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HINODE Operation Plan (HOP)

accepted on

19-dec-07


 HOP No.

 HOP title

HOP 0058

CORE/TOO: Measuring coronal outflows in coronal loops

plan term

2008/01/01-2008/01/31
2008/02/01-2008/02/28

@ @

proposer

 name : P. R. Young @  e-mail : P.R.Young[at]rl.ac.uk

contact person in HINODE team

 name : P. R. Young @  e-mail : P.R.Young[at]rl.ac.uk

 abstract of observational proposal
Doschek, G.A., Mariska, J.T., Warren, H.P., et al., 2007, ApJ, 667, L109
Sakao, T. , Kano, R., Narukage, N., et al., 2007, Science, 318, 1585
In order to investigate the time variability of the outflows, it is essential to obtain a long, continuous set of observations. We thus make the following special observing requests:  • for each of the six days, a single, complete 24 hour observing run is made; • to minimize disruption of the sequence, we request only 2 XRT synoptics each day; • the observation begins at the start of a single upload plan on Day 1, and ends at the end of the Day 6 upload plan (so that the modified DR allocations only affect six Hinode planning days) • if the instruments have particular engineering or calibration sequences that must be run during the 6 day period, then we request that the instrument teams schedule them for the same time slot to minimise any disruption to the coordinated data-set

 request to SOT
SOT data are vital for identifying the photospheric and chromospheric roots of the loop footpoints, and measuring the vector magnetic field. Repeated Spectro-Polarimeter (SP) observations are requested over a spatial region of 180hx164h over the duration of the program, interspersed with BFI images in G-band, Ca II and H-alpha (focus optimised for Ca II).

 request to XRT
A high cadence dynamics study using one filter and a 512x512 pixel field of view should be used. The filter should have some sensitivity to cool plasma, and we suggest Ti-poly. Every 10 minutes, single images in one or more different filters should be used to allow the temperature structure of the loops to be derived.

 request to EIS
EIS will run the study PRY_footpoints_HI which is identical to the well-used PRY_footpoints_v2 study except that the raster covers 512h in Y instead of the current 240h. This accounts for the increased share of the data recorder for EIS. The increased field of view in Y allows EIS to access quiet Sun areas that can be used as a reference to fix the wavelength scale for velocity determinations.

Notes for EIS CO: the study should be scheduled in two 12 hour blocks each day. The block should begin with a context study PRY_slot_context (duration 3 minutes), and then PRY_footpoints_HI should be repeated to fill the block. For the following blocks, make sure to use the same mirror position (MIP) as the previous block to ensure that PRY_footpoints_HI is pointed in exactly the same place each time. Check with David Williams or David Brooks if you are not sure how to do this.

 other participating instruments
SOT data are vital for identifying the photospheric and chromospheric roots of the loop footpoints, and measuring the vector magnetic field. Repeated Spectro-Polarimeter (SP) observations are requested over a spatial region of 180hx164h over the duration of the program, interspersed with BFI images in G-band, Ca II and H-alpha (focus optimised for Ca II).

 remarks
Target/Pointing: A well-developed active region close to disk centre. The target will be the base of large loop structures found near the edge of the active region (see Figure 1 above). The SOT pointing should be at the footpoints of the loops. E.g., in Figure 1 the centre of the SOT field of view would be approximately (-360,-50).
Duration: 6 days x 24hrs
Data rate allocation: Our solution for this HOP is to allocate a greater share of the data recorder (DR) to EIS, thus allowing greater spatial coverage and retaining wide spectral coverage. The normal EIS DR allocation is 15%. For this specific study we request 32% (see below for justification). XRT will have the usual 15%, and SOT will be reduced to 53%.

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