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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 of the groundbased observations
Groundbased observations
Googlemap:
http://www.evanmiller.org/maps/GoogleMaps-0.9.4.zip
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<googlemap><iframe width="425" height="350" frameborder="0" scrolling="no" marginheight="0" marginwidth="0" src="http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-3.162456,11.601563&spn=104.451773,149.414063&z=2&output=embed"></iframe>
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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
Celest observations
Venus Express
Instruments
- Analyser of Space Plasma and Energetic Atoms (ASPERA)
Led by Institute of Space Physics, Kiruna, Sweden
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.
- Venus Express Magnetometer (MAG)
Led by IWF, Graz, Austria
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.
- Planetary Fourier Spectrometer (PFS)
Led by IFSI-INAF, Rome, Italy
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.
- Ultraviolet and Infrared Atmospheric Spectrometer (SPICAV/SOIR)
Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia
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.
- Venus Radio Science Experiment (VeRa)
Led by Univ. der Bunderswehr, Munich, Germany
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.
- Ultraviolet/Visible/Near-Infrared mapping spectrometer (VIRTIS)
Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France
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.
- Venus Monitoring Camera (VMC)
Led by MPS, Katlenburg-Lindau, Germany
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.
Akatsuki
The Project
A short presentation of the project?
The project, a link to JAXA: JAXA
The Instrument and Techniques
- IR1
1.01um cloud (day-night), surface (nightside)
- IR2
1.73, 2.26, 2.32 (near-IR) 2.02 (CO2), 1.65um
- UVI 283, 365 nm
SO2 - UV absorber (dayside)
- LIR
10 um cloud top (day/nightside)
- LAC
777, 551, 553, 558, 630 nm O2/O airglow (night) lightning (night)
