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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0178

Investigation of Dynamics of pores at photosphere and chromospheres with Hinode and NST/FISS observations

plan term


@ @


 name : Cho @  e-mail : kscho[at]kasi.re.kr

contact person in HINODE team

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

 abstract of observational proposal
Solar pores are premature small sunspots. Cho et al. 2010 investigated the temporal variation of several tiny pores smaller than 2h at photosphere using Hinode/SOT and found that downflows always exist inside and around pores and the speed of downflows inside the pores is negatively correlated with their darkness. It is also found that the pores in the growing phases are associated with the converging flow pattern, and the pores in the decay phase are associated with the diverging flow pattern. Based on the photosphere observation using Hinode/SOT, they concluded that a pore grows as magnetic flux density increase due to the convergence of ambient mass flow and it decays with the decrease of the flux density due to diverging mass flow.
Meanwhile, Lagg et al. 2007 took a chromospheric observation in the vicinity of a growing pore. They analyzed spectropolarimetric data in He I 1083 nm obtained by VTT/TIP at Teide observatory and found a redshifts (> 40 km/s) in the vicinity of a growing pore. They interpret this downflow as a consequence of a draining of the rising loops.
Recently, SNU and KASI installed Fast Imaging Solar Spectrograph (FISS) in the Cude room of the 1.6 m New Solar Telescope at Big Bear Solar Observatory. FISS can do imaging of H-alpha and Ca II 8542 band simultaneously, which is quiet suitable for study of dynamics of chromosphere.
Our main science objective is to find relationship of horizontal motion inside and around pores at photosphere with their vertical motions both at photosphere and chromosphere. For this we propose a joint observation between NST/FISS and Hinode/SOT from October 25 to October 29, 2010. Our observation targets are pores at active region and miniature of pores (magnetic knots) at quiet region near disk center, respectively. Through this observation, we expect to find difference between the pore at active region and very tiny pores at quiet region.

 request to SOT
-  Observation time should be same as the NST/FISS observation time
-  Target: Pores at active region near Disk Center and miniature of pore at Quiet region(~ 1h)

Ca II H /G-band
FOV: FDB 89 (1408x1408 2x2, 77hx 77h)
Time Cadence: 30 sec
Data rate: ~300Mbits/hour

Normal map, 1 side
FOV: 512x512 (82hx 82h, 43min)
Time Cadence: Two maps for 3 hours
Data volume: 290x2 = 580 Mbits

When we run the observation for 3 hours, the total data amount is estimated to be about 1.5 Gbits.  

 request to XRT

 request to EIS

 other participating instruments
- H alpha line, Ca II 8542
- Exposure time : 1) 30 ms for Ha ; 2) 60 ms for Ca II 8542
- Step size: 0.16h
- Slit width : 0.16h
- Binning along the slit direction: 2 (effective pixel size = 0.16)
- Number of steps = 100 and 300
- Expected time interval between successive scan is 20sec and 60sec
- Field of view
: (0.16h * 100) by (0.16h * 250) = 16h * 40 g
: (0.16h * 300) by (0.16h * 250) = 48h * 40 g
- Expected total observing duration = 50 min

- Time period: Our observation proposal for NST/FISS will be accepted by BBSO. Our observation will be executed Oct 25 to Oct. 29. We may need communication with BBSO people before observation to targeting of telescope.
- Time window : 17:00 - 20:00 UT (09 - 12 EST)  
- Target of interesting : Pores at disk center

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