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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0133

Joint observation with SST - I. fine structures in sunspot, II. type-II spicule-

plan term


@ @


 name : Watanabe, H., Carlsson @  e-mail : watanabe[at]kwasan.kyoto-u.ac.jp

contact person in HINODE team

 name : Watanabe, H. @  e-mail : watanabe[at]kwasan.kyoto-u.ac.jp

 abstract of observational proposal

To study the phenomena of magnetoconvection, such as umbral dots and  penumbral filaments

<Scientific background>

The fine structures in sunspots, such as umbral dots, penumbral filaments, andlight bridges, are vigorously studied using the SOT data.  The origin of these fine structures are known to be the magnetoconvection.  Investigating the actual phenomena of the magnetoconvection is highly of interest in the viewpoint of the MHD simulation and physics in the accretion disk and low T stars.  Watanabe et al. (2009) suggested the possibility that the oscillatory  
convection may occur in umbral dots, which could be clarified by Hinode high cadence, high resolution data.  Investigating the proper motion of such phenomena is also important for understanding the interaction between magnetic field and plasma.

We are planning to perform a multiple line scanning of a sunspot with the SST/TRIPPEL.  The targets are the center of the umbra (umbral dots) and the boundary of the penumbra (light bridges, penumbral filaments).  The Fe I 557.6 nm and Ca IR 854.2 nm are the promising candidates.  These lines offers complimentary information between the Hinode, because the Fe I 557.6 nm is suitable for the bisector velocity analysis at the photosphere, and Ca IR 854.2 nm is good for investigating the dynamics of the photosphere to the chromosphere.

Target II. Type II spicules


To find the disk counterpart of type II spicules (De Pontieu et al. 2007).

<Scientific background>

De Pontieu et al. (2007) found two types of spicules; TypeI -spicules by shock  waves and Type-II picules by magnetic reconnection.  Especially, the type II spicule was newly found by Hinode and the thorough investigation of its properties is in progress now.  The study of the type II spicules is important in the viewpoint of transferring the heat to the corona.  We want to find the disk counterpart of type II spicules, with collaborative observation at SST/
TRIPPEL spectrograph (Ca II H) and Hinode.  We also do spectroscopy above the limb to determine the width of the emission and look for the absorption close to the limb of type II spicules.  As the time scale of the spicules is very short (10-150s), very high cadence images is necessary, in addition to the small region scanning by EIS and coronal temperature imaging by XRT.

 request to SOT
BFI (blue continuum)  55" x 55" 1x1 sum, 15 sec cadence -> 280 Mbits/1H
BFI (Ca II H) 55" x 55"1x1 sum, 15 sec cadence -> 280 Mbits/1H
SP (Fast map)  82"x82", 1x1 sum, 1 side CCDs -> 100 Mbit/1H

Note: At the beginning of the FG observation please run SP map once. If the telemetry allows, we want to request another SP map at the end of the FG observation. If the telemetry is not enough, please change the BFI summing to 2x2.

<no request for XRT and EIS>

BFI (G band) 55" x 55"1x1 sum, 2 min cadence  -> 50 Mbits/1H
BFI (Ca II H)  55" x 55"1x1 sum, 10 sec cadence -> 420 Mbits/1H
NFI (NaD)   55" x 55"1x1 sum, 2 min cadence -> 120 Mbits/1H

Note: If the telemetry is not enough, please omit G band and NaD, and next change the Ca II H summing to 2x2.

 request to XRT
thin-Al-poly and thin-Al-mesh, covering SOT and EIS FOV, 2 min cadence or lower

 request to EIS
High cadence slot observations with minimum FOV of 55" x 55"

 other participating instruments

Time period of proposed observations 2009/10/08-2009/10/21
Time window in day: 08:00-11:00UT, 15:00-18:00UT
Minimum duration is 2 hours (08:00-10:00UT) every day.

Target of interest
Sunspot (TOO) or pores (TOO), active region (TOO) or magnetic concentration regions on disk (theta < 45 degree), and limb)

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