SSyynneerrggyywwiitthhHHiinnooddee SSOOTT//SSPP

Toshifumi Shimizu(ISAS/JAXA)

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DKISTCSPWorkshopatNagoyaUniversity

SolarOpticalTelescope(SOT)

XRT

Hinode

2

EIS

2018/2/27

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

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/

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

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

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

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)

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

Magnetic fieldVelocity Intensity

Example: High cad SP movie

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

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

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.

DynamicchromosphereincomputersMartinez-Sykora etal.2017Science

Strongambipolar diffusioninanexpandingemergingfluxbubbleconcentratestheperpendicularcurrentattheedgesofthebubble. 20

PhotosphereChromosphere

Summary

• Hinode SOTspectro-polarimeter willsupportDKIST,notonlycalibrationbutalsoscience.

• Especially,scienceatInitialperiodreallyneedHinode SP.

• Hinode XRTwillbealsoanimportantinstrumentforstudiesoncoronalmicroflares andjets.

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