrument: VIRTISDescription: Large map of Venus's night side, as observed at 1.7 µm on 12 April 2006, during Venus Express's first orbit around the planet - capture orbit. The right side shows thermal radiation from the different cloud layers. Data from Venus Express have been available in the PSA since 2008. Instrument: VIRTISDistance: 35 000 kmDescription: Image at 2.3 μm of Venus's atmospheric region over which NASA's MESSENGER passed on 5 June 2007 (closest approach is marked with the circle). Dedicated studies of the surface shall be performed as well.

ESA uses cookies to track visits to our website only, no personal information is collected. Instrument: VIRTISDescription: The VIRTIS instrument has made the first detection of hydroxyl (OH) in the atmosphere of Venus. The spare model of the VIRTIS experiment for the ESA Rosetta mission has been considered, with some modification, as one of the instrument core payload for an ESA mission called Venus Express. The scientific objective of the ASPERA-4 experiment is to study the solar wind-atmosphere interaction and characterise the plasma and neutral gas environment in near-Mars space through Energetic Neutral Atom (ENA) imaging and local charged particle measurements. why is Venus so different from the Earth, in spite of the similarities in terms of size, basic composition and distance to the sun. Instrument: VMCDistance: 7505 - 1570 kmDescription: Mosaic of images taken at 365 nanometres on 24 April 2006, flying over the northern hemisphere. The difference in contrast and structure is readily apparent. MAG will study this process and will help in understanding the effect this has on the atmosphere. The most striking results are the observations of the south polar double vortex, which has for the first time been imaged at this level of detail. By searching for suddenly appearing, localized hotspots VIRTIS can search directly for volcanic activity. Scientific objectives cover meteorology of the middle atmosphere, surface mineralogy, aeronomy of the upper atmosphere and a dynamical study of the Venusian atmosphere. Our main interest in VIRTIS on Venus Express is in the use of the spectral windows to study the low atmosphere and the surface directly. Instrument: VIRTISDistance: 190 000 - 315 000 kmDescription: Composite views of Venus in ultraviolet at 380 nm (left side, blue colour scheme) and infrared at 1.7 µm (right side, red colour scheme). This is the first detection of OH in the atmosphere of a planet other than Earth. Venus Observational Parameters Discoverer: Unknown Discovery Date: Prehistoric Distance from Earth Minimum (10 6 km) 38.2 Maximum (10 6 km) 261.0 Apparent diameter from Earth Maximum (seconds of arc) 66.0 Minimum (seconds of arc) 9.7 Maximum visual magnitude -4.8 Mean values at inferior conjunction with Earth Distance from Earth (10 6 km) 41.44 Apparent diameter (seconds of arc) 60.2 Venus Express (VEX) is investigating the complex dynamics and chemistry of the Venusian atmosphere, and the interactions between the atmosphere and the surface, which will give clues about the characteristics of the surface. VRA (sometimes referred to as VeRa) uses the radio link between the spacecraft and Earth to investigate the density, temperature, and pressure of the atmosphere from ~35km up to 100km. VIRTIS is an imaging spectrometer which allows Venus Express to map details of Venus from the surface to the mesosphere. The derived differences in surface rock composition are consistent with suspicions that Venus once had a plate tectonics system and an ocean of water. La missione IXPE (Imaging X-ray Polarimetry Explorer) e’ stata selezionata come prossima missione spaziale del programma Explorer della NASA. VIRTIS is an imaging spectrometer which allows Venus Express to map details of Venus from the surface to the mesosphere. VIRTIS will be the first instrument to use the near-infrared atmospheric windows for for a global mapping and a global study of the surface composition. The difference in observing distances is reflected in the level of observed detail. Clearly visible are the "colder" mountain-tops on the "warm" lowlands. Instrument: VIRTISDescription: Temperature map of the Venusian surface based on data gathered on 10 August 2006, at 1.02, 1.10 & 1.18 μm during orbit 112 by VIRTIS (left), compared with predictions based on the Magellan topographic data obtained in the early 1990s (right). Following theoretical studies have shown the existing of several spectral windows in the infrared range. A localized enrichment of these gases would ba a tell-tale sign of active volcanism. Venus Express launched successfully on 9 November 2005 at 03:33 UT (8 November 10:33 p.m. EST) on a Soyuz-Fregat booster from the Baikonur Cosmodrome in Kazakhstan. Instrument: VIRTISDescription: The first infrared map of the surface temperature on Venus in the southern hemisphere has been obtained with VIRTIS. • Detailed latitudinal and local time profiles show symmetric features on both hemispheres. Instrument: VIRTISDistance: 190 000 - 315 000 kmDescription: Set of images at 5 µm of the Venus southern hemisphere. By taking the negative image, bright regions now represent the areas of more cloud cover. @ Venus Conference 2016 -Oxford VIRTIS-Venus Express-G. Piccioni, P. Drossart and the VIRTIS-VenusX Team

Instrument: VIRTISDistance: 190 000 - 315 000 kmDescription: Movie of false-colour images at 5 µm, showing Venus's southern hemisphere and the evolution of the south polar vortex. They clearly show the variation of cloud structures with latitude. Same colour scheme as the above movie. This type of images are used for measuring the wind speed. Instrument: VIRTIS and VMCDescription: The connection between the UV absorption features and the physical conditions and dynamical processes at the cloud tops have long been unclear. VMC will make global images and will study the cloud dynamics and image the surface.

Below are listed some highlights of the scientific results from the ESA Venus Express mission.

We use these data along with Magellan altimetry to map surface emissivity. At this wavelength atmospheric details are seen down to an altitude of 50 km. Copyright 2000 - 2020 © European Space Agency. The brightest area is from reflecting sunlight. The original launch was to have taken place on 26 October 2005 but was postponed due to contamination of the launch fairing, After launch the spacecraft went directly to a Venus transfer trajectory. The two views only differ in the colour scaling, to reveal different details. Many of these questions are of a multi-disciplinary nature and by combining the results from studies of several of the Themes above we hope to get answers to questions like the following: An improved general understanding and answers to these questions may put us in a better position to answer the perhaps most fundamental question of all: why Venus evolved so differently than Earth, in spite of the similarities at the beginning of the formation ?

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