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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0008

Stereoscopic Observation of the Coronal Structures

plan term


@ @


 name : S. Plunkett @  e-mail : simon.plunkett[at]nrl.navy.mil

contact person in HINODE team

 name : J. Mariska @  e-mail : John Mariska <mariska[at]nrl.navy.mil>

 abstract of observational proposal
Scientific Objectives
The aim of this joint observing program is to study the three-dimensional nature of coronal structures using observations from multiple vantage points in the ecliptic plane. Efforts at three-dimensional reconstructions to date have relied on solar rotation to provide multiple viewpoints of solar structures from a single observing location. These efforts are hampered by the fact that coronal structures are highly dynamic, and may evolve significantly over the timescales of several days that are necessary to obtain multiple lines of sight. The SECCHI instruments on the STEREO mission remove this restriction by providing simultaneous imaging of the corona from two spacecraft, one leading and the other lagging the Earth in heliocentric orbit. When combined with observations from SOHO, TRACE, and Hinode located along the Sun-Earth line, we have the capability for the first time to obtain near-simultaneous observations of coronal structures along three lines of sight. This will permit realistic three-dimensional reconstructions of coronal loops and other features, such as polar plumes.

Stereographic reconstruction techniques will be applied to EUV and visible-light imaging data from STEREO, SOHO and TRACE instruments. EUV spectroscopy from SOHO and Hinode will provide plasma diagnostics for selected target regions within the fields of view of the full-disk imaging instruments. Longitudinal and vector magnetograms from SOHO and Hinode will provide details of the photospheric and chromospheric magnetic fields underlying the coronal structures. Extrapolations of these data into the corona will provide sanity checks and constraints on the three-dimensional reconstructions of coronal features.

 request to SOT
Hinode/SOT: TBD, but should include photospheric and chromospheric vector magnetograms at a high cadence to permit reconstruction of coronal magnetic fields in target region.

 request to XRT

 request to EIS
Hinode/EIS: TBD, but should include lines over a broad range of temperatures to span the range covered by SECCHI/EUVI, and target region should be coordinated with SOHO/CDS.

 other participating instruments
STEREO/SECCHI: Full-disk EUV images will be obtained with a cadence of TBD minutes in 4 wavelengths: 304 A, 171 A, 195 A and 284A. Visible-light coronagraph images will be obtained with a cadence of TBD minutes in the range 1.4-4 Rs and 2.5-15 Rs.

SOHO/EIT: Full-disk images in wavelengths to match SECCHI, at synoptic cadence. If possible, these images should be in full-resolution (1024x1024 pixels), and should be synchronized with STEREO/SECCHI images.

SOHO/LASCO: Synoptic observations with C2 and C3. If possible, these images should be synchronized with STEREO/SECCHI images.

SOHO/CDS: Suggest using eject_v3/v18 study. This is a 240"x240" raster with a good selection of lines over a wide temperature (10,000 K to 2.5 x 106 K), and contains a
density diagnostic. Target region should be coordinated with Hinode and TRACE.

SOHO/MDI: Full-disk magnetograms at TBD cadence. If target region used by SOHO/CDS and Hinode is within the high-resolution field of view, high-resolution magnetograms and visible-light filtergrams with a 1 minute cadence would be desirable.

TRACE: TBD, but should include EUV images of target region used by SOHO/CDS and Hinode.

SECCHI Campaign Observations

For at least the first four days of the campaign (May 4th-7th), SECCHI will run its "Active Region/CME Watch" observation sequence. This consists of full-disk EUVI 171 A images every 75 seconds, with the other three wavelengths (195, 284 and 304 A) at a 5 minute cadence. COR1 will obtain pB sequences every 5 minutes. COR2 and the HIs will continue their synoptic observations.

For those instruments that need to select a target for their observations, I suggest AR 10953 as the best choice for now. If you can include AR 10954 in the field of view, that would be great. There may be a need to revisit the choice of target as these regions approach and cross the west limb. With luck, a new region will appear in the next few days.

1. High cadence 304 (spicules)
- regular synoptic HI, COR2, and COR1 program
- 304 every 37.5 sec (37/38 sec), ICER5 compression
- 195 every 10 min, ICER5
- 171, 195, 304 @ ICER4, and 284 @ ICER6 compression every 2 hours
- Run only for a couple of days and only if there are no ARs

2. AR and CME watch (2x synoptic cadence & lower compression)
- regular synoptic HI and COR2 program
- COR1 polarization sequence every 5 min
- 171 every 75 sec, ICER5 compression
- every 5 min: 195 @ ICER5 compression, 284 @ ICER6 compression, 304 @ ICER4 compression

3. All wavelengths at 2.5 min (ICER5/6 compression)
- regular synoptic HI and COR2 program
- COR1 polarization sequence every 5 min
- every 2.5 min: 171, 195, 304 @ ICER5 compression, 284 @ ICER6 compression

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