コロナ加熱・太陽風駆動機構でこれまで分かったことと，未解明問題
Solved & Unsolved Problems in theCoronal Heating & the Solar Wind
Acceleration
鈴木 建 (Takeru K. Suzuki)
名古屋大学 理 物理 (Physics Dept., Nagoya University)

Sep.13th, 2014

What to be clarified

What to be clarified
Energy/Momentum/Mass transfer
in the atmosphereWhat to be clarified
Energy/Momentum/Mass transfer
in the atmosphere
1 Extract the kinetic
energy of the surface
convective turbulenceWhat to be clarified
Energy/Momentum/Mass transfer
in the atmosphere
1 Extract the kinetic
energy of the surface
convective turbulence
2 Lift up the energy toupper layers

What to be clarified
Energy/Momentum/Mass transfer
Tin the atmosphere
Radiation
1 Extract the kinetic
Conduction
NuclearWind
Reactionenergy of the surface
convective turbulence
2 Lift up the energy to
Convection
Zone
upper layers
Photospherer
3 The energy dissipates at
In Situ Heating
appropriate locationsin the Corona & Wind

What to be clarified
Energy/Momentum/Mass transfer
Tin the atmosphere
Radiation
1 Extract the kinetic
Conduction
NuclearWind
Reactionenergy of the surface
convective turbulence
2 Lift up the energy to
Convection
Zone
upper layers
Photospherer
3 The energy dissipates at
In Situ Heating
appropriate locationsin the Corona & Wind
“Type II spicule” (De Pontieu+ 2011): Direct supply of hot gas

What to be clarified
Energy/Momentum/Mass transfer
Tin the atmosphere
Radiation
1 Extract the kinetic
Conduction
NuclearWind
Reactionenergy of the surface
convective turbulence
2 Lift up the energy to
Convection
Zone
upper layers
Photospherer
3 The energy dissipates at
In Situ Heating
appropriate locationsin the Corona & Wind
“Type II spicule” (De Pontieu+ 2011): Direct supply of hot gas: negligible contribution• need heating against the adiabatic loss (e.g. Klimchuk 2011)• IRIS observed falling back of Type II spicules (Pereira+ 2014)

Energy Transfer
Energy( Flux= ρ3∥)

32 /2 + h − GM/r

+ 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π

h: enthalpy

Energy Transfer
Energy( Flux)= ρ3∥ 32 /2 + h − GM/r + 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy• K.E.= Kinetic Energy• T.E.= Thermal Energy• G.E.= Gravitational Energy• P.F.= Poynting Flux

Energy Transfer
Energy( Flux)= ρ3∥ 32 /2 + h − GM/r + 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy• K.E.= Kinetic Energy• T.E.= Thermal Energy• G.E.= Gravitational Energy• P.F.= Poynting Flux
1

K.E.

Energy Transfer
Energy( Flux)= ρ3∥ 32 /2 + h − GM/r + 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy• K.E.= Kinetic Energy• T.E.= Thermal Energy• G.E.= Gravitational Energy• P.F.= Poynting Flux

K.E.
2 K.E.⇒ P.F.
1

Energy Transfer
Energy( Flux)= ρ3∥ 32 /2 + h − GM/r + 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy• K.E.= Kinetic Energy• T.E.= Thermal Energy• G.E.= Gravitational Energy• P.F.= Poynting Flux

K.E.
2 K.E.⇒ P.F.
3 P.F.⇒ T.E.
1

Energy Transfer
Energy( Flux)= ρ3∥ 32 /2 + h − GM/r + 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy• K.E.= Kinetic Energy• T.E.= Thermal Energy• G.E.= Gravitational Energy• P.F.= Poynting Flux

K.E.
2 K.E.⇒ P.F.
3 P.F.⇒ T.E.
4 P.F. + T.E.
⇒ K.E. + G.E.
1

Energy Transfer
Energy( Flux)= ρ3∥ 32 /2 + h − GM/r + 3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy• K.E.= Kinetic Energy• T.E.= Thermal Energy• G.E.= Gravitational Energy• P.F.= Poynting Flux

K.E.
2 K.E.⇒ P.F.
3 P.F.⇒ T.E.
4 P.F. + T.E.
⇒ K.E. + G.E.
1

Classification ?

Classification ?

