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HINODE Operation Plan (HOP)

accepted on

24-jul-2014


 HOP No.

 HOP title

HOP 0259

Detection of solar oscillations in sunspot (or plage) regions

plan term

2014/08/01-2014/08/06

@ @

proposer

 name : Su, Bai @  e-mail : sjt[at]bao.ac.cn

contact person in HINODE team

 name : T. Watanabe @  e-mail : watanabe[at]uvlab.mtk.nao.ac.jp

 abstract of observational proposal
With the 1.6m new solar telescope (NST) of Big Bear Solar Observatory, many small-scale jet-like events are detected in the intergranular space surrounding individual granules (e.g., Goode et al. 2010, ApJL, 714, L31; Yurchyshyn et al. 2011, ApJL, 736, L31). These events occur with greater frequency and appear to be directly responsible for heating of the solar atmosphere. However, Observations show that in corona the higher temperature appears in active regions (if no flares, likely in magnetostatic equilibrium) and the hottest zone is located in their cores (Aschwanden et al. 2013, Sol.Phys., 283,5). Therefore, these small-scale eruptions are likely not correlated with the heating of those active regionsf ambient atmosphere. On the other hand, it is well known that oscillations/waves in sunspots (or plages) are global and continuous, thus we believe that the shocks evolved from those waves may provide energy to heat chromosphere and corona. Motivated by this belief, we are going to carry out some coordinated observations with the instruments of NST, Hinode and IRIS to re-check the oscillations in sunspots (plages) in different layers.

 request to SOT
SOT/FG
SOT/FGIV Stokes I and V images with the field of view (164x164) and the cadence of ~30 seconds at Na I D 5896 IVDG }160mÅ to obtain line-of-sight magnetograms and Dopplergrams of the photosphere.

SOT/SP
Fast map mode: 0.32"/pixel, 3.2 sec integration. The vector magnetograms  with the field of view of  82"x 82" at the cadence of ~15 min are used to compare with NST InfraRed polarization observations.

 request to XRT

 request to EIS
EIS Study - 349
ACRONYM madj_ar_small
TITLE Active region small raster
TARGET Active Region
NO. OF RASTERS 1
NO. OF POINTING POSITIONS 12
SCAN STEP SIZE (arcsec) 2
NO. OF WINDOWS 12
WINDOW WIDTHS (pixels) 80,40,40,56,40,40,40,40,40,40,40,40
WINDOW HEIGHT (pixels) 248
SLIT/SLOT 2"
EXPOSURE TIMES (ms) 15000
EXPOSURE DELAY (ms) 0

Line List
Line Wavelength (Angstroms)
FeX 184.54
FeVIII 186.70
FeXI 188.23
CaXVII 192.82
FeXII 195.12
FeXIII 202.04
FeXIII 203.80
HeII 256.32
FeXXIII 263.76
FeXIV 274.20
SiVII 275.67
FeXV 284.16

 other participating instruments
The BFIs at the New Solar Telescope (NST) and adaptive optics (AO) in Big Bear Solar Observatory, CA, USA. BFIs will follow a same target region on each day, with HeI 1083 nm, Ha and TiO 706 nm (90" x 90" FOV, 5-10 sec cadence).

 remarks
-- Observing time of 17 UT - 21 UT
-- The longitudinal magnetic component has the highest priority.
-- We will use simultaneous AIA/SDO and IRIS observations.
-- In addition, combing with HMI/SDO observations, we may utilize the high-resolution vector magnetograms of Huairou Solar Observing Station in both photosphere and chromosphere to study evolution of solar active regions in several days.

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