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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0116

Joint Observations for HINODE with CORONAS-TESIS

plan term




 name : Korreck, Golub, Bogachev    e-mail : kkorreck[at]cfa.harvard.edu

contact person in HINODE team

 name : Golub    e-mail : golub[at]head.cfa.harvard.edu

 abstract of observational proposal
This proposal requests an observation of the full solar disk using XRT to coordinate with TESIS-CORONAS observations for the period of April 6-10, 2009 while CORONAS is out of eclipse.  If an active region or well developed coronal hole is present, we request support from EIS and SOT.  These observations will also be coordinated with TRACE.

TESIS an EUV imager aboard CORONAS-F  a recently launched Russian mission is the coordinating observatory.  The TESIS instrument is an imager with several band in the EUV  (304, 171 Angstrom).  TESIS has also 2 high-temperature channels: the first is MgXII 8.42 A (imaging of plasma with T~8 MK), and the second - FeXIII 132 A (T~10 MK).  Both channels can work in full disk and frame mode. In MgXII TESIS already has successful observation of high-temperature plasma even in deep minimum conditions. This will be utilized in our coordinated program.

TESIS has shown great first results: The resolution is 1 arcsecond and their cadence for full disk photometric studies is 5 minutes.

 request to SOT
SOT data are requested to do alignment with MDI and CORONAS. A Spectro-Polarimeter (SP) observations are requested over the largest field of view once an hour each day, interspersed with BFI images in G-band, Ca II and H-alpha.

 request to XRT
XRT will follow TESIS in full disk observations. XRT will take a full resolution image in Al-poly and Be-thin once an hour throughout the observation period.  Then XRT will take 2x2 binned full disk long exposure images in Ti-poly every 5 minutes during the rest of the 6 hours.

 request to EIS
EIS is requested to do a wide range of temperature raster on an active region or coronal hole.

 other participating instruments

Target/Pointing: Sun center unless there is a well-developed active region or coronal hole. The Sun center pointing will allow us to image the Sun at the same time as TESIS in complemetary wavelengths for studies of the extended coronal emission as well as loop structures, and overall morphology.

Duration: The study should be run for five days for a 6-hour period each day.

・We request Sun-center pointing from the 12 UT synoptic to the 18UT synoptics so that the program can be run inside this time frame every day for each of the 5 days.

・If an active region or well-developed coronal hole is present, we would request EIS and SOT to support us in the coordinated observations.

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