Received: 14 September 2000 JOP 131 Dynamics of Active Regions. Two programs are proposed: 1) Flare activity of young and decaying ARs, interaction between the new and pre-existing magnetic fields. 2) Destabilization of filaments leading to two-ribbon flares and CMEs Magnetic field evolution and reconnection process will be investigated before and during flares. The energy release leading to chromospheric motions and heating of coronal loops will be estimated. The multi-wavelength campaign should be very promising in this respect. The speed of MSDP allows imaging spectroscopy of fast chromospheric motions. - VTT at Tenerife Time allocation 6 -15 Oct (8-18 UT) H-alpha observation with the MSDP: profiles, intensities and velocities - THEMIS Time allocation 9 - 15 Oct (8-18 UT) . Ca II 8542 line with the MSDP: profiles, intensities and velocities. The choice of this line is suggested by previous results: Yuan Yong Dend et al. A&A,1999, 349, 927, P.Mein et al A&A 2000, 355,1146, . Magnetic field in the Na D1 line. - CDS - Program 1: Determination of densities and abundances of some atoms. Young and Masson (1997, SP175) found an anomalous abundance ratio of Mg/Ne in the corona explained by emerging flux. More recently Fletcher et al. detected in CDS brightenings photospheric abundances and explained it using magnetic extrapolations. We want to continue this study and also to determine temperatures in bright regions for approaching heating problems. Program 2: Bright regions in the TR lines correspond often to network, locations where the magnetic field in enhaced. 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 - No observation with SUMER in this JOP: AR would be on the disk, not on the SUMER slit at x=-980 - 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. JOP 104 - SUMER - - We shall follow the JOP 104, if the target is not at too high latitude (y not too big). - THEMIS and VTT- - We will observe Halpha with the VTT, and CaII 8542 line if the signal is not too small. - This program will be carried 2 hours every day( between 8 and 18 UT) - Precise hours will be given daily. ********** List of participants and contacts: SUMER UV spectra planner@sumop1.nascom.nasa.gov curdt@linax1.dnet.gwdg.de innes@linax1.dnet.gwdg.de CDS UV spectra Richard Harrison harrison@solg2.bnsc.rl.ac.uk planner@cds8.nascom.nasa.gov EIT EUV images Joe Gurman gurman@gsfc.nascom.nasa.gov TRACE EUV/UV images Harry Warren hwarren@cfa.harvard.edu schryver@lmsal.com trace_planner@cheyenne.nascom.nasa.gov MICA coronagraph Marta Rovira rovira@iafe.uba.ar YOHKOH SXT images David Mckenzie hudson@isass1.solar.isas.ac.jp mckenzie@mithra.physics.montana.edu nitta@isass1.solar.isas.ac.jp sxt_co@isass0.solar.isas.ac.jp GSFC ecs@soc.nascom.nasa.gov MDI saba@mdisas.nascom.nasa.gov VTT Nicole.Mein@obspm.fr Kostas.Tziotziou@obspm.fr Brigitte.Schmieder@obspm.fr THEMIS Pierre.Mein@obspm.fr cbriand@ll.iac.es WROCLAW rompolt@astro.uni.wroc.pl DEBRECEN ludmany@tigris.klte.hu NANCAY klein@obspm.fr IRKUTSK smolkov@sitmis.irkutsk.su