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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0171

Magnetic Field Structure of Active Region from Photosphere to Chromosphere

plan term




 name : Oi, Nozawa, UeNo, Ichimoto, Hagino, Hanaoka    e-mail : 10nm304n[at]mcs.ibaraki.ac.jp

contact person in HINODE team

 name : Suematsu, Ichimoto    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 spectro-polarimetry observation at the Hida Observatory and the Mitaka Campus.

This proposal aims to establish an observational picture of the magnetic field vector within and under active region sunspot or filaments. Active region filaments are particularly interesting because the fields are strong enough, and the filament structures are generally low enough in the solar atmosphere, that traditional Zeeman effect measurements of the field in the photosphere consistently show signatures characteristic of the magnetic structure of the filament at that level.

It is now appropriate to attempt similar measurements of the photosphere below filaments coupled with simultaneous measurements of the filament structure at chromospheric temperatures and densities. The latter measurements of filaments on the disk are made possible by significant advances within the past few years toward interpretation of polarization measurements in chromospheric lines sensitive to both the Hanle and Zeeman effects If such measurements can be obtained with good spatial resolution, and then coupled to the proven measurements of the vector field in the photosphere below the filament, we hope to develop a glimpse of the actual 3-dimensional structure of the entire filament magnetic field system.

To this end, Hida observatory will provide highly complementary data sets to Hinode, i.e., DST will take chromospheric full-stokes profiles in He I and upper photospheric ones in Si I lines near 1083 nm (MTK campus will take them, too).
SMART telescope will also take full disk H-alpha Dopplergram with a spatial resolution of 1 arcsec (see section [8]:appendix).

The concrete list of our targets are described in section [6].

 request to SOT
1. Active Region (Sunspot 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. 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

 request to XRT
 512"x512"/30sec  75Mb(?)/hr

 request to EIS
   1. Active Region

           - 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. Dark Filaments

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

 other participating instruments
Observations with DST at Hida Obs. and SFT at MTK campus

    1. Active Regions

          * H-alpha 5 wavelength filtergraph (at Hida Obs.):
Wavelength: 0.0, +/-0.5, +/-0.8 A
        Time cadence: 2 min

          * Spectro-Polarimetry (at Hida Obs. and MTK campus):
    in the chromospheric He I and upper photospheric Si I lines
                    near 1083 nm (full-stokes)

   2. Dark Filaments

       * H-alpha 5 wavelength filtergraph (at Hida Obs.):
            Wavelength: 0.0, +/-0.5, +/-0.8 A
        Time cadence: 2 min

* Spectro-Polarimetry (at Hida Obs. and MTK camus):
   in the chromospheric He I and upper photospheric Si I lines
                   near 1083 nm (full-stokes)

○Point of contact. Name and email address:
       <<Hida Obs.>>
          Satoru UeNo         e-mail: ueno[at]kwasan.kyoto-u.ac.jp
          Kiyoshi Ichimoto    e-mail: ichimoto[at]kwasan.kyoto-u.ac.jp
<<Mitaka Campus>>
  Masaoki Hagino      e-mail: hagino[at]solar.mtk.nao.ac.jp
  Yoichiro Hanaoka    e-mail: hanaoka[at]solar.mtk.nao.ac.jp
       <<Hinode Team>>
          Kiyoshi Ichimoto    e-mail: ichimoto[at]kwasan.kyoto-u.ac.jp
<<Ibaraki univ.>>
  Akihito Oi          e-mail: 10nm304n[at]mcs.ibaraki.ac.jp
  Satoshi Nozawa      e-mail: snozawa[at]mx.ibaraki.ac.jp

○Time period of proposed observations, if required:

     <<Start and end dates>>
        27-Sep-2010 (Tue) to 7-Oct-2010 (Fri)
        The seeing and weather condition around Hida Obs. in this season is the best.

     <<Minimum number of observation days>>
        Everyday is the best. If it is impossible, 5 days

     <<Continuity of observations>>
        Continuity of 24 hours is not required.
        We desire continuous observations for several hours in everyday.

○Time window in day, if required:
     <<Miminum duration>>
        Desirable duration is about 5 hours per one day (22:00 - 03:00 UT).
        Mimimum duration is 1 hours pending on the target.
        The best time-period:  23:00 - 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.

○Target of interest:

   1. Active Region (Sunspot Dynamics)
   2. Dark Filament

●Oi's master thesis

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