Classification of Regions
Withbroe & Noyes (1977)
RegionCH
QS
AR
Loss(erg/cm2 s) 8 × 105
3 × 105
107
TypeWind Cond. & Rad. Rad.
Open ⇐⇒ Closed ?
CH=Coronal Holes; QS=Quiet Regions; AR=Active Regions

Classification ?
Classification of Heating• Reconnection (DC)• Wave (AC)τmotion > or < τAlf
The difference is vague–e.g. waves with short duration.

Classification of Regions
Withbroe & Noyes (1977)
RegionCH
QS
AR
Loss(erg/cm2 s) 8 × 105
3 × 105
107
TypeWind Cond. & Rad. Rad.
Open ⇐⇒ Closed ?
CH=Coronal Holes; QS=Quiet Regions; AR=Active Regions

Fluctuation at the PhotosphereFluctuation at the Photosphere• δ3⊥ in QSs by local correlation tracking

Fluctuation at the Photosphere• δ3⊥ in QSs by local correlation tracking
Matsumoto & Kitai 2010⟨δ3⊥ ⟩ = 1.1km/s(
)(
)3
ρ
δ3
8
2
F = 10 (erg/cm s) 10−7 g/cm3 1km/s
see also Tarbell+ 1990

Fluctuation at the Photosphere• δ3⊥ in QSs by local correlation tracking
Matsumoto & Kitai 2010⟨δ3⊥ ⟩ = 1.1km/s(
)(
)3
ρ
δ3
8
2
F = 10 (erg/cm s) 10−7 g/cm3 1km/s
see also Tarbell+ 1990

• δB, δ3los , & δI in pores & IMS near an AR
IMS=intergranular magnetic structure

Fujimura & Tsuneta 2009

Fluctuation at the Photosphere• δ3⊥ in QSs by local correlation tracking
Matsumoto & Kitai 2010⟨δ3⊥ ⟩ = 1.1km/s(
)(
)3
ρ
δ3
8
2
F = 10 (erg/cm s) 10−7 g/cm3 1km/s
see also Tarbell+ 1990

• δB, δ3los , & δI in pores & IMS near an AR
IMS=intergranular magnetic structure

Fujimura & Tsuneta 2009

Phase correlation δB ⇔ δ3
see also Ulrich 1996
⇒ direction of Alfvénic wave

Fluctuation at the PhotosphereFluctuation at the Photosphere• Sufficient energy in the surface convection

Fluctuation at the Photosphere• Sufficient energy in the surface convection• But, most of energy (& 90%) is reflected back.

Fluctuation at the Photosphere• Sufficient energy in the surface convection• But, most of energy (& 90%) is reflected back.
• Consistent with numerical simulations.

Suzuki & Inutsuka 2005; Cranmer+ 2007; Verdini & Velli 2007

Reflection testEnergy Transfer in Chromosphere

Energy Transfer in Chromosphere• Sufficient Energy flux(≈ (4 − 7) × 106 erg/cm2 s)
with transverse waves
via spicules.

HINODE/SOTDe Pontieu+ 2007

Energy Transfer in Chromosphere• Sufficient Energy flux

HINODE/SOTDe Pontieu+ 2007(≈ (4 − 7) × 106 erg/cm2 s)
with transverse waves
via spicules.
• But, complexities• Reflection• Short lifetime( Pw . τlife )• filling factor

HINODE/SOT obs of a CH boundary
Okamoto & De Pontieu 2011

OBS: waves with short period (.100 s)

Energy Transfer in Chromosphere• Sufficient Energy flux

HINODE/SOTDe Pontieu+ 2007(≈ (4 − 7) × 106 erg/cm2 s)
with transverse waves
via spicules.
• But, complexities• Reflection• Short lifetime( Pw . τlife )• filling factor

HINODE/SOT obs of a CH boundary
Okamoto & De Pontieu 2011

Each event seems nice,but spatial (⇔ filling factor)& time (⇔ lifetime)
OBS: waves with short period (.100 s)
integration ?

Propagation to chromosphere ?

Propagation to chromosphere ?

Alfvénic waves in prominence(Okamoto+ 2007)

Propagation to chromosphere ?

Alfvénic waves in prominence(Okamoto+ 2007)

Hiller+ 2013

Propagation to chromosphere ?

Alfvénic waves in prominence(Okamoto+ 2007)

Lines: P(3) at Photosphere• Solid: Matsumoto & Kitai 2010
• Dashed: Chitta+ 2012

Hiller+ 2013

P(3): Chromosphere – PhotospherePropagation to chromosphere ?

