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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0198

Hinode-NST joint studies of magnetoc diffusion in Coronal Holes

plan term


@ @


 name : Abramenko @  e-mail : avi[at]bbso.njit.edu

contact person in HINODE team

 name : Berger @  e-mail : berger[at]lmsal.com

 abstract of observational proposal
We plan a study of magnetic flux dispersal in the solar photosphere. Properties and mechanisms of the flux dispersal can be used as important constrains and clues for dynamo theories. Large-scale dynamo models essentially depend on the flux transport models, which require the magnitude of diffusivity of about 600 km^2/s on supergranular scales, which is 2-3 times higher than observed diffusivity. Local turbulent dynamo, to be successful in generation of small-scale flux tubes, requires very small magnitudes of diffusivity on small scales.  Observational and model data for the entire spectrum of diffusivity on all scales are definitely required now to make a further step in understanding of the solar magnetism.

A combination of New Solar Telescope (NST) and Hinode SOT magnetograms and filtergrams will enable significant progress in understanding magnetic flux dispersal over the solar surface.

We will use this data to detect and track magnetic elements (Hinode/FG
magnetograms) and bright points (NST/TiO, G-band, Hinode G-band).

We will extend this study on all types of magnetic configuration and we want to start with coronal holes, where the numbers of bright points is not high, so the analysis may be a bit simplier.

 request to SOT
Hinode SOT G-band and Ca II H Requirements

Hinode G-band observations will be comlementary to hight resolution NST TiO and G-band images. We need 1 min or shorter cadence data.

Hinode SOT FG observations

I and V Stocks parameters measured in Na I 5896A spectral line. The 60 sec cadence is preffered, lower cadence 120 s could be acceptable.

 request to XRT

 request to EIS

 other participating instruments

Since we are only interested in Hinode G-band and FG magnetograms, we hope that higher cadence data could be acquired.

Dates and Time period of proposed joint observations

We ask for about 4 hours per day for 5 days during August 2011.
Target is a north or south low latitude (<30 deg from the equator) coronal hole. The joint campaign should start when the CH is about 30 deg east of the meridian.

BBSO experiences best seeing during our morning ours, therefore we would
strongly prefer our coordinated observations to be within the following window: 17:00UT - 21:00UT.

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