1 / 14

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

varsha
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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…

More Related