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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0233

A Detailed Magnetic and Thermal Study of an Active Region

plan term


@ @


 name : White @  e-mail : white[at]astro.umd.edu

contact person in HINODE team

 name : SSC @  e-mail :

 abstract of observational proposal
I have been awarded observing time with the Very large
Array to image at high resolution a solar active region over a wide and continuous frequency range (2-12 GHz). The radio data are sensitive both directly to the coronal magnetic field as well as to the coronal plasma that produces the solar EUV flux. This will be the first VLA data set with such complete frequency coverage of an active region.

In order to build a complete picture of the active region, I request a scan with SP in order to generate a
vector magnetogram in the photosphere that can be used for a nonlinear force-free extrapolation of coronal fields, and a scan with EIS at a selection of Fe lines in order to build up a spatially-resolved picture of the thermal emission in the corona, and to permit an abundance measurement.
Since there is no intent to study time evolution in this project, single scans are all that is required and data volumes are low. KD Leka is likely to be able to help with the SP analysis.

 request to SOT
SOT/SP (first priority).

A single SP "normal map" over 164" x 164" in Fe I 5250 for a photospheric vector magnetogram

Data volume: 1160 Mbits

 request to XRT

 request to EIS
EIS (2nd priority).

A single EIT raster covering sufficient Fe lines to sample the full coronal temperature range of active regions. Study 377 (cam_ar_limb_lite_v2) would be acceptable, but I am open to alternative suggestions.

Data volume: 186 MBits

 other participating instruments

Time period of proposed observations: single date likely to be on the first weekend in August (Aug 3-4; currently being negotiated with VLA schedulers)

Time window in day: anywhere within the likely VLA observing window in the US daytime: noon at the VLA is at 19 UT, so anywhere within the 16-22 UT window. Interruptions are acceptable, and observations within 24 hours are acceptable if the schedule does not permit the 16-22 UT window.

Target of interest: single active region to be chosen several days in advance, likely the largest active region on the disk at the time of observing.

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