Alfvénic waves in prominence(Okamoto+ 2007)

Lines: P(3) at Photosphere• Solid: Matsumoto & Kitai 2010
• Dashed: Chitta+ 2012

Turbulent cascade tohigher-frequency fromphotosphere tochromosphere ?

Hiller+ 2013

P(3): Chromosphere – PhotosphereTransverse Waves in TR & Corona

Transverse Waves in TR & Corona• Spectroscopic OBSs always
suffer from the projection effect.
⇒ Tiny flux
e.g. 10(erg/cm2 s) Tomczyk+2007

CoMP/NSO

Tomczyk+ 2007

Transverse Waves in TR & Corona• Spectroscopic OBSs always

CoMP/NSO

Tomczyk+ 2007

suffer from the projection effect.
⇒ Tiny flux
e.g. 10(erg/cm2 s) Tomczyk+2007• OBS of lateral motions⇔ numerical simulation.
⇒ (1 − 2) × 105 (erg/cm2 s)
McIntosh+2011

SDO/AIA

McIntosh+ 2011

Transverse Waves in TR & Corona• Spectroscopic OBSs always

CoMP/NSO

Tomczyk+ 2007

suffer from the projection effect.
⇒ Tiny flux
e.g. 10(erg/cm2 s) Tomczyk+2007• OBS of lateral motions⇔ numerical simulation.
⇒ (1 − 2) × 105 (erg/cm2 s)
McIntosh+2011

However, Criticism

SDO/AIA

McIntosh+ 2011

Transverse Waves in TR & Corona• Spectroscopic OBSs always

CoMP/NSO

Tomczyk+ 2007

suffer from the projection effect.
⇒ Tiny flux
e.g. 10(erg/cm2 s) Tomczyk+2007• OBS of lateral motions⇔ numerical simulation.
⇒ (1 − 2) × 105 (erg/cm2 s)
McIntosh+2011

However, Criticism• a filling factor, f = 1??

FA ≈ f ρδ32 3A

SDO/AIA

McIntosh+ 2011

Transverse Waves in TR & Corona• Spectroscopic OBSs always

CoMP/NSO

Tomczyk+ 2007

suffer from the projection effect.
⇒ Tiny flux
e.g. 10(erg/cm2 s) Tomczyk+2007• OBS of lateral motions⇔ numerical simulation.
⇒ (1 − 2) × 105 (erg/cm2 s)
McIntosh+2011

However, Criticism• a filling factor, f = 1??

FA ≈ f ρδ32 3A• Simulation ??

SDO/AIA

McIntosh+ 2011

Transverse Waves in TR & Corona• Spectroscopic OBSs always

CoMP/NSO

Tomczyk+ 2007

suffer from the projection effect.
⇒ Tiny flux
e.g. 10(erg/cm2 s) Tomczyk+2007• OBS of lateral motions⇔ numerical simulation.
⇒ (1 − 2) × 105 (erg/cm2 s)
McIntosh+2011

However, Criticism• a filling factor, f = 1??

FA ≈ f ρδ32 3A• Simulation ??

Pure OBS by the same
method gives(0.9 − 2.4) × 104 (erg/cm2 s)Thurgood+ 2014

SDO/AIA

McIntosh+ 2011

Transverse Waves in Corona –contd.
SDO/AIA obs (Thurgood+ 2014)
Time-Position at Slit 1

Transverse Waves in Corona –contd.
SDO/AIA obs (Thurgood+ 2014)
Time-Position at Slit 1• The concept of reconnection(DC) vs. waves(AC) is notreasonable.

Observable Transverse Waves ??

Observable Transverse Waves ??

• Kink waves• Weakly compressive• Observable with δI

Observable Transverse Waves ??

• Kink waves• Weakly compressive• Observable with δI• Torsional waves• Incompressive• No δI

Observable Transverse Waves ??

• Kink waves• Weakly compressive• Observable with δI• Torsional waves• Incompressive• No δI

Hidden energy flux in torsional waves in fine-scale tubes ???
⇔ Observation of helicity in the corona Curdt & Tian 2011

Longitudinal Waves in Corona

Longitudinal Waves in Corona
Plenty of Observations

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)• Norikura obs. of QSs gives 15(erg/cm2 s) (Sakurai+2002)⇐ projection effect ?

