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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0275

Chromospheric dynamics in active region with a coordinated observation between Hida, Hinode and IRIS

plan term




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

contact person in HINODE team

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

 abstract of observational proposal
Chromospheric dynamic phenomena such as jets, sudden heatings, etc. are all related with the fundamental plasma processes, i.e., magnetic reconnections, waves and shocks, and they have become more clear by recent MHD simulations and high-resolution observations with the HINODE and IRIS.

We intend to quantitatively verify the present models of such phenomena by simultaneous and high-cadence observations covering a wide range of solar atmosphere from the photosphere to the lower corona by using the HINODE, IRIS and multi-line spectroscopic observation with the Domeless Solar Telescope (DST) at the Hida Obs.

For example, we will verify whether the mechanisms of chromospheric jets are all magnetic reconnection (ubiquitous reconnection) by measuring the 3D structures & evolutions of the velocity field   (bidirectional flow, reconnection flow, shock wave), temperature, density around the jets.

Gas dynamics in flare kernels is another interest. We will try to detect the downward propagating shock in chromosphere just beneith the evapolation site and verify the dynamic model of the flaring chromosphere and determine the spatial distribution of energy deposition to clarify the heating mechanism.

Oscillation of sunspots is another target of this proposal. Waves propagating upward and their evolution into shocks will be investigated to evaluate the energy flux and dissipation that may heat the sunspot chromosphere and oberlaying corona.

To this end, Hida observatory will provide highly complementary data sets to Hinode and IRIS i.e., DST will take full spectral  ine profiles of CaII K, Ha and CaII854nm over a FOV of 50"x150" with a time cadence of 10 sec and a moderately high spatial resolution of 1 arcsec or better. It is stressed the combination of Hinode, IRIS and DST/Hida, provides  a powerful tool for diagnosing the 3D solar atmosphere for the first time.

 request to SOT
BFI (CaII H)    56"x112" /10sec 862Mb/hr/2
BFI (G-band)    56"x112" /60sec 310Mb/hr/2
NFI (NaI IV)    82"x 82" /60 sec 106Mb/hr
SP (fast map)   41"x 82" (15min) once/hr

 request to XRT
384"x384"/30sec  75Mb(?)/hr

 request to EIS
study ID 398 slit2 hot loop osc1: 20x112" /75sec, exp=5sec

 other participating instruments
Sit and stare, slit on a sunspot umbra
Cadence: 10sec for spectra
Mg II h/k, C II and Si IV

For flares: OBS 3860009153,
 Large sit-and-stare 0.3x120 1s  C II   Si IV   Mg II h/k Deep x 8,
 which has a 9.6 s raster cadence and 29s SJI cadence.
For non-flaring sunpots: OBS 3820009153,
 same but with medium linelist instead of flare linelist

Observations with DST at Hida Obs.
          * H-alpha 5 wavelength filtergraph:
            Wavelength: -0.8, -0.5, 0.0, +0.5, +0.8 A
        Time cadence: 15 sec
          * Multi-line (CaII K, Ha, CaII 854nm) spectro-heliograph:
            Scan width: about 50 arcsec
        Time cadence: about 10 sec

Time period of proposed observations:
  <<Start and end dates>>
    9-Nov-2014 (Sun) to 15-Nov-2014 (Sat)
    26-Nov-2014 (Wed) to 28-Nov-2014 (Fri)

  <<Minimum number of observation days>>
    6 days in total

  <<Continuity of observations>>
     We desire continuous observations for a few hours in everyday
     (see section [5]).

Time window in day:
  <<Miminum duration>>
     Desirable duration is about 4 hours per one day
     (-1:00 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.

Target of interest:
Specific target of observation will be daily proposed from the following themes with taking into account solar situations:

1. Active Region on the disk
   Sunspot oscillation, small scale energy release, Flare ribbons

2. Chromospheric jets
   spicules (in case there is no sunspot on the disk)

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