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HINODE Operation Plan (HOP)

accepted on

 HOP No.

 HOP title

HOP 0029

IHY FILAMENT OBSERVING CAMPAIGN: Activity in Filaments and Filament Cavities

plan term


@ @


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

contact person in HINODE team

 name : A.Sterling
Scott McIntosh
Kathy Reeves
David Williams
@  e-mail : alphonse.sterling[at]nasa.gov

 abstract of observational proposal
Goals: 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
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

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

Alternating at 10s cadence
Ca II H (3968.5 Ang) full field (200" x 100") of channel region
CN I (3883.0 Ang) full field (200" x 100") 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" x 100")
H I 6562.8 Ang. line core at 5s cadence (200" x 100")

- 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" x 100")

 request to XRT
XRT (Hinode/XRT -- campaign contact: Kathy Reeves):

XRT observations will be of the form of basic main observation loop over a
target-focused FOV, with less frequent context observations including full-disk

Main Loop:

Filters: Al/poly (8-16 sec exposure), Ti/Poly (16-23 sec exposure)
Cadence: ~1.5 min for whole loop
FOV: 768"x384"

Context Observations:

Al/poly (2048x2048, 2x2 binned), 5 thin Be (768"x384" 23 sec) every ~30 minutes

For both types of observations, cadences will be reduced as required to protect
the CCD if there is an active region on the disk during the observations.

 request to EIS
EIS (Hinode/EIS -- campaign contacts: Alphonse Sterling and David Williams):

EIS will run different studies, depending on whether we are observing cavities
or filaments.


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.


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
Other Instruments (with campaign points of contact):
SOHO/CDS and SOHO/EIT (Terry Kucera); SOHO/UVCS (Kuen Ko, John Raymond); SMEI
(David Webb); STEREO/SECCHI (Simon Plunkett, James Mcateer); TRACE (Kathy
Reeves); MLSO (Joan Burkepile); HELIO (Sara Martin); COMP (Steve Tomczyk)

1800-2200 UT daily

The campaign web site is:

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