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HINODE Operation Plan (HOP)

accepted on

30-Jul-09


 HOP No.

 HOP title

HOP 0128

CORE: Coordinated Observations between Hida Observatory & Hinode Satellite

plan term

2009/08/03-2009/08/16
2010/08/16-2010/08/28
2011/08/13-2011/08/18
2011/11/14-2011/11/26
2012/08/13-2012/08/24
2013/08/12-2013/08/24

   

proposer

 name : Ichimoto, Ueno
Suematsu
   e-mail : ichimoto[at]kwasan.kyoto-u.ac.jp
ueno[at]kwasan.kyoto-u.ac.jp

contact person in HINODE team

 name : Suematsu    e-mail : suematsu[at]solar.mtk.nao.ac.jp

 abstract of observational proposal
  Chromospheric active phenomena, reconnections, coronal heating process and sunspot evolution that are all related with the solar magnetic field  have become more clear by recent MHD simulations and high-resolution observations with the HINODE satellite. We intend to quantitatively verify the present models of such phenomena by simultaneous and high-cadence observations of diversified observation from the photosphere to the corona with the HINODE satellite and spectrum observation at the Hida Obs.
  For example, Hinode has found many and various chromospheric jets (Ca jets). We must verify whether the mechanisms of such jets are all magnetic reconnection (ubiquitous reconnection ?), and investigate the amount of contribution of such jets to the coronal heating process. Therefore, we will measure the 3D distributions & evolutions of the velocity field (bidirectional flow, reconnection flow, shock wave), temperature, density and magnetic field configuration around various type of jets.
  On the other hand, Hinode has also found wave-like phenomena in prominences. By adding chromospheric spectral informations, we intend to verify whether such phenomena in the prominences or dark filaments correspond to Alfven waves or fast-mode kink waves, from the point of view of the coronal heating and prominence-seismology.
  Moreover, we try to observe wave propagation from the photosphere to corona around sunspot region and investigate relationship between spatial distribution of coronal heating rate and spatial difference of characteristics of oscillation.
  To this end, Hida observatory will provide highly complementary data sets to Hinode, i.e., DST will take full spectral line profiles of CaII H,K or H-alpha with a very high time cadence of 1 to 10 sec and a moderately high spatial resolution of 1 arcsec or better (see section [8]: appendix). SMART telescope will also take full disk H-alpha Dopplergram with a spatial resolution of 1 arcsec.

 request to SOT
  1. Active Region
     1a. Low Cadence (EFR)

           BFI (CaII H)    112"x112" /600sec 432Mb/hr/30
           BFI (G-band)    112"x112" /600sec 646Mb/hr/30
           NFI (NaI or 5250A IVDG)  82"x 82" /60 sec 306Mb/hr/3
           SP (fast map)            82"x 82" (15min) once/hr

     1b,c. High Cadence (Sunspot & Flare Dynamics)
           BFI (CaII H)    56"x112" /20sec 432Mb/hr/2
           BFI (G-band)    56"x112" /20sec 646Mb/hr/2
           NFI (NaI or 5250A IVDG)  82"x 82" /20 sec 306Mb/hr
           SP (fast map)            82"x 82" (15min) once/hr

  2. Chromospheric jets

           BFI (CaII H)    56"x112" /20sec 432Mb/hr/2
           BFI (G-band)    56"x112" /20sec 646Mb/hr/2
           NFI (NaI IVDG or 5250A IQUV)  82"x 82" /20 sec 306Mb/hr

  3. Dark Filament

           BFI (G-band)    110"x110", 2x2,  /30sec 432Mb/hr/1.5
           NFI (H-alpha 3 wl)  164"x 164",2x2, /30 sec 306Mb/hr*2
           SP (fast map)       164"x 164" (30min) once/hr

  4. Prominences

           BFI (CaII H)    110"x110", 2x2,  /30sec 432Mb/hr/1.5
           NFI (H-alpha 3 wl)  164"x 164",2x2, /30 sec 306Mb/hr*2

 request to XRT
1. -- 4.

