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What can we learn from the vector magnetic field measured in filament channels ?

What can we learn from the vector magnetic field measured in filament channels ?. B. Schmieder, G. Aulanier,. Arturo López Ariste. Introduction. THEMIS Observations: Magnetic field vector. Chirality and resolution of the 180° ambiguity. SST La Palma. Lin , Wiik, Engvold (2004, 2005)

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What can we learn from the vector magnetic field measured in filament channels ?

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  1. What can we learn from the vector magnetic field measured in filament channels ? B. Schmieder, G. Aulanier, Arturo López Ariste Introduction • THEMIS Observations: • Magnetic field vector Chirality and resolution of the 180° ambiguity The 6th Solar-B Science meeting Kyoto Nov 8 2005

  2. SST La Palma Lin , Wiik, Engvold (2004, 2005) 60% of ends are rooted in network boundaries Barbs and feet are related to Minority magnetic polarities (Martin 1994) How is oriented the field vector? Is it horizontal (Chae et al 2005) or vertical (Lin et al 2005) ? The 6th Solar-B Science meeting Kyoto Nov 8 2005

  3. Presence of minority polarities in filament channels Simulation of the observations of cool plasma visible in multi-l(Aulanier and Démoulin 1998, van Ballegooijen 2004, Régnier and Amari 2004) Computations of the dips in each field line in the computation model box (B . s) B > 0 h altitude (z) Bz = 0 ligne de champ dHa = Hg = 300 km Dips filled by plasma The 6th Solar-B Science meeting Kyoto Nov 8 2005

  4. Extrapolation of B from SoHO/MDI 3D magneto-hydrostatic linear model with free parameters constrained by the theory and the observations Lignes de champ filament arcades coronales Matière froide z > 4 Mm z < 4 Mm CDS OV THEMIS 08:12 UT 07:52 UT Topology of B and distribution of the cool matter Aulanier G., Schmieder B., 2002, A&A, 386, 1106-1122 The 6th Solar-B Science meeting Kyoto Nov 8 2005

  5. Modeled dips Adapted from Aulanier et al. (1999) – i + barb Ha filament Dips viewed in 3D Bz(z=0) & Magnetic dips Bt (z=0) The 6th Solar-B Science meeting Kyoto Nov 8 2005

  6. JOP 178 International campaign 16 October 2004 THEMIS The 6th Solar-B Science meeting Kyoto Nov 8 2005

  7. THEMIS Observations in the Multi lines mode 1. Simulaneously observations of the polarized profiles of Fe I doublet 6301-6302 A, Na I, Ha with beam exchange technique 2 . Data processing (flat field, dark current) SQUV 3. Inversion code for the Fe I doublet with a PCA-based algorithm in a Milne-Eddington atmosphere using a grid of models B, Inc., Azi. with error bars in the LOS ref. frame 4. Change of the system of reference to local frame 5. The 180 ° ambiguity is not resolved, two solutions for incl. and azi. Criterion used for resolving the ambiguity : the chirality rules for filaments The 6th Solar-B Science meeting Kyoto Nov 8 2005

  8. SINISTRAL CASE DEXTRAL CASE According to the directions of the fine structuresand thefeet (Halpha) Filament The 6th Solar-B Science meeting Kyoto Nov 8 2005

  9. I(Ha) B Sinistral filament B (Fe I) The 6th Solar-B Science meeting Kyoto Nov 8 2005

  10. B horizontal mean direction if the chirality is sinistral SINISTRAL CASE – + Filament axis Photospheric inversion line (Bz) The 6th Solar-B Science meeting Kyoto Nov 8 2005

  11. B horizontal mean direction if the chirality is dextral DEXTRAL CASE – + Filament axis Photospheric inversion line (Bz) The 6th Solar-B Science meeting Kyoto Nov 8 2005

  12. #4 #3 #1 #2 #5 #6 The 6th Solar-B Science meeting Kyoto Nov 8 2005

  13. #4 #3 #1 #2 #5 #6 The 6th Solar-B Science meeting Kyoto Nov 8 2005

  14. -8.8 Mx/cm2 114.7 Mx/cm2 The 6th Solar-B Science meeting Kyoto Nov 8 2005

  15. Inversion errors (case #1) The 6th Solar-B Science meeting Kyoto Nov 8 2005

  16. – l + Case #1 3D The 6th Solar-B Science meeting Kyoto Nov 8 2005

  17. Case #1 3D view Case 2 Case 4 In the filament channel : horizontal dip The 6th Solar-B Science meeting Kyoto Nov 8 2005 Case 5

  18. Lopez Ariste, Aulanier, Schmieder , Sainz A &A 2006 – l + barb Ha filament Bz & Bt (z=0) Dip viewed in 3D The 6th Solar-B Science meeting Kyoto Nov 8 2005

  19. Conclusion THEMIS/MTR observes simultaneously in multi lines: Ha, Fe 6302 and 6301, Na D1 High sensitivity of the magnetic flux: -10 Mx/cm2 Magnetic field vector tangential to the photosphere Photospheric dips = « bald patches » observed in filament channels consistent with model of Aulanier & Démoulin (1998) Needs more cases : SOLAR-B The 6th Solar-B Science meeting Kyoto Nov 8 2005

  20. Observational evidence of photospheric magnetic dips in filament channels B. Schmieder, G. Aulanier, Arturo López Ariste Magnetic loops filament flux tube overlaying arcades Magnetic dips z > 4 Mm z < 4 Mm The 6th Solar-B Science meeting Kyoto Nov 8 2005 Adapted from Aulanier & Schmieder (2002)

  21. EUV filament A Dark, bright threads or no existing Emission in hot lines C A B B C OV 105 K Long extensions The 6th Solar-B Science meeting Kyoto Nov 8 2005

  22. Case # 6 The 6th Solar-B Science meeting Kyoto Nov 8 2005

  23. Conclusion THEMIS/MTR observes simultaneously in multi lines: Ha, Fe 6302 and 6301, Na D1 THEMIS/MSDP Ha and Na D1 High sensitivity of the magnetic flux: -10 Mx/cm2 1. Magnetic field vector tangential to the photosphere Photospheric dips = « bald patches » observed in filament channels consistent with the model of Aulanier & Démoulin (1998) Emerging and cancellation of magnetic flux Filament disappearance and formation 2. The 6th Solar-B Science meeting Kyoto Nov 8 2005

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