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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0067

One-Week Campaign #4: Quiet Sun (to occur on disk, near center)

plan term


@ @


 name : McIntosh @  e-mail : mcintosh[at]boulder.swri.edu

contact person in HINODE team

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

 abstract of observational proposal
Our global objective is to make a detailed study of the response of the quiet solar chromosphere, transition region and corona to the constantly evolving photospheric magnetic field - these joint observations will show that there is no place in the solar atmosphere that is magnetically or dynamically quiet. With these observations we hope to gain reasonable estimates of the energy flux
through the chromosphere and lower transition region. Further, this study will allow to study the structural elements [spicules, fibrils, mottles, etc] of the chromosphere and transition region, assess the relevance/importance of magneto-atmospheric [MA] wave energy versus direct magnetic energy release in the atmosphere below temperatures at which thermal conduction becomes significant. Further, we can use these observations to investigate MA mode generation, coupling and conversion as a result of photospheric motions and their interplay with magnetic structures.

To reach the global objective we will need to make detailed measurements of the targeted magnetic environment, monitor the multitude of magneto-atmospheric waves and the radiative response of the plasma at multiple "heights" threading the atmosphere. We will perform the observations [detailed below] at chosen target locations during the WHI QS period.

 request to SOT
Solar Optical Telescope [POC:McIntosh/DeWijn]
SP: Fast Maps [0.3" spatial resolution]
1) Prior and after Observing Period Perform 100"X100" spectropolarimetric maps in Fe I 6301/6302
2) During Observing Period perform 100"x100" repeated rastering of SP.

Alternating at 15s cadence
Ca II H (3968.5 Ang) full field (100"x100"), long exposure
Gband full field (100"x100")

Choice of -
Fe I 6301 Ang. photospheric magnetograms at 10s cadence (100"x100")
Na I 5890.6 Ang. chromospheric magnetograms at 10s cadence (100"x100")
H I 6562.8 Ang. line core at 5s cadence (100"x100") -- Fibrils/Mottles : Context for Ca II H
H I 6562.8 Ang. (+/- 800mA) Dopplergrams at 10s cadence (100"x100") -- Straws and Dynamic Spicules
H I 6562.8 Ang. (+/- 400mA) Dopplergrams at 10s cadence (100"x100") -- Straws and Dynamic Spicules
Na I 5890.6 Ang. Dopplergrams at 10s cadence (100"x100")

 request to XRT
X-Ray Telescope [POC: Reeves]
Filters: Al/poly (8 sec exposure), Ti/Poly (16 sec exposure) Cadence: ~30 sec cadence
FOV: 250"x250" centered on target region [capture aspects of global connectivity]
Context: Al/poly (2048x2048, 2x2 binned), 5 thin Be (768"x384" 23sec) every ~30 minutes
Note: In the case of an active region on the sun, the long exposures can be replaced by multiple short exposures.

 request to EIS
Extreme-Ultraviolet Imaging Spectrometer [POC: Hansteen]
- 2 repeated rasters of target region "HPW004_QS_RAST_120m" at start and end of sequence.
- for one hour of each targeted run do "IUU_QS_SNS_001" sit and stare at the image center of SOT/XRT

 other participating instruments
Ground-based instruments (synoptic observations).
(Consult web page - http://web.hao.ucar.edu/~sgibson/WHI/WHI-QS.html - for
further details.)

Observation Time Period: When targets are available, likely 1600 - 2000 UT or 2000 - 2400 UT.  See main campaign page (http://ihy2007.org/WHI/targeted_plans.shtml) for details and updates.

Operational Considerations: The ground based observations critical to this study are based in SW Mainland US and Hawaii. At NSO/SP the prime seeing time is 14:00-18:00 UT and is 18:00-22:00 UT in HI. If possible an IBIS/MOTH overlap would be advantageous, but opportunities will be difficult given the 4 hour time difference. We will most likely have two observing periods per day [same target region - mostly disk center] suited to best seeing and overlap for IBIS and MOTH/COMP respectively. Observing targets will be chosen to maximize scientific return and for their diagnostic differences. For example, we hope to spend at least one day characterizing the limb of the quiet atmosphere for comparison to disk center measurements of extended structure [spicules] in the chromosphere and transition region - the limb target will also permit Alfven wave studies combining Hinode [SOT, EIS], SOHO [UVCS/SUMER] & COMP. A team member in Japan [De Wijn] will have final ability to change the target and will be based on the Hinode pointing of that day.

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