JOP149 Onset on flaring activity and Coronal mass ejections between space and ground based instruments in Europe (Poland, Ondrejov, Canaries....). Received: September 7, 2001 List of applicants: B.Schmieder, Mein P., Malherbe J.M., Vilmer N., van Driel L., Mein N. Tziotziou K. (Observatoire de Paris), Vial J.-C. ( IAS Orsay) J.Staiger (KIS), Heinzel P. (Ondrejov CS), Kucera T. and Poland A.(GSFC), DeLuca E., and Golub L. (Harvard-Smithonian Center for Astrophysics) Rompolt B., Rudawy P. ( Wroclaw , Poland). For the ground based instruments we have 2 windows of possible supports : October : 3-10 included - VTT at Tenerife Time allocation 3-10 Oct (8-18 UT) H-alpha and Ca 8542 observation with the MSDP: profiles, intensities and velocities October 18-23 (during the MEDOC campaign) this jop or the JOP 131: Spectro-polarimetric diagnostics of prominences and filaments - THEMIS Time allocation 18-23 Oct (8-18 UT) . Halpha 6563, . Ca II 8542 line with the MSDP: profiles, intensities and velocities. The choice of this line is suggested by previous results: Yuan Yong Deng et al. A&A,1999, 349, 927, P.Mein et al A&A 2000, 555,1146, . Magnetic field in Na D1 . slit jaw (Halpha) filter -CDS Bright regions in the TR lines correspond often to network, locations where the magnetic field in enhanced. We would like to check the destabilization of filaments at their footpoints due either to EMF or flux cancellation. We expect to see new bright regions close to the footpoints or moving bright features. He and OV lines would be useful to align all the observations. For all these purpose we want to use the studies: EFINAR1 EFINAR2 FILOBS1 - SUMER - 3-10 October No observation with SUMER in this JOP: AR would be on the disk, not on the SUMER slit at x=-980 17-23 October JOP 131 " spectro polarimetric diagnostics of fil/prominences" if opportunity - EIT - -1- CME watch with your possible cadence (17 mn) will be the basis-program for our two programs. Occasionally, if the target needs it, we shall ask the possibility to run: either : -2- Active region program ( full resolution, 1/4 Sun ) at 195 A for 2 to 4 hours (with the highest cadence as possible). or -3- Filament eruption program at 304 A, also full resolution, also for 2 to 4 hours (with the highest cadence as possible) We shall ask only one of these two items ( item 2 or item 3) by day. - MDI - . One large full disc magnetic map each 96 mn will be sufficient. This will be a good extension to the THEMIS observations, permitting magnetic fields extrapolations. THEMIS providing fast observation and MDI large field of view Observations are required between 8 and 18 UT. The target and precise schedule will be given daily. - TRACE - - Program 1 The coronal loops are good diagnostics to derive the magnetic field lines and to study the interaction of emerging and pre-existing magnetic fields. With MDI and THEMIS we would have data of photospheric magnetic fields. Magnetic extrapolation allows to understand where the energy can be released. Separatrices and bald patches (Demoulin et al.) would be computed and compared with the bright regions. - Program 2. We would like to continue our program on the absorption of coronal lines by H and He continua. We would derive the hydrogen column density of the cold plasma related to the destabilization of filaments. Halpha and CaII lines giving more informations on electron density and temperature For these two programs, we would like to observe 171, 195 A lines and white light during our observing times ( 8 - 18 UT). - Yohkoh SXT As we expect flares, soft X-ray images of the AR, are required as frequently as possible. -if HESSI is operating we will be happy to collaborate Scientific motivation of the program: Onsets of Flaring Activity and Coronal Mass Ejections. 1.Introduction: Recent observations have shown that the ejection of plasma from the Sun, called coronal mass ejection (CME) is the major cause of interplanetary shocks and geomagnetic storms. Although a number of studies give insight, until now, the physical mechanism which causes CME initiation is unclear. Multi wavelength studies are required to determine what causes the CME. We would like to be able to detect the magnetic origin, the dynamics of the plasma at different temperatures. We expect that a campaign involving ground based instruments ( in particular Canaries telescopes: THEMIS,VTT) and space instruments (SOHO,TRACE, HESSI,Yohkoh) would provide information on the causes of CMEs: new emerging flux at the solar surface dynamics of the phenomena (filament eruption, ejection) reconnection and flaring process 2. Aim Earlier it was suggested that a CME was initiated by the impulsive expulsion of the overlying corona due to the energy released from the associated flare. However this suggestion was not supported by observations. Many CMEs are not accompagnied by flares. Furthermore, it was pointed out that CMEs are found to precede or at best to start at about the same time, as the associated