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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0070

WHI ToO #3: Activity in Filaments and Filament Channels

plan term


@ @


 name : Gibson @  e-mail : sgibson[at]hao.ucar.edu

contact person in HINODE team

 name : Sterling @  e-mail : alphonse.sterling[at]nasa.gov

 abstract of observational proposal
To study filaments, filament channels, and filament cavities in order to (a) understand the time dependent, three dimensional density, temperature, and magnetic structure of filaments and filament channels and cavities (b) study how filaments form (c) study filament activation in the chromosphere and CMEs in the corona to better understand how this process works and how it is related to CMEs.

In addition, if the observed structures erupt we will (d) study the evolution of the cavity during eruption, and (e) map the EUV signatures into the coronal structures as represented by the coronagraphs, with the goal of understanding more clearly the structure and manifestations of CMEs in the low corona.

 request to SOT
Hinode/SOT -- campaign contact: Scott McIntosh
We plan slightly different settings, depending on whether we are observing on disk (e.g., filament or filament channel), or off disk (e.g., cavity or prominence).

- On disk:
1) Prior and after Observing Period Perform 1" x 100" X length-of-channel spectropolarimetric maps in Fe I 6301/6302
2) During Observing Period perform 1"X100"x100" repeated rastering of SP.

Alternating at 10s cadence
Ca II H (3968.5 Ang) full field (200"x100") of channel region
CN I (3883.0 Ang) full field (200"x100") of channel region

Choice of one - maybe we'll be able to tune by then and get both 10s
Fe I 6302.5 Ang. magnetograms at 5s cadence (200"x100")
H I 6562.8 Ang. line core at 5s cadence (200"x100")

- Off disk:

Ca II H (3968.5 Ang) full field (200"x100") of prominence region, 5s cadence

H I 6562.8 Ang. line core at 5s cadence (200"x100")

 request to XRT
Hinode/XRT -- campaign contact Kathy Reeves
Main Loop:
Filters: Al/poly (8-16 sec exposure), Ti/Poly (16-23 sec exposure)
Cadence: ~1.5 min for whole loop.
FOV: 512"x512".

In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures.

Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (512"x512" 23 sec) every ~30 minutes.

 request to EIS
Hinode/EIS -- campaign contacts: David Williams, Alphonse Sterling
EIS will run different studies, depending on whether we are observing cavities or filaments.

Cavities: Our main plan for observations if we have a good filament cavity at the limb is to choose from among these three basic programs: 1) A combination of the 2" slit study CMEO_SLIT_STUDY and the slot (40" wide slit) study CMEO_SLOT_STUDY. These studies are designed to observe CME eruptions and related phenomena. 2) A 4.5 hour raster which includes several different cool (TR) lines; this study is GAD002_AR_RAST, and would allow us to make deep spectrograms over a fairly large (about 300'') FOV. We hope to be able to determine physical properties of the cavity material, or at least of its bright boundary if we cannot detect the cavity material itself. 3) A spatially-sampling raster, using a 1" slit but with 10" steps. This would take about 45 min to complete and include full spectral information. This study is called QS_ATLAS_OFFLIMB.

We would favor running (1) during the observing Focus Time Period in the hope of observing an eruption, since MLSO and SECCHI/COR1/EUVI (also involved in the campaign; see below) might be running high time-resolution observations. We would perhaps choose to run the longer rasters (3, and especially 2) during the observing Focus Time Period if our best guess says that an eruption is not eminent (e.g., due to lack of rise of the cavity over the previous days - Gibson et al. 2006; S. Martin 2006, private comm.), or we would request that the Hinode team consider running the longer rasters prior to the start of the campaign prime time if there is no conflicting observational target.

Filaments: When a good cavity at the limb is not visible, then we will look at filaments or filament channels on the disk. We would run a selection of the previously-developed filament studies for these observations.

 other participating instruments
TRACE -- campaign contact Kathy Reeves
MLSO -- campaign contact Joan Burkepile
HELIO -- campaign contact Sara Martin
COMP -- campaign contact Steve Tomczyk

Further Details:
More details can be found at the following page:
(especially under "targeted observing plans").

When appropriate ToO is available, during the campaign period 20 March - 16 April 2008.  Sarah Gibson is to notify the instrument contacts when an appropriate target is available.

Observation Time Period:
1600-2000 UT on selected days during campaign, as targets of opportunity permit; this is good for for joint observations with ground stations in Hawaii and California.  During some periods, EIS may run a 4.5 hr raster (see EIS entry below).

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