JOP 178 / 2005 Campaign http://bass2000.bagn.obs-mip.fr/jop178/index.html Slide 1 : List of the JOP 178 members and their institutes Slide 2: I just wrote 2 objectives but our program has four goals. 1) Scientific objective Four goals should be achieved with this program. 1. The first objective is to study at the same time the photospheric and chromospheric motions around filaments. Filaments are one of the most observed features on the Sun. They are located in the upper solar atmosphere and are submitted to the effects of the lower layer, the photosphere. On basis of detailed observations, it is widely believed that the medium which transfers perturbations into the corona through the filament is a magnetic field. Since the interaction between photospheric motions and magnetic fields extending into the corona plays an important role in the dynamics of filaments, it is natural to investigate how material moves under the filament and how coronal magnetic fields evolve when a particular kind of photospheric motion is imposed at their footpoints. The aim of the program is to detect the torsion and shearing motions around the footpoints of the filaments. Such measurements are possible (Roudier et al 1999, Rieutord et al. 2001) and will be done in the areas corresponding to the footpoints where magnetic parasitic polaritic are frequently observed (Aulanier et al 1998, Martin etal 1996) 2. The second objective is to understand the environment of the filament inside the corona. Recent observations (Heinzel et al 2001, Schmieder et al 2002, 2004) show that cool material could exist below or around filaments and be not visible in Halpha because of low optical thickness but be visible as dark absorbing features in the transition region and coronal lines. The mass of filament could be twice as much as what is commonly believed. Filament eruptions are associated with some Coronal mass ejections (CMEs). Therefore the mass loading of a filament should be estimated with some accuracy. Target a filament , not too far from the equator, on the East side of the Sun at the beginning of the campaign. A filament in a region of low-medium magnetic field (100 to 400 G) 3. The third objective is to follow the passage of a filament from the disk to the limb where it becomes a prominence. On the disk, the photospheric underlying magnetic field would be obtained as usual by interpretation of the Zeeman effect, and on the limb the prominence field would be obtained by interpretation of the Ha Aulanier G., and Demoulin P., "3D magnetic configurations supporting prominences Aulanier G. and Schmieder B., "The magnetic nature of wide EUV filament channels Bommier, V., Rayrole J., and Eff-Darwich, A., "Vector magnetic field map at the photospheric level below and around a solar filament (neutral line)", 2005, A&A (Heinzel P., Schmieder B. and Tziotziou K, "Why are solar EUV filaments more extended ?Heinzel P., Anzer U. and Schmieder B., "A spectroscopic model of EUV filaments", Schmieder B., Tziotziou K., Heinzel P., "Spectroscopic diagnostics of an H_alpha Schwartz P., Heinzel P., Anzer U., and Schmieder B., "Determination of the 3D top Target:d by SOHO and VTT/MSDP", 2004, A&A 421, 323 A filament located near the central meridian at the beginning of the campaign, in a region of low-medium magnetic field (100 to 400 G). A vector magnetic field filters images interleaved about 30 s cadence, strictly regular cadence, Dopplergrams, magnetograms and Igrams in 1me filament channel. 4) Fourth objective : oscillations in Filaments and Prominences Purpose: To find long period oscillations in filaments and prominences, and to derive a diagnostic of these structures. Method: From the identification of the MHD modes derived from the observations, Joarder and Roberts (1993) model leads to 3 equations linking these modes with the alfven velocity, the temperature and the angle (between the filament and the magnetic field lines supporting the filament). Long time observations (>15h) with a high temporal resolution (less than 30s) are needed to detect -if they exist- all the periods (up to 5 or 6 hours) useful to derive these 3 parameters. We plan to observe filaments near the central meridian with CDS in He I (584 angstrom), Mg X (625 angstrom) and O V (629 angstrom), in a "sit and stare" slit configuration ; the solar rotation will be compensated (see the CDS study POUGET_3). When those filaments reach the limb, we plan to observe them as prominences with CDS and SUMER. EIT (He II at 304 A, in CME watch mode) will give the context of the observed region. THEMIS observations of the magnetic field around the filament will help in the determination of the angle mentioned above and in the determination of the distance between the opposite polarities which is also an important parameter of the model. 2) list of the Participating instruments: Slide 3 : map showing the location of the observatories participating to our campaign. We can note a nice longitude coverage. slides 4 -5 - 6 - 7: example of coordinate observations on 11 Sept. 2005. details and full sun simultaneous observations. slides 8 - 9 - 10 : second example of coordinate observations on 13 Sept. 2005. details and full sun simultaneous observations. slides 11- 12 : third example of coordinate observations on 15 Sept. 2005. details and full sun simultaneous observations. The eruption start 8h30 UT, peak at 8h38 UT, stop at 8h46 UT, class X1.1. Slide 11 shows the intensity and the doppler component during the eruption. The raw treatment of the data does not allow to give now a good precision for the Doppler velocity (only difference between red and blue part of the line) in the eruption part. More detailled reduction is needed. Slide 13 : example of Halpha movie with high spatial resolution obtained at * Sac Peak DST (USA). The duration of the movie is 1h23mn (the time step is around 10 sec). Slide 14 : more data to give an idea of some details that are observed. For example at the DOT the observation is done in 5 points of the H-alpha line. The cadence is around 30 secondes. Slide 15 : Gives an overview of the JOP 178 campaign 2004 (last year). High spatial resolution and magnetic field measurements and full Sun context. Slide 16 : example of a filament for which we measure photospheric magnetic field, Doppler velocities and horizontal flows. slide 17 : example of a movie in H-alpha with high spatial resolution at the DOT. The duration of the movie is 50 min (the time step is around 30 sec). slide 18 : example of the horizontal photospheric flow field measured in white light of the preceding movie. we observe during all the sequence (and also one hour before and after) a diverging flow between the feet of filament. That divergent field correspond to a family of granules which are visible in the movie (granule are in blue) which represents x,y and t. slide 18 : example of determination of the horizontal photospheric flow field with TRACE data (White Light) overlaped on ISOON large field of view observation. This shows our capabilities to overlap exactly both observation for the long time sequence.