New MSDP improvements

Advances and prospects

P. Mein, MSDP workshop, Tarbes 2006

THEMIS - New CCD cameras

- Linear polarization of prominences

- New line 6103 CaI and B vector

- High resolution and 3D flux tubes

German VTT - High speed DALSA cameras

Pic du Midi LJR, Meudon Tower

- JOP 178

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

NaD1

Stokes V

+/-240 mA

167 ’’

H Intensity

Line centre

Intensity

+/- 410 mA

Velocity

+/- 410 mA

Stokes V

+/- 410 mA

H prominences

Observ. P. & N. Mein (July 2004)

THEMIS/MSDP Q,U profiles

D3 prominences

THEMIS / MSDP I, 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

Stokes profiles at a peculiar point (cross)

B vector

Unno-fit inversion

(points where Filling factor > 0.07)

(V. Bommier)

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.

Prospects

NaD1 +/- 320 mA NaD1 +/- 80mA

15 arcsec

LOS Magnetic Field

Prospects: High Spatial Resolution with THEMIS/MSDP

Obs. J-M Malherbe, May 2000

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

VTT / MSDP Fast DALSA cameras

15 m spectrograph large X-steps 10’’ fast scans

3’ x 3’ expected < 20 sec

H line centre Sep 17, 2005 490 x 150 arcsec

H Intensity +/- 440 mA

H velocity +/- 440 mA

JOP 178

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

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

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

JOP 178

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

CATANIA Observatory

September 15 , 2005

JOP 178

Pic du Midi ( MSDP / LJR)

H_aplha compound H_aplha and Doppler velocity

(Blue =up, red= down)

NOAA808, eruption 8h 53mn 52 s UT

White Light

September 11, 2005 NOAA808, eruption 8h 40mn 36.47 s UT

Meudon Observatory: MSDP

JOP 178

Doppler Velocity and H-alpha intensity

(Blue =up, red= down)

H-alpha 656nm

NOAA808, 8h40mn 36.47 s UT

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)