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)• Norikura obs. of QSs gives 15(erg/cm2 s) (Sakurai+2002)⇐ projection effect ?
• ARs• Loop oscillation by TRACE (De Moortel+ 2000 & more)• Associated with outflows (Nishizuka & Hara 2011)• Both transverse & longitudinal waves (Kitagawa+ 2010)

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)• Norikura obs. of QSs gives 15(erg/cm2 s) (Sakurai+2002)⇐ projection effect ?
• ARs• Loop oscillation by TRACE (De Moortel+ 2000 & more)• Associated with outflows (Nishizuka & Hara 2011)• Both transverse & longitudinal waves (Kitagawa+ 2010)

Longitudinal (slow MHD) waves from thephotosphere cannot reach the corona.

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)• Norikura obs. of QSs gives 15(erg/cm2 s) (Sakurai+2002)⇐ projection effect ?
• ARs• Loop oscillation by TRACE (De Moortel+ 2000 & more)• Associated with outflows (Nishizuka & Hara 2011)• Both transverse & longitudinal waves (Kitagawa+ 2010)

Longitudinal (slow MHD) waves from thephotosphere cannot reach the corona.
⇒ These waves are excited via

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)• Norikura obs. of QSs gives 15(erg/cm2 s) (Sakurai+2002)⇐ projection effect ?
• ARs• Loop oscillation by TRACE (De Moortel+ 2000 & more)• Associated with outflows (Nishizuka & Hara 2011)• Both transverse & longitudinal waves (Kitagawa+ 2010)

Longitudinal (slow MHD) waves from thephotosphere cannot reach the corona.
⇒ These waves are excited via• Nonlinear mode conversion from Alfvénic waves
Hollweg 1982; Kudoh & Shibata 1999; Moriyasu+ 2004; Antolin+2008;
Matsumoto & Shibata 2010; Antolin & Shibata 2010

Longitudinal Waves in Corona
Plenty of Observations ⇐ observable by δI• Long-period slow waves in CHs (Ofman+ 2000 & more)• Norikura obs. of QSs gives 15(erg/cm2 s) (Sakurai+2002)⇐ projection effect ?
• ARs• Loop oscillation by TRACE (De Moortel+ 2000 & more)• Associated with outflows (Nishizuka & Hara 2011)• Both transverse & longitudinal waves (Kitagawa+ 2010)

Longitudinal (slow MHD) waves from thephotosphere cannot reach the corona.
⇒ These waves are excited via• Nonlinear mode conversion from Alfvénic waves
Hollweg 1982; Kudoh & Shibata 1999; Moriyasu+ 2004; Antolin+2008;
Matsumoto & Shibata 2010; Antolin & Shibata 2010

• Reconnections or motion of loops
Sturrock 1999; Nishizuka+ 2009; Kigure+ 2010

Outflows near ARs

Outflows near ARs
XRT obs (Sakao+ 2007)

Outflows near ARs
XRT obs (Sakao+ 2007)

Harra+ 2008

Outflows near ARs
XRT obs (Sakao+ 2007)

Nishizuka & Hara 2011;

Harra+ 2008

Hara+ 2008

Outflows near ARs
XRT obs (Sakao+ 2007)

Harra+ 2008

Blue-shifted (outflow)
regions= large non-thermal δ3⇐ Impulsive Heating?

Nishizuka & Hara 2011;

Hara+ 2008

T dependent flows

T dependent flows
EIS obs of a CH near an AR(Imada+ 2007; 2011)

T dependent flows
EIS obs of a CH near an AR(Imada+ 2007; 2011)

T dependent flows
Warren+ 2010 see also Brooks & Warren 2012

EIS obs of a CH near an AR(Imada+ 2007; 2011)

T dependent flows
Warren+ 2010 see also Brooks & Warren 2012

EIS obs of a CH near an AR(Imada+ 2007; 2011)

Taroyan & Bradshaw 2014

can be explained by OBS ofmultiple unresolved loops• Heated loops = upflows• Cooled loops = downflows

Outflows in CHs

Outflows in CHs
Tian+ 2010

5.8

6.0

log T

6.11

6.2

Outflows in CHs
Tian+ 2010

Blue-shifted (outflow)
regions gradually dominate
with T ⇑
5.8

6.0

log T

6.11

6.2

Outflows in CHs
Tian+ 2010
Shiota+ 2012

5.8

6.0

log T

6.11

6.2

Blue-shifted (outflow)
regions gradually dominate
with T ⇑⇐ Merging of super-radiallyopen flux tubes

