JOP017 (Updated 20 April 1999) TITLE: " Dynamics of Arch Filament Systems: " CONTRIBUTORS: Schmieder, B., Malherbe, J.-M., Mein P., Mein N., Staiger J. Vial J.C., L. van Driel-Gezstelyi INSTRUMENTS INVOLVED: CDS, SUMER, MDI, EIT TRACE GROUND-BASED OBSERVATIONS: VTT, THEMIS (Tenerife) Ondrejov, Bialkov,.. =================================================================== Request of observing time during GBos and Space campaign May 13-19 1999 between 08 UT- 18:00 UT ============================================================= OBJECTIVE: Study of the dynamics of the Arch filament systems observed in a large temperature range during emerging flux in an active region in order to understand the response of the Transition region and the corona via magnetic reconnection Scientific justification: Within emerging flux in the photosphere, Arch Filament Systems are developing in active regions. They are well observed as dark filaments in H alpha and models have shown that when the tubes rise they bring denser material to chromospheric level and material is falling along both legs of the tube. The MSDP spectrographs for chromospheric lines and TRACE in EUV lines are well adapted to study the dynamics of chromospheric and coronal material in different ranges of temperatures. Many questions remain to be solved: 1) How form AFS and how they expand, is there a long flux tube below the photosphere which is partially lifted up progressively, or is there magnetic reconnection between different tubes ? We need to have coordinated observations with magnetographs as the GCT (Tenerife), SOHO/MDI and THEMIS. Extrapolations of the magnetic field to the corona can be performed and compared to the location of loops observed by TRACE. 2) In higher levels, we have observed large coronal loops with TRACE (Sept 98) and brightening in X rays with YOHKOH. Does it mean that the coronal material is compressed to higher density ? How does the material relax ? Is it a thermal or dynamic process ? Do the loop cool progressively ? Is the soft X ray brightening due to reconnection of magnetic field lines with the pre-existing field ? These questions could be studied with coordinated space and ground based observations involving TRACE, YOHKOH/SXT and SOHO (EIT, CDS, SUMER). TRACE offers the best spatial resolution in EUV lines, which is essential for our purpose. CDS: slit 2x 240 " item one : context raster 240 X 240 " with 6 lines in 3100 sec (EFINAR_1) item two : diagnostic raster 120X 120" with 14 lines in 1900 sec (EFINAR_2) (number of rasters as long as the period of observations allowed) SUMER co_pointing with CDS item one : context raster 300 X 240 " Lyman 4 item two spectra: JOP17MAY97_NV.SCL 1 h 45 min Obs in N V and neighboring lines 1x300" slit Contains: He scans, calibration exposure in N V etc, main observations in N V etc. 35 sec exposures for main observations 25x360 format for 4 lines rotation compensation JOP17MAY97_SVI.SCL;4 (add Ly betta) 3h 12min obs in S VI and various Lyman lines (L4,L5-L6,L7 +L betta) 1x300" slit 25x360" formats Contains: Full detector calibrations scan main obs in S VI and Lyman lines 60 sec exposures for main obs rotation compensation JOP 17 SEPT96 Si IV 1393 A and O V 1371 A slit 1x 129" exposure 35 sec/60 sec MDI high cadence of 1 min if possible EIT: Images of the active region in each of the four lines covering the target area with a cadence of ~10 min. TRACE: 195 (high cadence), 171 (high cadence), Lyman alpha, C IV continuum. YOHKOH SXT raster of the Active region. Campaigns for 1999: We got observing time at the VTT (Tenerife) between 11 and 20 May, 1999 and observing time at THEMIS. The MSDP will observe in H alpha and H beta at the VTT and in CaII 8542 and one more line at THEMIS. Report on previous activities: This kind of study has been partially performed with the VTT in coordination with the GCT, THEMIS (1998) and TRACE in Sept 1998. We got some preliminary results about the dynamics of the chromospheric plasma (paper I and II), the magnetic configuration (paper III) and the loops overlying the AFS (paper IV in preparation with TRACE data). In the last campaign of 1998, we observed filaments and active regions. H alpha and H beta were used at the VTT, while CaII 8542 was observed at THEMIS with the MSDP. TRACE was running on the same targets in Ly alpha, Fe IX, Fe XII and white light. Other ground based observatories were involved, for example Meudon, Wroclaw or Ondrejov. Other observers, as the PROM group (coordinated by S. Martin in USA), were observing the same targets. paper I: Mein P, Mein N, Malherbe JM, Heinzel P, Kneer F, Von Uexkull M and Staiger J: 1997, Solar Phys, 172, 161 paper II: Mein P, Demoulin P, Mein N, Engvold O, Molovny R, Heinzel P, Gontikakis C: 1995, Astron Astrophys paper III: Malherbe JM, Schmieder B, Mein P, Mein N, Van Driel L, Von Uexkull M: 1998, Solar Phys, 180, 265 paper IV: Schmieder B, Malherbe JM, Mein P, Mein N: in preparation, campaign of Sept 1998, 3D loops above AFS observed with TRACE and the VTT