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| * Analyser of Space Plasma and Energetic Atoms ('''ASPERA''') | | * Analyser of Space Plasma and Energetic Atoms ('''ASPERA''') |
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| Led by Institute of Space Physics, Kiruna, Sweden
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| ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.
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| * Venus Express Magnetometer ('''MAG''') | | * Venus Express Magnetometer ('''MAG''') |
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| Led by IWF, Graz, Austria
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| Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.
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| * Planetary Fourier Spectrometer ('''PFS''') | | * Planetary Fourier Spectrometer ('''PFS''') |
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| Led by IFSI-INAF, Rome, Italy
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| PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.
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| * Ultraviolet and Infrared Atmospheric Spectrometer ('''SPICAV/SOIR''') | | * Ultraviolet and Infrared Atmospheric Spectrometer ('''SPICAV/SOIR''') |
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| Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia
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| SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.
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| * Venus Radio Science Experiment ('''VeRa''') | | * Venus Radio Science Experiment ('''VeRa''') |
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| Led by Univ. der Bunderswehr, Munich, Germany
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| VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.
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| * Ultraviolet/Visible/Near-Infrared mapping spectrometer ('''VIRTIS''') | | * Ultraviolet/Visible/Near-Infrared mapping spectrometer ('''VIRTIS''') |
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| Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France
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| VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.
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| * Venus Monitoring Camera ('''VMC''') | | * Venus Monitoring Camera ('''VMC''') |
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| Led by MPS, Katlenburg-Lindau, Germany
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| VMC is a wide-angle multi-channel camera that will be able to take images of the planet in the near infrared, ultraviolet and visible wavelengths. VMC will be able to make global images and will study the cloud dynamics and image the surface. In addition it will assist in the identification of phenomena seen by other instruments.
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| <gallery>
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| [[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]
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| </gallery>
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| [[File:venusexpress.jpg|200px|thumb|center|Venus Express]]
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| [[Fichier:http://www.stp.isas.jaxa.jp/venus/images/gallery/PLANET-C2.jpg]]
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| === Akatsuki === | | === Akatsuki === |
Overview of the Page venus-atm
Goal of Earth-based observations in the VEx-VCO/Akatsuki context
- Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
- Obtain simultaneous measurements over several levels in Venus' upper atmosphere
- Obtain cross-validation of different measurement techniques
- Extended spatial (both hemispheres) and temporal scales
- Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation
Map
Googlemap:
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Instrumentation and Techniques
Explanation of the table, contenu et but
Link on the table:
Instrumentation and Techniques
Observations and Operation Planning
Link on the table:
Observations and Operation Planning
In-orbit observations
Venus Express
File:Venus Express in orbit.jpg⎮200px⎮thumb⎮left⎮ESA's Venus Express
Instruments
- Analyser of Space Plasma and Energetic Atoms (ASPERA)
- Venus Express Magnetometer (MAG)
- Planetary Fourier Spectrometer (PFS)
- Ultraviolet and Infrared Atmospheric Spectrometer (SPICAV/SOIR)
- Venus Radio Science Experiment (VeRa)
- Ultraviolet/Visible/Near-Infrared mapping spectrometer (VIRTIS)
- Venus Monitoring Camera (VMC)
Akatsuki
The Project
A short presentation of the project?
The project, a link to JAXA:
JAXA
The Instrument and Techniques
1.01um
cloud (day-night), surface (nightside)
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65um
SO2 - UV absorber (dayside)
10 um
cloud top (day/nightside)
777, 551, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)
More about the Akatsuki Instruments