Heating in CHs

Heating in CHs
Tsuneta+ 2008

Heating in CHs
Shimojo & Tsuneta 2009
Tsuneta+ 2008

• kG-patches (Tsuneta+ 2008; Ito+ 2010)⇔ X-ray bright points• Triggered by reconnection events?
• Excite Alfvénic waves (Cirtain+ 2007)

Heating in CHs
Shimojo & Tsuneta 2009

Kamio+ 2007

Tsuneta+ 2008

• kG-patches (Tsuneta+ 2008; Ito+ 2010)⇔ X-ray bright points• Triggered by reconnection events?
• Excite Alfvénic waves (Cirtain+ 2007)• Contribute to ∼ 10% of Ṁ of the solar wind
(Cirtain+ 2007)⇐ Estimated occurrence rate of X-ray jets

Heating in AR Corona

Heating in AR Corona
Filling factor – δ3

Heating in AR Corona
Filling factor – δ3

XRT(red)/TRACE(green)

Continuum Intensity

filling factor

δ3 from SOT/SP

Kano+ 2014

Heating in AR Corona
Filling factor – δ3

XRT(red)/TRACE(green)

Continuum Intensity

filling factor

δ3 from SOT/SP

Kano+ 2014

Heating in AR Corona
Filling factor – δ3

XRT(red)/TRACE(green)

Continuum Intensity

filling factor

δ3 from SOT/SP

Inconsistency/Consistency with
Katsukawa & Tsuneta (2005)?

Kano+ 2014

Heating in AR Corona
Filling factor – δ3

XRT(red)/TRACE(green)

Continuum Intensity

filling factor

δ3 from SOT/SP

Inconsistency/Consistency with
Katsukawa & Tsuneta (2005)?

Similar studies for QS & CH are important.

Kano+ 2014

Other Issues should be Addressed• B at Photosphere ⇔ Injection of Poynting Flux

Magnetic Field at PhotosphereΦh & Φz in QS (Ishikawa & Tsuneta 2011)

Katsukawa & Orozco Suárez 2012

δT
δ3

Iida+ 2012

Bh
Bz

Other Issues should be Addressed• B at Photosphere ⇔ Injection of Poynting Flux

Other Issues should be Addressed• B at Photosphere ⇔ Injection of Poynting Flux
• Distribution of Flare Energetics– Nanoflare heating⇒ Contribution to Coronal Heating ?
Shimizu 1995; Sakamoto+ 2009

Other Issues should be Addressed• B at Photosphere ⇔ Injection of Poynting Flux
• Distribution of Flare Energetics– Nanoflare heating⇒ Contribution to Coronal Heating ?
Shimizu 1995; Sakamoto+ 2009

• Height dependence of Non-thermal δ3⇔ Dissipation of Alfvénic waves
Hara & Ichimoto 1999; Banerjee+ 2009; Hahn+ 2012

Other Issues should be Addressed• B at Photosphere ⇔ Injection of Poynting Flux
• Distribution of Flare Energetics– Nanoflare heating⇒ Contribution to Coronal Heating ?
Shimizu 1995; Sakamoto+ 2009

• Height dependence of Non-thermal δ3⇔ Dissipation of Alfvénic waves
Hara & Ichimoto 1999; Banerjee+ 2009; Hahn+ 2012

• Footpoint of Solar Wind
–Plume vs Interplume– Krishna Prasad+ 2011

Other Issues should be Addressed• B at Photosphere ⇔ Injection of Poynting Flux
• Distribution of Flare Energetics– Nanoflare heating⇒ Contribution to Coronal Heating ?
Shimizu 1995; Sakamoto+ 2009

• Height dependence of Non-thermal δ3⇔ Dissipation of Alfvénic waves
Hara & Ichimoto 1999; Banerjee+ 2009; Hahn+ 2012

• Footpoint of Solar Wind
–Plume vs Interplume– Krishna Prasad+ 2011

• Solar–Stellar–Astro Connection• Stellar Flare – Stellar Corona – Stellar Wind

– Protoplanetary Disks

Summary –Individual Events
Wind
Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:

Heatingwell-done
Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating• X-ray flux in ARs

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating• X-ray flux in ARs• Need Further studies
in QSs & CHs

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating• X-ray flux in ARs• Need Further studies
in QSs & CHs• Wind Acceleration

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating• X-ray flux in ARs• Need Further studies
in QSs & CHs• Wind Acceleration• “Bright” outflows observed(ARs & XBPs)

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating• X-ray flux in ARs• Need Further studies
in QSs & CHs• Wind Acceleration• “Bright” outflows observed(ARs & XBPs)• How about wind from CHs?

