Title: 3-D structure and evolution of filaments/prominences Authors: D.E. Innes, M. Madjarska, B. Inhester, S.K Solanki Intruments and POCs SOHO/SUMER: D.E. Innes, M. Madjarska SOHO/CDS: A. Fludra SOHO/MDI: TBD HINODE/SOT: H. Isobe HINODE/EIS: TBD HINODE/XRT: TBD TRACE: TBD STEREO: B. Inhester VTT (Tenerife): A. Lagg Huairou (China): H. Zhang Scientific Objectives: Filaments are cold, dense structures rising up to 50” into the corona. They are believed to be supported by magnetic fields and are surrounded by hot ionized coronal plasma. Their evolution is possibly accompanied by small high temperature reconnection jets in the transition region and corona. The aim of this HOP-JOP is to observe the 3-D structure of filaments/prominences and their relationship to the surrounding coronal structure. Measurements of the photospheric and chromospheric vector magnetic fields will be used to reconstruct the coronal fields and test theories of filament support. Spectroscopic observations of the chromosphere, transition region, and corona will provide signatures of reconnection and plasma diagnostics. Target: Filament as it rotates across the disk and prominences on the limb. The observation time is 6 hours at each position. Proposed Dates: The time for this proposal has two constraints. One is that the two STEREO spacecraft are at the correct separation for stereoscopy of filaments. This constrains the observations to be before the end of 2007. Later when the s pacecraft are further apart, it will be difficult to make stereoscopic images of filaments. The second constraint is the availability of ground-based vector field and Halpha observations. We have VTT observing time from 2007 Oct 22 - Nov 2, when we can obtain measurements of chromospheric vector fields. SUMER is also planning a campaign to be run at the same time, so this would be a good time to run this JOP. Detailed Observing sequences: STEREO: Stereoscopic high cadence 304, 171, 195 images SOHO/SUMER: map connection to chromosphere, pick up transition region and coronal flows. Observations in two bands C I, Si III, Ne VI, Ca X, Ca XIII, Fe XIX and C I, Si I, N V, O V, Mg IX SOHO/CDS: Detect brightenings with high cadence He I, O V, Mg IX SOHO/MDI: High Res when possible Hinode/SOT: Ca II, Blue continuum, magnetic field, Halpha + SP scan and fast rasters Hinode/EIS: He II, Si VII, Fe VIII, Fe X, XI, XII, XIII, XIV, XV, XVI, FeXXIV Hinode/XRT: Structure and evolution of hot loops overlying the filament. TRACE: 171 and 1215, with 1600 for coalignment VTT: Chromospheric flows and vector fields (Spectropolarimetry in He I 10830) Huairou: Vector magnetic fields