flare. The recently added capability of SOHO/Yohkoh and TRACE observations significantly improved our ability to determine the relative times of flares and CMEs. Only half or less than half of CMEs are directly related to flares in active region. Some filament eruptions are precursors of CMEs but no statistics are really convincing. On the 31 may 1997, in the frame of a SOHO (SUMER, CDS, EIT, LASCO, MDI) JoP 17 coordinated with the MSDP at Pic du Midi, we could observe a disappearing filament in H$\alpha$ and related its disappearence to large velocities observed in Lyman lines and to a CME observed by LASCO. (Schmieder et al. 2000 A et A, 358, 728). The H$\alpha$ observations stopped too early (because of clouds), SUMER and EIT started too late, thus we could not really have a good timing of the event. We would like to obtain new observations of CMEs and related active phenomena in the low atmosphere. Observations of the magnetic field in the photosphere, the Dopplershifts in the chromosphere, in the corona, and images of CMEs are suitable. 3. Data set needs We propose a coordinated campaign involving ground based instruments as well as space instruments. On the ground THEMIS will provide the magnetic field vector at different altitudes in the solar atmosphere, VTT/MSDP the dynamics of the chromosphere, in space SOHO/SUMER CDS, EIt will give information on the transition region and coronal plasma. TRACE will give a 3D view of coronal loops, HESSI the X rays coming from the flaring regions. Multiwavelength campaign in coordination with satellites :\\ SOHO ( Vial J.-C., Kucera T, Poland A.\\ TRACE ( De Luca E., Golub L.)\\ Yohkoh \\ HESSI (Vilmer N.) \\ and ground-based observatories:\\ VTT - MSDP (Schmieder B., Mein P.) Bidimensional spectroscopy in Halpha line. Sequences with good time resolution for active phenomena, reconnections, mass ejections, instabilities connected with CMEs...\\ THEMIS - (Mein P.) MSDP mode : 4 lines with good time resolution and polarization analysis to get the stratification of the magnetic field and the chromospheric dynamics.\\ Ondrejov - ( Heinzel P.) Spectroscopy in Balmer lines. Nan\c{c}ay - ( Vilmer N.) radio-heliograph observations Wroclaw - (Rompolt B.) filtergrams and bidimensional spectroscopy in chromospheric lines\\ 4. Project management plan The campaign coordinator will distribute the target of the observations to all the observatories from China, Europe and US which are interested to follow the campaign. 5. Results of previous campaigns. The results obtained with previous international campaigns are published in teh reference list. They concern: the 3D magnetic configuration of prominence, and active regions the signatures of emerging flux in the chromosphere and corona, the formation of sunspots fibrils, diagnostics of densities of cool structures. \\ van Driel,L, Schmieder B., Gauzzi G., Mein N., Hofmann A., Nitta N.,\\ Kurokawa H., Mein P. and Staiger J.:\\ X Ray Bright Point Flares due to Magnetic Reconnection\\ 1996, {\it Sol. Phys.}, 163, 145.\\ Mein P., Mein N., Malherbe J-M., Heinzel P., Kneer F., Von Uexk\"ull M. and Staiger J.\\ Flare multi-line 2D-spectroscopy\\ 1997, {\it Sol. Phys.}, 172, 161.\\ Aulanier G. and D\'emoulin P.\\ 3-D magnetic configurations supporting prominences. I The natural presence of lateral feet\\ 1998, {\it Astron. Astrophys.}, 329, 1125.\\ Aulanier G., D\'emoulin P., van Driel-Gesztelyi L., Mein P.,De Forest C.\\ 3-D magnetic configurationss supporting prominences. II The lateral feet as a pertubation of a twisted flux-tube\\ 1998, {\it Astron. Astrophys.}, 335, 309.\\ Malherbe J.M., Schmieder B., Mein P., Mein N., van Driel-Gesztelyi L. and von Uexk\"ull M.\\ Arch Filament systems associated with X-ray loops\\ 1998, {\it Sol. Phys.}, 180, 265.\\ Aulanier G., D\'emoulin P., Mein N., Van Driel-Gesztelyi L., Mein P. and Schmieder B. \\ 3-D Magnetic Configurations Supporting Prominences: III - Evolution of fine structures observed in a filament channel\\ 1999, {\it Astron. Astrophys.}, 342, 867.\\ Heinzel P., Mein N. and Mein P.\\ Cloud model with variable source function for solar Halpha structures II - Dynamical models\\ 1999, {\it Astron. Astrophys.}, 346, 322.\\ Rudawy P., Van Driel-Gesztelyi L., Cader-Sroka, Mein P., Mein N., Schmieder B., Malherbe J-M. and Rompolt B.\\ Analysis of evolution of NOAA7912 active region on 19 October 1995\\ 1999, {\it Astron. Astrophys. Suppl.}, 139, 89.\\ Kucera T.A., Aulanier G., Schmieder B., Mein N. and Vial J-C.\\ Filament channel structures in a SiIV line related to a 3D magnetic model\\ 1999, {\it Sol. Phys.}, 186, 259.\\ Tziotziou K., Heinzel P., Mein P. and Mein N.\\ Non-LTE inversion of chromospheric CaII cloud-like features\\ 2001, {\it Astron. Astrophys.},366, 686.\\ Mein N., Schmieder B., DeLuca E., Heinzel P., Mein P., Malherbe J-M. and Staiger J.\\ A study of hydrogen density in emerging flux loops from a coordinated TRACE and Canary Islands observation campaign\\ 2000, {\it ApJ}, 556, 438