2007-08-01T21:35:33.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE SOT Arikawa Sterling Shine 24 Filament in small AR Filament FIL FIL 3 212 -283 111 111 2007-07-31T15:39:34.000Z 2007-07-31T23:58:03.000Z 212 -283 Filament in small AR H lc 30sec, CaH and Gb 120sec, 2Kx2K 2x2, ROI2 Daily Note and User Entry: EIS: extended observations on one target if possible. Would prefer quiet Sun or limb observations. Coalignment program run (N-limb, E-limb, 2hour for each) to run in Tuesday plan. SOT: HOP24 prominence obs (time TBD, maybe 12 - 18 UT). 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)