JOP173 THE THREE-DIMENSIONAL STRUCTURE AND DYNAMICS OF SUNSPOTS Short title: 3D Structure and Dynamics of Sunspots Version: 29 October 2004, small update of TRACE program by SOC History: update October 2004, update March 2004 Scientists and institutes: H. Balthasar (campaign coordinator, POC for GBOs) AIP, Germany M. Sanchez Cuberes AIP, Germany K. Muglach (POC for TRACE) NRL, USA G. Aulanier Observatoire de Paris, Meudon, France A. Berlicki Observatoire de Paris, Meudon, France J.-M. Malherbe Observatoire de Paris, Meudon, France P. Mein Observatoire de Paris, Meudon, France G. Molodij Observatoire de Paris, Meudon, France B. Schmieder Observatoire de Paris, Meudon, France (POC for CDS) G. Cauzzi Osservatorio Astrofisico di Arcetri, Florence, Italy K. Janssen, Osservatorio Astrofisico di Arcetri, Florence, Italy M. Collados IAC, Tenerife B. Fleck ESA/GSFC (POC at EOF) S. Regnier ESA/ESTEC K. Langhans The Institute for Solar Physics, Stockholm, Sweden G. Scharmer The Institute for Solar Physics, Stockholm, Sweden P. Suetterlin Universiteit Utrecht, Utrecht, Netherlands K. Tziotziou Universiteit Utrecht, Utrecht, Netherlands B.W. Lites High Altitude Observatory, Boulder, CO, USA Participating instruments: TRACE (EOF GSFC) SOHO MDI (EOF GSFC) SOHO CDS (EOF GSFC) VTT (Vacuum Tower Telescope, Tenerife) THEMIS (Tenerife) SST (Swedish Solar Telescope, La Palma) DOT (Dutch Open Telescope, La Palma) DST (Dunn Solar Telescope, Sac Peak) will not participate in Nov/Dec 2004 MST (Meudon Solar Tower, Meudon) Scientific objective and justification The aim of this Joint Observing Program is to study the three-dimensional structure of sunspots and active regions. State-of-the-art spectro-polarimetry will be carried out at a number of ground-based observatories to deliver the vector magnetic field. As these observations will be carried out in several heights in the solar atmosphere we can also derive the vertical gradient of the field. In addition, we are interested in the presence of magneto-acoustic waves. We plan to use the four Canarian solar telescopes (VTT, THEMIS, SST, DOT) together with TRACE and SOHO/MDI. Additional data will be collected at the Dunn Solar Telescope at Sac Peak and at the Meudon Solar Tower. TRACE and MDI will complement the spectro-polarimetric data from ground. They can deliver continuous high resolution images over longer time periods and will help to connect the data taken in the US to the ones taken at the European observatories. Oscillations in coronal loops are another topic we plan to investigate in this JOP. These oscillations (as seen in TRACE 171 images) are assumed to be excited at their footpoints which are located at or near sunspots. Our photospheric and chromospheric magnetic field observations from ground will provide excellent boundary conditions to study the excitation of the loop oscillations. Observing Sequences for TRACE, MDI and CDS: TRACE: a) 1550,1600,1700 in about 20s cadence, strictly regular cadence 256 x 256 pixel FOV. EUV/UV Context images 2-3 times during 9h run Calibrations, including darks, between 07-08UT b) filters: 171, 1600 171: 768 x 768 FOV (if possible) 1600: 512 x 512 FOV cadence should be around 20s, but STRICTLY regular, no other filter images interleaved. We hope to observe loop oscillations with this program in 171. In case we do not find them, the 1600 data will still be useful as long as the sequence is fast and regular. Before and after the sequence additional images in all other filters should be taken as context. We would also appreciate if calibration data were taken around this time. Especially several dark images in the selected filters and FOVs taken before the start of the sequence each day. Which program will be run will eventually depend on solar conditions like the presence of sunpot and loops. As TRACE will be in eclipse at the time of the 2004 campaign we will mostly run the UV program. MDI: For a target inside the HR FOV: hr_t2_ve_fe_me (Doppler grams, magnetograms and Igrams in 1 min cadence) Otherwise a full disk 3 variable program in 1 min cadence Note, that we ask for MDI support for the times specified below (7-18 UT). Note, that we do not ask for continous coverage. If additional DSN is requested then it should only cover these specific times. CDS: studies that should be used: repeat mainly: SIG-FT44 context raster 4X4 24 min SIG_FT44 4x4' with He I, O IV (density-sensitive), O V, Si X (density-sensitive), Mg X Si XII, Fe XIX one run every 2hours with ARDIAG_2 4x4' with lots of diagnostic lines 1 h 24 or if the field of view is small ARDIAG_1 smaller 120"x120" (but faster) raster with lots of diagnostic lines (similar to ARDIAG_2) In 2004 the campaign will take place 23. Nov. - 02. Dec. 2004, 07:00 - 18:00 UT Target selection will be done at TF and pointing coordinates will be given according to the planning schedule of TRACE (which will be in eclipse at this time of the year). Coordinator on ground will be H. Balthasar (HBalthasar@aip.de), POC at the EOF will be B. Fleck (bfleck@esa.nascom.nasa.gov).