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SSyynneerrggyywwiitthhHHiinnooddee SSOOTT//SSPP
Toshifumi Shimizu(ISAS/JAXA)
2018/2/27 1
DKISTCSPWorkshopatNagoyaUniversity
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SolarOpticalTelescope(SOT)
XRT
Hinode
2
EIS
2018/2/27
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5500ccmmaappeerrttuurreetteelleessccooppee,,00..22--00..33””aarrccsseecc
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SSOOTTSSppeeccttrroo--PPoollaarriimmeetteerr ((SSPP))• Scanningslitspectrographforpolarimtetry.
• StokesIQUVprofilesoftwoFelinesat630nm
SPSpecificationsSlitwidth 0.16”Spectralresolution 30 mASpectral sampling 21.5mAFOV(slit) 164”(N-S)maxFOV(scan) 320”(E-W)max
(Tsuneta etal.2008;Lites etal.2013)2018/2/27 4
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FFlleexxiibblleeiinnmmaappppiinnggMode ofoperation Normal Fast Dynamics Deep
Timeperposition 4.8s(3rots)
3.2s(1+1rots)
1.6s(1rot)
12.8s(upto 8rots)
Polarimetric S/N 10^3 1.15 x10^3 580 >10^3
Samplingalongslit 0.16” 0.32” 0.16” 0.16”
FOValongslit 164”(max) 164”(max) 32”(max) 164”(max)
Slit-scan sampling 0.16” 0.32” 0.16” 0.16”
Slit-scanFOV 320”(max)wide
Timeformaparea(1) 83minfor160”wide
30minfor160”wide
50sfor1.6”wide
18sfor1.6”wide
18sfor1.6”wide
130sfor1.6”wide
Datarate 191kpix/s 127kpix/s 120kpix/s 73kpix/s
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MMaappddaattaavvoolluummee• 2500-3500Mbits perdayforSP,dependingontheresourceavailable.
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FOV Data Duration Datavolume320”x164” 2000x(1024x112x1x4) 166min 2280Mbits
164”x164” 1024x(1024x112x1x4) 85min 1160Mbits
123”x123“ 768x(768x112x1x4) 64min 660 Mbits
82”x82” 512x(512x112x1x4) 43min 290Mbits
19”x82” 120x(512x112x1x4) 10min 68Mbits
3.8”x82” 24x(512x112x1x4) 2min 14Mbits
FOV Data Duration Datavolume320”x164” 1000x(512x112x1x4) 60min 600Mbits
164”x164” 512x(512x112x1x4) 31min 310Mbits
123”x123“ 384x(384x112x1x4) 23min 170 Mbits
82”x82” 256x(256x112x1x4) 15min 77Mbits
20”x82” 64x(256x112x1x4) 4min 19Mbits
5.1”x82” 16x(256x112x1x4) 1min 5Mbits
Normalmap(0.16”pix)
Fastmap(0.32”pix)
http://hinode.nao.ac.jp/en/for-researchers/instruments/sot/operation/
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DDKKIISSTTiinnssttrruummeennttss
• FeI630nmcommonlymeasuredbysomeDKISTinstruments
ViSP=VisibleSpectro-Polarimeter
VTF=VisibleTunableFilter2018/2/27 7
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HHiinnooddee SSPP–– DDKKIISSTTccoollllaabboorraattiioonnss• ”Initial”phase
• Characterizingthepolarimetric behaviorsofDKISTspectropolarimeters toachievehighpolarimetric accuracy.
