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V isible light I mager and M agnetograph T.Appourchaux on behalf of the VIM team IAS

V isible light I mager and M agnetograph T.Appourchaux on behalf of the VIM team IAS. Contents. Scientific objectives Instrument design Instrument challenges What now ?. Scientific objectives. Probe the Solar Dynamo: High-latitude fields, flows and seismic waves

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V isible light I mager and M agnetograph T.Appourchaux on behalf of the VIM team IAS

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  1. Visible light Imager and MagnetographT.Appourchaux on behalf of the VIM teamIAS

  2. Contents • Scientific objectives • Instrument design • Instrument challenges • What now ?

  3. Scientific objectives • Probe the Solar Dynamo: • High-latitude fields, flows and seismic waves • Explore at all latitudes: • Energetics, dynamics and fine-scale structure of the Sun’s magnetized atmosphere • Investigate links: • Between the solar surface, corona and inner heliosphere

  4. Stereoscopic helioseismology

  5. What are the observables? • High and low resolution imaging • Vector magnetic field • Solar radial velocities

  6. How can we do that? • High and low resolution imaging • Full Disk Telescope (FDT), Field of view >2.5 deg, 2.5 cm dia. • High Resolution Telescope (HRT), 150 km resolution at 0.22 AU (1”), Field of view >15, 16 cm dia; • Vector magnetic field • Stokes polarimetry in FeI 6173 Angström • Solar radial velocities • 5 to 6 positions on the line profile

  7. VIM: Subsystems • FDT: • Off-pointing mechanism: wedge prism (2.5 deg) • HRT: • Image Stabilization System (0.02” overs 10 s) • Filtergraph (passband of 75 mAngström) • Polarization modulation package (PMP based on Liquid Crystal Variable Retarder) • Camera: 2k x 2k Active Pixel Sensor • Electronic box

  8. The VIM team • Germany: • PI ship, management, HRT, Structure:MPS • Pointing: KIS • Spain: • FDT, PMP: INTA • E-box: IAA • Structural and thermal analysis: IDR • France: • Filtergraph: IAS

  9. Filtergraph concept • Telecentric • No velocity change • Passband shifted and widened • All defects imaged on the solar image • Aperture apodization • Baseline solution: Lithium Niobate Fabry-Pérot, 6 cm dia. • Back-up: Fabry-Pérot with piezoelectric spacers

  10. Tunability requirement(TN-VIM-2005-02 and 03)

  11. Response (TN-VIM-2005-01)

  12. Challenges • Space qual. of LCVR • Space qual. Of LiNb03 etalons • High solar flux 25 solar constant… • Reduced telemetry: 20 kbits/s

  13. What now ? • Call for Letter of Intent (ESA, 11 July 06) • MPS response as of 15 September 06 • Heat Shield study till end 2007 • AO hopefully in 2008 • Launch in 2017 • Observation till 2023-2028…

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