HINODE observation :Solar Wind

Takeru K. Suzuki(Physics dept., Nagoya University)

Outline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Solar Winds
65Rs=0.3AU

HeatingAcceleration
Yohkoh/SXTFast Wind from Polar Coronal Holes
Quasi-steady Component

Slow Wind from ? (Streamer ?)Outline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Outline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Open flux tubes near Active Regions
Sakao et al.2007_EIS obs by Harra et al~>100km/s at ~1.1Rsun

Plage near Active Regions
Imada et al.2007 (EIS)_~>100km/s in the low corona (<<2 Rsun)

Solar Wind Simulation
Suzuki & Inutsuka 2005
_Difficult to explain >100km/s at << 2Rsun
Other 1D models (Cranmer & van Ballegooijen 2007; Verdini & Velli 2007) : SameOutline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Polar Jets
Cirtain et al.2007_Outflows~800km/s(~Alfven speed; Initial Phase)~200km/s(~Sound Speed; Frequently Observed so far)Wave propagation as well

Polar Jets
Kamio et al.2007_Blue shift with ~ 30km/s=> up to~300km/s with LoS effectDifficult to explain by 1D Solar Wind Calculations

2D Simulations
Nishizuka et al.2008_Mass Loss Rate from ‘New Generations’Open Flux Tubes near Active Region :1/4 of Total (possibly)
Sakao et al.2007

Polar Jets :1/10 of Total
Cirtain et al.2007

Other Regions ? Coronal Holes<=> ’Classical’ solar winds (Old Generation)

Outline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Polar Coronal Holes
Observation by EIS (Tian et al.2010)

Polar Coronal Holes -cont.Blue (& Red) Shifts for Different Temperature (Tian et al.2010)

Fine Structure => Smooth Structure as T increases

Polar Coronal Holes -cont.-(Tian et al.2010) LoS effect is taken into account~30km/s at Low Coronal Height :Slower than Sakao Event & Polar Jets
Consistent with 1D solar wind calculations

Solar Wind Simulation
Suzuki & Inutsuka 2005
_Outline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Alfven Wave at Photosphere
Fujimura & Tsuneta 2009 (from Fujimura’s presentation)_Correlation of B & v => Direction of Alfvenic Waves

Alfven Wave at Photosphere -cont.Fujimura & Tsuneta 2009 (from Fujimura’s presentation)_Observed Region of SP

19:15(UT)
2."1

19:36

19:57

20:18

I VI VI V

Obtain Correlation of, Intensity, B, & v
Pores & Intergranule Magnetic Concentration

Alfven Wave at Photosphere -cont.-

Phase correlation of dB & dv : (+/-)90 deg.
=> Upward component ~ Downward component

Dissipation of Alfven Waves(Wave Action Normalized at 1.02Rs for Superradial Expansion of Flux Tube)
Suzuki & Inutsuka 2005, ApJ, 632, L49_85% is reflected back before reaching corona(Qualitatively) Consistent with Fujimura & Tsuneta

Alfven waves in Corona? (Nonthermalbroadening)
Banerjee et al.2009_Consistent with non-dissipative Alfven waves<=> Simulations

Alfvenic Wave-driven Spicules
Matsumoto & Shibata 2010
_Photospheric Motion from SOT => Spicules

Outline
Upward Motion (Direct observation of flows)
Open Flux Tubes near Active Regions (New Generation)
EIS (Imada et al.2007; Hara et al.2008; Harra et al.2008)
XRT (Sakao et al.2007)

Polar Jets (New Generation)
EIS (Kamio et al.2007)
XRT (Cirtain et al.2007; Shimojo et al.2007)

Upward Motions in Polar Coronal Holes (Old Generation)
EIS(Tian et al.2010)

Alfven(ic) motions (Energy Source)
SOT (Phase correlation of B & v) (Fujimura & Tsuneta 2009)
EIS (Nonthermal Broadening) (Banerjee et al.2009)

Configuration of Magnetic Field (Environment)
Poles (Tsuneta et al.2008)
Active Regions (Harra et al.2008)

Flux Tube
Tsuneta et al.2008, ApJ, 688, 1374

Suzuki 2006, ApJL, 640, L75

SolarWind
fmax
Gravity
Gas
Pressure
Alfven Waves(Poynting E)

kG patches~1000 times super-radial expansion

Consistent with the flux tubes adopted in the solar windcalculations

Summary
Observation of Flows
Near-Active Regions & Polar Jets (New Generations)High Speed near Surface
Coronal Holes (Old Generations)
Consistent with ‘Classical’ Solar Wind Calculation

Observation of Energy Source (Poynting Flux)
Alfvenic Motions at Photosphere
Downward Comp ~ Upward Comp: Reflected Waves
Nonthermal Broadening in Corona
Coinsistent with Nondissipative Alfven Waves

Observation of Environment (B-Field Configuration)Pole(s): Super-radial Expansion of Open Flux Tubes

Missing:
Simultaneous Observations of Flow, Poynting Flux, & B-field
EnvironmentA vs. B
Option A
Flows & Velocity Profile in Various Regions
Large-scale Structure of Solar Winds
Option B
Propagation / Reflection / Dissipation of Alfvenic Waves in
Chromosphere & Transition Regions (Phase Correlation ofB,v,Intensity)
Details of Density and Velocity Structure at Low Corona