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HINODE Operation Plan (HOP)

accepted on

19-may-11


 HOP No.

 HOP title

HOP 0189

Coordinated observation with Akatsuki

plan term

2011/06/23-2011/06/27

@ @

proposer

 name : Isobe, Asai, Imamura, Shiota, Yaji @  e-mail : isobe[at]kwasan.kyoto-u.ac.jp

contact person in HINODE team

 name : Sakao @  e-mail : sakao.taro[at]isas.jaxa.jp

 abstract of observational proposal
Information on the small-scale structures of plasma near the sun is important for understanding the mechanism of plasma heating and accelerating the solar wind. Phase and amplitude scintillation measurement of spacecraft radio signals during solar conjunctions can be used to obtain information of the small-scale strucutures of the electron density.

The solar conjunction of AKATSUKI in June 2011 provides an opportunity to perform such observation in coordination with Hinode. AKATSUKI (Planet-C) is Venus Climate Orbiter of JAXA. The injection to the the Venus orbit in December 2010 was not successuful and the space craft is now in solar orbit at around 0.7AU. There will be four close conjunction of Akatsuki and the Sun by the end 2015, and the one in June-July 2011 is the closest. The minimum sun-earth-probe (SEP) angle is 0.405 degree (=1458 arcsec ~ 1.54 R_sun) when the prove passes just above the north pole as seen from th Earth.

The Akatsuki team plans to perform radio sounding observation of solar wind on June 6 - July 8, 2011, when the SEP angle changes in the range of 0.4 ~ 5.4.  It will provide the spectra of electron density fluctuation in the range of 0.0001-10Hz,  corresponding to the spatial scale of about 30~300000km (assuming solar wind speed of 300km/s).

We propose coordinated observation of Hinode during June 23-27 when the prove passes above the north pole.  XRT and EIS observation, along with EUV and coronagraph images from SDO, STEREO and SOHO, can provide the information of steady strucutre in the corona/solar wind as well as of the occurrence of polar jets and CMEs.  By comparison with these imaging observation we will be able to investigate the difference of electron density fluctuation in and outside the coronal hole and plumes, and, if they occur, in jets and CMEs. Moreover, spectroscopic observation by EIS may allow us to study the correllation between the density fluctuation and other plasma parameters such as  intensity in different lines (i.e., DEM), electron density, and line width (if there are enough counts). We note that the Akatsuki's position will be slightly (~20") above the EIS field of view even in the closed conjunction on 25th. However, EIS data is still useful because it provides unique information of plasma parameters between the solar surface and the height at with Akatsuki measurement is done. The vector magnetogram from SOT/SP can be used to model the magnetic fields in the coronal hole and plumes. We also plan to obtain some H-alpha images in the north pole region at the Hida observatory to monitor
the transient events.

 request to SOT
NO request for SOT in Day 1 and 4

Day 2 and 3:
SP:
Two full FOV fast map in the beggining and end of the observation.
FoV 320h x 164h, Pixel size: 0.32h/pix, Binning: 2x2, Single side mode
Exposure: 4.8 sec (6 Cycles), JPEG Quality: Q75, Data rate: 600Mbits/map

FG:
BFI G-band and CaH: FOV 221"x111",, Binning: 2x2
Cadence: one image per one orbit
NFI Na I: IVDG mode, FoV: 328h x 164h, Binning: 2x2
One image per orbit

 request to XRT
Day 1 and 4:
Filter: Al/poly
Full FoV, Binning: 2 x 2
Exposure time: As long as possible.  (Depending on the presence of ARs).
Cadence as high as telemetry allows (minimum is one image per orbit)

Day 2 and 3:
Filter: Al/poly
Full FOV, Binning: 2 x 2
Exposure time: as long as possible (Depending on the presence of ARs).
Cadence as high as telemetry allows (minimum is one image per orbit)

 request to EIS
No request for EIS in Day 1 and 4.

Day 2 and 3:
EIS_STUDY: To be prepared by J-side EIS team.
Exposure: 120s
Raster : scanning
Slit: 2"
Step_size: 5"
FOV: ~40" ~ 512" (use the upper half of CCDs)
Lines: series of Fe lines (from VIII to XV), Si X (258.37A)

 other participating instruments
Akatsuki

 remarks
<Time period of proposed observations>
June 23-27, 2011  (Starting around 22UT of 23th)

<Time window in day>

Day 1:
2011/06/24/23:00UT - June 24 06:30UT
Only XRT data is requrired in this window. We wish to have XRT data coverage as good as possible during this period, but the minimum requirement is one XRT image during that time.

Day 2:
2011/06/24.22:57(SAA_EXIT) - 2011/06/25.08:03(SAA_ENTRY)
This includes6 consecutive observation window between eclipses/SAAs. Minimum requirement is 4 consecutive observation window during this period.

Day 3:
2011/06/25.23:29(SAA_EXIT) - 2011/06/25.08:40(SAA_ENTRY)
This includes6 consecutive observation window between eclipses/SAAs. Minimum requirement is 4 consecutive observation window during this period.

Day 4:
2011/06/26/23:00UT - June 27 06:30UT
Only XRT data is requrired in this window. We wish to have XRT data coverage as good as possible during this period, but the minimum requirement is one XRT image during that time.

The  scintillation measurement by Akatsuki will be performed during 01-07UT on June 25 and 26, and 02-06UT on June 24 and 27.

<Target of interest>
Off-limb coronal hole region in the north pole. Exact pointing will be provided to CP and COs using the information from Akatsuki team. Basically, pointing should be as close to the limb as possible toward Akatsuki.

<Remarks>
- Since SOT does not take much telemetry, we'd appreciate it, if part of the data allocation for SOTcan be given to EIS and XRT.
- One of the proposers (H. Isobe) will be at ISAS for coordination during the HOP period.

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