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'''Page venus-atm'''
'''Overview of the Page venus-atm'''


Goal of Earth-based observations in the VEx-VCO/Akatsuki context  
Goal of Earth-based observations in the VEx-VCO/Akatsuki context  


* Perform direct measurements not feasible by an orbiter
* Perform direct measurements not feasible by an orbiter e.g. provide direct absolute wind measurements
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Obtain cross-validation of different measurement techniques
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__TOC__
__TOC__


==Map of the groundbased observations==
==Map==
Groundbased observations


Link on google map
* http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2


http://www.evanmiller.org/maps/GoogleMaps-0.9.4.zip
 
Googlemap:
* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign]
 


$wgGoogleMapsKey = "ABQIAAAAlPAF_RpXQsb-9OA4bmfhuBROdUV6dnkNQ2wycpqjH1x_Q4S5MRRZCrmYQpMvvMzZ3_8K13uVJi0KhQ";
$wgGoogleMapsKey = "ABQIAAAAlPAF_RpXQsb-9OA4bmfhuBROdUV6dnkNQ2wycpqjH1x_Q4S5MRRZCrmYQpMvvMzZ3_8K13uVJi0KhQ";
require_once( "$IP/extensions/GoogleMaps/GoogleMaps.php" );
require_once( "$IP/extensions/GoogleMaps/GoogleMaps.php" );
<googlemap><iframe width="425" height="350" frameborder="0" scrolling="no" marginheight="0" marginwidth="0" src="http://maps.google.com/maps/ms?ie=UTF8&amp;hl=fr&amp;msa=0&amp;msid=106784557914957315781.000481c7cd8ab690441fc&amp;ll=-3.162456,11.601563&amp;spn=104.451773,149.414063&amp;z=2&amp;output=embed"></iframe><br /><small>Afficher <a href="http://maps.google.com/maps/ms?ie=UTF8&amp;hl=fr&amp;msa=0&amp;msid=106784557914957315781.000481c7cd8ab690441fc&amp;ll=-3.162456,11.601563&amp;spn=104.451773,149.414063&amp;z=2&amp;source=embed" style="color:#0000FF;text-align:left">2010 Venus Coordinated Campaign</a> sur une carte plus grande</small><googlemap/>


==Instrumentation and Techniques==
==Instrumentation and Techniques==
Explanation of the table, contenu et but
Explanation of the table, contenu et but


Link on the table
Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr]
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr Instrumentation and Techniques]


==Observations and Operation Planning==
==Observations and Operation Planning==


Link on the table
Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr]
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr Observations and Operation Planning]


== In-orbit observations ==


== Celest observations ==


=== Venus Express ===


=== Venus Express ===


==== Instruments ====
==== Instruments ====
* Analyser of Space Plasma and Energetic Atoms ('''ASPERA''')
* ASPERA : Analyser of Space Plasma and Energetic Atoms
   
   
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''')
* MAG : Venus Express Magnetometer  
   
   
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.
* SPICAV/SOIR : Ultraviolet and Infrared Atmospheric Spectrometer  
 
* 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.
* VeRa : Venus Radio Science Experiment
 
* 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.
* VIRTIS : Ultraviolet/Visible/Near-Infrared mapping spectrometer
 
* 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.
* VMC : Venus Monitoring Camera


* Ultraviolet/Visible/Near-Infrared mapping spectrometer ('''VIRTIS''')
=== Akatsuki ===
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.
==== The Project====


* Venus Monitoring Camera ('''VMC''')
A short presentation of the project?
The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.
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.  
extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html


The project, a link to JAXA:
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]


<gallery>
==== The Instrument and Techniques ====


[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]
* IR1
1.01um
cloud (day-night), surface (nightside)


</gallery>
* IR2
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65um


[[File:venusexpress.jpg|200px|thumb|center|Venus Express]]
* UVI 283, 365 nm
SO2 - UV absorber (dayside)


=== Akatsuki ===
* LIR
10 um
cloud top (day/nightside)


==== The Project====
* LAC
777, 551, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)


The project, a link to JAXA:
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html]
==== The Instrument and Techniques ====


Lancement
[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]
Projets

Latest revision as of 16:26, 10 May 2010

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:


$wgGoogleMapsKey = "ABQIAAAAlPAF_RpXQsb-9OA4bmfhuBROdUV6dnkNQ2wycpqjH1x_Q4S5MRRZCrmYQpMvvMzZ3_8K13uVJi0KhQ"; require_once( "$IP/extensions/GoogleMaps/GoogleMaps.php" );

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

Instruments

  • ASPERA : Analyser of Space Plasma and Energetic Atoms


  • MAG : Venus Express Magnetometer


  • SPICAV/SOIR : Ultraviolet and Infrared Atmospheric Spectrometer


  • VeRa : Venus Radio Science Experiment


  • VIRTIS : Ultraviolet/Visible/Near-Infrared mapping spectrometer


  • VMC : Venus Monitoring Camera

Akatsuki

The Project

A short presentation of the project? The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

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)


More about the Akatsuki Instruments

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