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New MSDP improvements Advances and prospects

New MSDP improvements Advances and prospects. New CCD cameras Linear polarization of prominences New line 6103 CaI and B vector High resolution and 3D flux tubes. THEMIS. German VTT. - High speed DALSA cameras. Pic du Midi LJR, Meudon Tower. - JOP 178.

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New MSDP improvements Advances and prospects

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  1. New MSDP improvements Advances and prospects • New CCD cameras • Linear polarization of prominences • New line 6103 CaI and B vector • High resolution and 3D flux tubes THEMIS German VTT - High speed DALSA cameras Pic du Midi LJR, Meudon Tower - JOP 178 P. Mein, MSDP workshop, Tarbes 2006

  2. THEMIS/MSDP 2005 • 2 New CCD cameras 1024x1075 • 2 lines, pixel ~ 0.2 arcsec • Polarization analysis with 5 steps of grid 170 arcsec Sep 13, 2005 NaD1 Intensity +/-240 mA 167 ’’ NaD1 Stokes V +/-240 mA

  3. Ha Intensity Line centre Intensity +/- 410 mA Velocity +/- 410 mA Stokes V +/- 410 mA

  4. THEMIS/MSDP Q,U profiles Ha prominences Observ. P. & N. Mein (July 2004)

  5. D3 prominences

  6. THEMIS / MSDPI, Q,U,V profiles Polarization analysis of 6103 CaI V / I -80/+80 mA Q / I 0 / +80 mA U / I 0 / +80 mA Obs. K. Tziotziou

  7. Stokes profiles at a peculiar point (cross)

  8. B vector Unno-fit inversion (points where Filling factor > 0.07) (V. Bommier)

  9. Prospects The first MSDP observations of 6103 show that we can expect to measure B vector in the photosphere - either from standard processing and Stokes profiles inversion - or by direct inversion using c-files (to avoid profile interpolations) The 2005 observations have been - performed with the 16 channels optics (wavelength step 80 mA), - processed with standard processing using various corrections improving the effective spectral resolution (curvatures interpolated between different y-positions, smoothing around 1 arcsec). Measurements with the new optics which should be adjusted in the near future (14 channels, wavelegth step 50 mA) - would still increase the wavelength resolution - would allow to observe also 6302.

  10. Prospects:High Spatial ResolutionwithTHEMIS/MSDP LOS Magnetic Field NaD1 +/- 320 mA NaD1 +/- 80mA 15 arcsec Obs. J-M Malherbe, May 2000

  11. 8 pm 32 pm THEMIS/MSDP, J-M Malherbe, 2000 - Larger size of facular magnetic structures at high levels - 3D flux-tube models in progress

  12. VTT / MSDPFast DALSA cameras 15 m spectrograph large X-steps 10’’ fast scans 3’ x 3’ expected < 20 sec Ha line centre Sep 17, 2005 490 x 150 arcsec

  13. Ha Intensity +/- 440 mA Ha velocity +/- 440 mA

  14. JOP 178 / 2005 Campaign http://bass2000.bagn.obs-mip.fr/jop178/index.html Th. Roudier (P.I.) (1) , S. Rondi (1) , J.M. Malherbe (2) , P. Mein (2) , B. Schmieder (2), V.Bommier (2) , N. Mein (2) , J. Moity (2), Ch. Coutard (2) G. Molodij (2), N. Meunier (1), M. Rieutord (1), R. Tkaczuk (1), G. Aulanier (2), Berlicki (2) , E. Pariat (2) , K. Bocchialini (3), G. Pouget (3) , J. Solomon (3), P. Suetterlin (4), M. Svanda (5), Tziotziou (4), Steve Keil (6) , K.S. Balasubramaiam (6), Y. Deng (7) , J Staiger (8), P. Rudawy (9) D. Pallamraju (10), R. Kitai (10), M. Svanda (11) Presented by Pr. K. SHIBATA (Hida and Kwasan observatories ,Japan) (1) Observatoire Midi Pyrénées. (2) Observatoire de Paris, Meudon, France A. (3) Institut d'Astrophysique Spatiale France (4) Universiteit Utrecht, Utrecht, Netherlands (5) Astronomical Institute Ondrejov Czech Republic K and the Global High Resolution H-alpha Network (6) Sacramento Peak Observatory (USA) (7) Yuanyong Huairou Solar Observing Station (China) (8) KIS-Freiburg- VTT (Germany) (9) Wroclaw Observatory (10) Hida and Kwasan observatories (Japan) (11)Astronomical Institute Ondrejov Czech Republic JOP 178

  15. September 11, 2005 : NOAA808 (40 degrees East, 10 degrees South) THEMIS/MSDP: simultaneaous observation at 12:00 UT   Field of view 360 arcsec by 160 arcsec CATANIA Observatory Target Intensity D1 a 24 nm to line center Stokes V in D1 at 24 nm to line center Intensity Halpha at 25 nm  to line center Intensity Halpha at 50 nm  to line center THEMIS/MTR: 14h44-17h59 UT Magnetic field compound of both: H_aplha and magnetic field map the magnetic field vector is given in line-of-sight coordinates:- color scale for the longitudinal magnetic field- yellow dashes (without arrow: the ambiguity is not solved) for thetransverse magnetic field JOP 178

  16. September 15 , 2005 Pic du Midi ( MSDP / LJR) NOAA808, eruption 8h 53mn 52 s UT H_aplha compound H_aplha and Doppler velocity (Blue =up, red= down) White Light JOP 178

  17. September 11, 2005 NOAA808, eruption 8h 40mn 36.47 s UT Meudon Observatory: MSDP NOAA808, 8h40mn 36.47 s UT H-alpha 656nm Doppler Velocity and H-alpha intensity (Blue =up, red= down) JOP 178

  18. THEMIS / MSDP prospects • Fast CCD cameras + large FOV ( grid 170’’) + Polar analysis: • Time evolutions (oscillations, ejections,…) • Linear polarization of flares • Large FOV for coordinated campaigns • High spatial resolution(tilt, astigmatism?) • 3D structures of flux tubes • B vector in the photosphere • Fast measurements of B vector (6103) • Expected higher spectral resolution • (14 channels, 6103, 6302)

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