• Science!• Forexample.imagingandspectroscopicinstruments(Visiblebroadbandimager,Visibletunablefilter)withHinode SP
• Followedby(chromospheric)spectropolarimeters(CryogenicNiR SP,Diffraction-limitedNiR SP)
• Hinode SPAdvantages• High-accuracydatafromseeingfreecondition• Coveragefor24hours,thoughthecadenceof2-3hours• Possibletohavealargerfieldofview
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DDyynnaammiiccCChhrroommoosspphheerree
Hinode/SOTGà CaIIH2018/2/27 10
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Sunspot light bridgesLong-lasting chromospheric plasma ejections
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SP LOS velocityCurrent Jz CaIIH
8:57:56
9:14:57
SP scan at 8:56-8:59
0.7km/s
(Shimizu et al. 2009, ApJ, 696, L66)(Shimizu 2011, ApJ, 738, 83)
26-180km/s
Behaviors supporting MR• Bi-directional flows• Enhanced current along the apex
of the LB
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Sunspot light bridgesLong-lasting chromospheric plasma ejections
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SP LOS velocityCurrent Jz CaIIH
8:57:56
9:14:57
SP scan at 8:56-8:59
0.7km/s
(Shimizu et al. 2009, ApJ, 696, L66)(Shimizu 2011, ApJ, 738, 83)
26-180km/s
Behaviors supporting MR• Bi-directional flows• Enhanced current along the apex
of the LB
ejections
Helicalweakmagneticfluxtubeembeddedalonglightbridge
Magneticfieldandvelocitymeasurementsatthechromosphere coordinatedatthephotosphere
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CChhrroommoosspphheerriicc jjeettss
• Multiplebright,plasmaejectionsalongjets,showingtime-dependent aswellasintermittent natureofMRinchromosphere
• Howmuchenergyistransportedupward?2018/2/27 13
(Shibata+07)
Collisionless,fullyionized,lowb
Collisional,weaklyionized,b~1
HinodeSOTCaIIH
(Singhetal.2012ApJ)
(Shibata+2007)
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High cadence observations
Parameter Wavelength Cadence FOVHinode/SP IQUV FeI 27sec 3.8” x61”
IRIS I MgII,Si IV,OIV 3sec 0.3”x31”
HinodePhotosphere
IRISChromosphere
Lower TR
AR11836
Hinode
IRIS
(Kanoh etal.2016)
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DKIST
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Magnetic fieldVelocity Intensity
Example: High cad SP movie
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Comparison between the photosphere and chromosphere
・Sawtooth pattern in IRIS plot→ Signature of shock formation at the chromosphere・Higher frequency waveforms→ Leakage of high-frequency waves (>6mHz)
Hinode/SPDoppler velocity
IRIS Si IVDoppler velocity
Photosphere
Chromosphere
km/s
km/s
Time(sec)
(Kanoh etal.2016ApJ)
DKIST
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MMRRiinntthheeccoorroonnaa::SSooffttXX--rraayymmiiccrrooffllaarreess//jjeettss
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ARtransientbrightenings
SynergyalsowithHinode/XRT
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Fromphotospheric magneticinformation
• Emergence, cancellation (classical picture)• No apparent encounters at the photosphere for the half of
samples!2018/2/27 18
(Shimizu 1996 PhD, Shimizu et al. 2002, ApJ)
Hinode/XRT– Hinode/SOT
(Kano, Shimizu & Tarbell 2010, ApJ)
Yohkoh/SXT– LaPalma/SOUP
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Emergence,Cancellationand?
• No major improvement only with higher-resolution “imaging” measurements of the photospheric magnetic field
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Emerging
Reconnection
Submerging
MMF
Reconnection
Submergingpenumbra
• “Chromospheric” magnetic field and velocity measurements, to explore the events which origins have not yet been identified.
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DynamicchromosphereincomputersMartinez-Sykora etal.2017Science
Strongambipolar diffusioninanexpandingemergingfluxbubbleconcentratestheperpendicularcurrentattheedgesofthebubble. 20
PhotosphereChromosphere
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Summary
• Hinode SOTspectro-polarimeter willsupportDKIST,notonlycalibrationbutalsoscience.
• Especially,scienceatInitialperiodreallyneedHinode SP.
• Hinode XRTwillbealsoanimportantinstrumentforstudiesoncoronalmicroflares andjets.
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