Heating

Propagation

Reflection

DrivingSummary –Individual EventsWind• Driving Poynting Flux:
well-done• Propagation/Reflection:need quantitative studies
B2⊥ 3∥ /2 − B∥ 3⊥ B⊥ :Non-observable; but B ⇔ 3A
• Heating• X-ray flux in ARs• Need Further studies
in QSs & CHs• Wind Acceleration• “Bright” outflows observed(ARs & XBPs)• How about wind from CHs?

Heating

Propagation

Reflection

Driving

based on Matsumoto & Suzuki 2012

⇔ Forward-type Numerical Simulations

Summary –Integration

Summary –Integration
Want to know Integrated Energy Input.

Summary –Integration
Want to know Integrated Energy Input.

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
FactorSummary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs

Photosphere – Corona Coupling ?
An example observation of an AR

Coordinate observation incomparison with numericalsimulation
Reconnection-triggered• Ca II jet• Propagating Alfvénic waves• X-ray jet
Need quantitative arguments.
HINODE – IRIS coordinate
observation.

Nishizuka+ 2008

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution ⇒ B ⇑ & f ⇓Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

t
Time

• t

(x,y)

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

t
Time

• t
• High Cadence(x,y)

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

t
Time

• t
• High Cadence• Time filling factor ?;(x,y)

Filling
Factore.g. flare stats
how about for waves• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration

Summary –Integration
Want to know Integrated Energy Input.

Summary –Integration
Want to know Integrated Energy Input.

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
FactorSummary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution ⇒ B ⇑ & f ⇓Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

(x,y)

t
Time

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

t
Time

• t

(x,y)

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

t
Time

• t
• High Cadence(x,y)

Filling
Factor• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary –Integration
Want to know Integrated Energy Input.
Vertical z
Coupling

t
Time

• t
• High Cadence• Time filling factor ?;(x,y)

Filling
Factore.g. flare stats
how about for waves• z ⇔Phtsph-Chmsph-TR-Crn-Wnd coupling
particularly in QSs & CHs• (x, y) ⇔ filling factor ( f )higher resolution⇒B⇑& f ⇓∫• Φ = BdS: OK• 3A changes ⇒ reflection

Summary• Vertical Direction

Photosphere – Chromosphere – Corona &Wind: Our understandings are decoupled at
the moment⇒ Coordinate Observations• Horizontal Direction
Filling Factor of energy flux / tubes / magnetic
elements⇒ Smaller scale• Time Direction
Heating in time integration ??
⇒ Need compiling works with present
observational data

Energy Transfer()
F = ρ3∥ 32 /2 + h − GM/r
+3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy

Energy Transfer)(
F = ρ3∥ 32 /2 + h − GM/r
+3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy
1

ρ3∥ 32 /2

Energy Transfer)(
F = ρ3∥ 32 /2 + h − GM/r
+3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy

ρ3∥ 32 /22
2 ρ3∥ 3 /2⇒
3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
1Energy Transfer)(
F = ρ3∥ 32 /2 + h − GM/r
+3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy

ρ3∥ 32 /22
2 ρ3∥ 3 /2⇒
3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
1

3

3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π⇒ ρ3∥ hEnergy Transfer)(
F = ρ3∥ 32 /2 + h − GM/r
+3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy

ρ3∥ 32 /22
2 ρ3∥ 3 /2⇒
3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
1

3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π⇒ ρ3∥ h2
4 3∥ B /8π −⊥B∥ 3⊥ B⊥ /4π + ρ3∥ h⇒ ρ3∥ 32 /2
3

Energy Transfer()
F = ρ3∥ 32 /2 + h − GM/r
+3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
h: enthalpy

ρ3∥ 32 /22
2 ρ3∥ 3 /2⇒
3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π
1

3∥ B2⊥ /8π − B∥ 3⊥ B⊥ /4π⇒ ρ3∥ h2
4 3∥ B /8π −⊥B∥ 3⊥ B⊥ /4π + ρ3∥ h⇒ ρ3∥ 32 /2
3

Input & Response in TR & Corona• Direct (spectroscopic/imaging) OBS oftransverse waves• Direct (spectroscopic/imaging) OBS of
longitudinal waves• Indirect OBS –Non-thermal broadening–
Propagation & Dissipation of Alfvénic waves• OBS of outflows
Ubiquitous in open flux tubes near ARs• X-ray bright points