SOTSP: HOP12 for Hida
2007-08-06T01:53:47 to 2007-08-06T02:03:37
Science Goal: coronal heating
Program: Fast map 50 arcsec
Target: Plage
xcen=915 ycen=-132
Instrument: SOTSP
HOP/JOP: 12
Description:
Daily Note and User Entry: Eclipse season calculated to start ending 4 Aug, with transition continuing for several days or weeks, depending on instrument. (HOP20 starts for other instruments on 3 Aug, Hinode may choose to join. Hinode official HOP20 obs begin 18 Aug.) HOP24 filament and prominence 13:30 (4 Aug) - 7:00 (5 Aug), and 13:30 - 24:00 on 5 Aug. HOP29 filament/cavity cmpn starts(8 Aug) EIS: sensitivity monitoring (3.5 hours) to run in weekend plan. Coalignment program run (N-limb, E-limb, 2hour for each) to run in weekend 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)
wavelength: 6302A Continuum Intensity cadence: 0 min fov: 49,162 images: 156 JavaScript Landing Page
