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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0074

Search for photospheric/chromospheric drivers of chromospheric penumbral micro-jets

plan term


@ @


 name : Katsukawa and Bellot Rubio @  e-mail : yukio.katsukawa[at]nao.ac.jp

contact person in HINODE team

 name : Katsukawa @  e-mail : yukio.katsukawa[at]nao.ac.jp

 abstract of observational proposal
HINODE SOT found sub-arcsec chromospheric activities, penumbral microjets, in sunspot penumbrae. Their very dynamical nature suggests that they are possibly driven by magnetic reconnection in the uncombed magnetic field configuration of penumbral filaments. The purpose of this observation is to detect a possible signature of sudden change of photospheric magnetic fields using Hinode SOT and the Fabry-Perot imaging spectro-polarimeter newly installed to SST at La Palma.

So far, their temporal evolution and apparent velocity have been studied only using image sequences taken through the CaII H filter. It is important to directly measure velocities with Dopplergrams of chromospheric spectral lines. For this purpose, SOT can provide Dopplergrams in Na D with  CaII H imaging. Diagnostic by SP is also important to know magnetic configuration around the footpoints of penumbral microjets.

Another important question is what the transition region and coronal response to the penumbral microjets is. EIS and XRT observations together with SOT are essential to know the coronal and transition region response.

(ref. Katsukawa et al. 2007, Science 318 (5856), 1594-1597)

 request to SOT
Combination of FG and SP observation is rqeusted. If enough telemetry amount
is not allocated to the observation, either FG or SP is used.

(1) CaIIH (exp 300msec), 704x1632 2x2, 1.6sec cadence   ->  350Mbits/15min
(2) CaIIH (exp 300msec) + G-band, 704x1632 2x2, 16sec cadence -> 360Mbits/1hour
(3) CaIIH (exp 300msec) 704x1632 2x2 + MgIb DG+-116mA (ObsID:80)
    512x1024 2x2, 16sec cadence -> 210Mbits/1hour

(1) Normal map, 12 slit pos, half height, one side
   (1.9" x 82", 1min cadence) -> 420Mbits/hour
(2) Normal map, 512x512, one side
   (82" x 82",  ~43min) -> 290Mbits/map

(Observation of faculae as a backup)
 BC+GC+RC 1024x1024 1x1, 1min cadence -> 280Mbits/1hour
 Normal map, 512x512, one side
 (82" x 82",  ~43min) -> 290Mbits/map

 request to XRT
Al/Poly + Thin-Be, 512x512, 30 - 60sec cadence (depending on the telemetry
situation). Low cadence G-band images are helpful for alignment with SOT.
Telemetry rate: TBD

 request to EIS
YK_AR_50x384 (1" slit, 20sec exp, FOV 50"x384", duration ~20min)
Repeating the study for ~2 hrs produces 17Mbits x 6 ~100Mbits.

ACRONYM: YK_AR_50x384 (Study ID: )
This active region study is intended to capture penumbral micro-jets and their counterparts in the transition region and the corona.

Spectral windows cover cool lines as well as hot lines.
T < 6.0 : He II 256.32, O V 248.46, Mg VI 268.99, Fe VIII 186.60
T = 6.2 : Fe XII 195.12/186.88, Fe XV 284.16
T  6.4 : Fe XVII 254.87, Fe XXIV 255.11

TARGET: Active region
RASTER: Scanning
SLIT:  1"
FOV: 50"x384"
Compression: JPEG90
Volume per raster: 17 Mbits
Volume/hour: 52 Mbits/hour

Penumbra of active region sunspots.
Align EIS FOV with SOT.

Repeat this raster for two hours or more. It is essential to get SOT Ca II H filtergram to study penumbral micro-jets.


 other participating instruments
SST at La Palma

[Time window] Good seeing condition is expected between 8UT and 12UT at La Palma. Minimum duration is 2 hours (9UT-11UT) every day.

[Target] Penumbra in a sunspot. The detailed pointing will be informed to COs  
from POCs everyday. When there is no sunspot during the campaign, we will  
switch the target to faculae in QS. In this case, the supports from XRT and EIS
are not indispensable.

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