    512"x512"/30sec  75Mb(?)/hr

 request to EIS
1. Active Region

     1a. Low Cadence (EFR)
         - SK_AR1_50x320c: 50x320" /180sec, exp=5sec
           - CAM_ARTB_RHESSI_b_2: 40x120" /200sec, exp=10sec
         - TR_BRIGHT_LO: 20x144" /300sec, exp=30sec

     1b,c. High Cadence (Sunspot & Flare Dynamics)
         - SK_AR2_12x200p: 12x200" /~20sec, exp=1.5sec
         - DRW_Alf_01_2: 12x152" /60sec, exp=10sec
           - SK_AR2_50x240p: 50x240" /106sec, exp=2sec
           - CAM_ARTB_RHESSI_b_2: 40x120" /200sec, exp=10sec

  2. Chromospheric Jets
         - DRW_Alf_01_2: 12x152" /60sec, exp=10sec
           - SK_AR2_50x240p: 50x240" /106sec, exp=2sec
           - CAM_ARTB_RHESSI_b_2: 40x120" /200sec, exp=10sec

  3. Dark Filaments
         - SK_AR1_50x320c: 50x320" /180sec, exp=5sec
         - TR_BRIGHT_LO: 20x144" /300sec, exp=30sec

  4. Prominences
         - SK_AR1_50x320c: 50x320" /180sec, exp=5sec
         - TR_BRIGHT_LO: 20x144" /300sec, exp=30sec

 other participating instruments
DST/Hida

Observations with DST at Hida Obs.

   1. Active Regions

      1a. EFR
         * H-alpha 5 wavelength filtergraph:
            Wavelength: -0.8, -0.5, 0.0, +0.5, +0.8 A
        Time cadence: 15 sec
          * Ca-line spectro-heliograph:
            Scan width: about 120 arcsec
        Time cadence: about 15 sec
         * H-alpha spectro-heliograph:
            Scan width: about 120 arcsec
            Time cadence: about 15 sec

      1b,c. Sunspot & Flare Dynamics
         * H-alpha 5 wavelength filtergraph:
            Wavelength: -0.8, -0.5, 0.0, +0.5, +0.8 A
        Time cadence: 15 sec
          * Ca-line spectro-heliograph:
            Scan width: about 80 arcsec / 50 arcsec
        Time cadence: about 10 sec  /  6 sec
         * H-alpha spectro-heliograph:
            Scan width: about 80 arcsec / 50 arcsec
            Time cadence: about 10 sec  /  6 sec

  2. Chromospheric Jets
         * H-alpha 5 wavelength filtergraph:
            Wavelength: -0.8, -0.5, 0.0, +0.5, +0.8 A
        Time cadence: 15 sec
          * Ca-line spectro-heliograph:
            Scan width: about 100 arcsec / 50 arcsec
        Time cadence: about 12 sec  /  6 sec
         * H-alpha spectro-heliograph:
            Scan width: about 100 arcsec / 50 arcsec
            Time cadence: about 12 sec  /  6 sec

  3. Dark Filaments

         * H-alpha 5 wavelength filtergraph:
            Wavelength: -0.8, -0.5, 0.0, +0.5, +0.8 A
        Time cadence: 15 sec
          * Ca-line spectro-heliograph:
            Scan width: about 120 arcsec / slit-fixed
        Time cadence: about 15 sec   / 10 Hz
         * H-alpha spectro-heliograph:
            Scan width: about 120 arcsec / slit-fixed
            Time cadence: about 15 sec   / 10 Hz

  4. Prominences

         * H-alpha 5 wavelength filtergraph:
            Wavelength: -0.8, -0.5, 0.0, +0.5, +0.8 A
        Time cadence: 15 sec
         * He I 1083 nm or Ca II 854 nm full-Stokes profiles:
            Scan width: about 120 arcsec / slit-fixed
        Time cadence: about 30 sec

 remarks
[4] Time period of proposed observations, if required:

   <<Start and end dates>>
     12-Aug-2013 (Mon) to 24-Aug-2013 (Sat)

   <<Minimum number of observation days>>
     Everyday is the best. If it is impossible, 10 days.

   <<Continuity of observations>>
      Continuity of 24 hours is not required.
      We desire continuous observations for several hours in everyday
       (see section [5]).


[5] Time window in day, if required:

    <<Miminum duration>>
       Desirable duration is about 5 hours per one day
       (-02:00 to 03:00 UT).
       Mimimum duration is 1 hours pending on the target.
        The best time-period:  00:00 to 01:00 UT (AM in Japanese time)

    <<Allowability of short interruptions>>
       It is preferable that there are no interruptions except for moments
       for changing targets.


[6] Target of interest:

  1. Active Region
     1a. Low Cadence (EFR)
     1b. High Cadence (Sunspot Dynamics)
     1c. High Cadence (Flare Gas Dynamics)

  2. Chromospheric jets

  3. Dark Filament

  4. Prominences

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