2007-08-01T15:30:20.000Z http://sot.lmsal.com Ted Tarbell LMSAL http://lmsal.com 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA, 94304 +1-650-424-2400 tarbell@lmsal.com Hinode SOT Arikawa Sterling Nagata 29 29 null filament Ha CaH Gb FIL FIL Filament 3 667 -432 0 0 2007-08-03T00:19:30.000Z 2007-08-04T10:37:00.000Z 667 -432 IHY FILAMENT OBSERVING CAMPAIGN: Activity in Filaments and Filament Cavities H lc 30sec, CaH and Gb 120sec, 2Kx2K 2x2, ROI2 Daily Note and User Entry: * Second pass probably to be canceled due to anticipated typhoon at USC. * andnbsp;Will modify plan schedule accordingly. andnbsp;Have only two passes: OP/OG upload, and only one table upload (EIS). EIS: MHC software will be updated soon. andnbsp;Will stop observations for one day. Coalignment program run (N-limb, E-limb, 2hour for each) to run in Thursday plan. XRT: Stop X-ray observation (and perform CCD bakeout).; Request to SOT: SOT (Hinode/SOT -- campaign contact: Scott McIntosh): --- We plan slightly different settings, depending on whether we are observing on disk (e.g., filament or filament channel), or off disk (e.g., cavity or prominence). - On disk: SP: 1) Prior and after Observing Focus Time Period perform 1"" x 100"" X ; ; length-of-channel spectropolarimetric maps in Fe I 6301/6302 2) During Observing Focus Time Period perform 1"" X 100"" x 100"" ; ; repeated rastering of SP. BFI: Alternating at 10s cadence Ca II H (3968.5 Ang) full field (200"" x 100"") of channel region CN I (3883.0 Ang) full field (200"" x 100"") of channel region NFI: Choice of one - maybe we'll be able to tune by then and get both 10s Fe I 6302.5 Ang. magnetograms at 5s cadence (200"" x 100"") H I 6562.8 Ang. line core at 5s cadence (200"" x 100"") - Off disk: BFI: Ca II H (3968.5 Ang) full field (200""x100"") of prominence region, 5s cadence NFI: H I 6562.8 Ang. line core at 5s cadence (200"" x 100"") ; Scientific Objectives: Goals: To study filaments, filament channels, and filament cavities in order to (a) understand the time dependent, three dimensional density, temperature, and magnetic structure of filaments and filament channels and cavities (b) study how filaments form (c) study filament activation in the chromosphere and CMEs in the corona to better understand how this process works and how it is related to CMEs. In addition, if the observed structures erupt we will (d) study the evolution of the cavity during eruption, and (e) map the EUV signatures into the coronal structures as represented by the coronagraphs, with the goal of understanding more clearly the structure and manifestations of CMEs in the low corona.; Other Instruments: Other Instruments (with campaign points of contact): -------------------------------------------------- SOHO/CDS and SOHO/EIT (Terry Kucera); SOHO/UVCS (Kuen Ko, John Raymond); SMEI (David Webb); STEREO/SECCHI (Simon Plunkett, James Mcateer); TRACE (Kathy Reeves); MLSO (Joan Burkepile); HELIO (Sara Martin); COMP (Steve Tomczyk)