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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0010

CORE: Joint Observation of the Solar Corona between Hinode EIS and NAOJ Norikura Observatory for nonthermal line broadening in the coronal emission

plan term


@ @


 name : H. Hara
Y. Suematsu
K. Ichimoto
@  e-mail : hara[at]solar.mtk.nao.ac.jp

contact person in HINODE team

 name : H. Hara @  e-mail : hara[at]solar.mtk.nao.ac.jp

 abstract of observational proposal
To understand the origin of non-thermal line broadening in coronal emission lines

 request to SOT
Observation of Ca H spicules.
The sequence that was run previously is used. Widest FOV in the NS direction is desired.

 request to XRT
The sequence that was run previously is used. No strong request.

 request to EIS
Hara is preparing the EIS study for this campaign. The following lines
will be contained in the study to compare the line width of emission
lines in the velocity unit:

       EIS                                     Norikura (two lines at the same time)
Fe X    184.54, 190.05, 195.40, 201.53    <-->   6374
Fe XI   180.41, 188.23, 192.82, 201.75    <-->   7892
Fe XIII 196.54, 202.04, 203.83,(251.94)   <-->  10747
Fe XIV  211.32, 264.78, 274.20            <-->   5303

Other EIS emission lines: Ca XVII192, Fe XII195, Fe XV284 etc.
Long exposure duration: about 120 sec will be used for high accuracy
                       of line-profile fitting.
Slit: 1 arcsec width
Raster scan step: 3  arc sec
Number of raster steps: 60 points
Raster scan area: EWxNS = 180x512 arcsec^2
Number of raster scan: 3 times possible at least for 4 hr campaign.
EIS FOV center: intentionally shifted to limb side by 100 arcsec.

 other participating instruments
Norikura: High dispersion spectra of Fe X6374 and Fe XIV5303 are obtained. High-acuracy Doppler velocity and line width are given. Independent Fe XIV 5303 imaging observations provide high-cadence imaging and Doppler informaiton.

Bi-products: <This is the most important for EIS team.> : By the simultaneous observations with Norikura Solar Observatory, EIS line width of instrumental origin is absolutely calibrated. In EIS bandpass there are Fe X lines in the short wavelength band and Fe XIV lines in the long wavelength band. These are calibrated with Fe X 6374 and Fe XIV 5303 emission lines. Norikura Solar
Observatory is going to support this campaign observation with a high priority.

Area to be observed: East or west limb in the active band, but Hinode SOT FOV should be within solar disk by 10-20 arcsec from the limb. Active regions are
good targets for higher counting statistics.

Time:  22 - 02 UT
<< Communication for Target Selection >>
The Hinode team selects the target at the limb. Bright regions have
high priority. Norikura observatory observes the Hinode target
region. In the case of no active region at the limb, heliocentric
latitude 0 deg shall be at the center of SOT FOV.

When no clear sky is expected at Norikura for a few days, the campaign can
be cancelled for other better observations. This is informed from the
Norikura observatory.

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