Achievements of Hinode: Part 1	 coronal heating and the acceleration of the solarwind	 waves	 nanoflares	 magnetic coupling between the surface and thecorona	 physics of flux tubes and convection	
 elementary flux tubes
 sunspots	Coronal Heating:Temperature Distribution, DEM	 EIS quiet-sun DEM （Brooks et al. ApJ 2009）	
 similar to CDS

results	

CDS: Temperature Variations with Height
Schmelz & Martens 2006 ApJ

EIS: ?
XRT: Kano et al. 2008 PASJXRT filter ratio
 high temperaturecomponent log T>7
Reale et al. 2009 ApJ(Cf. Yohkoh
Yoshida & Tsuneta
1996 ApJ)	

Active Region DEM
Schmelz et al. ApJ 2009	
 combination ofXRT andRHESSI data high temperaturecomponent
logT>7signature ofnanoflares
 EIS?	

 wave heating, if any, is not due tocoherent (large-scale, > a few arsec)
waves.
 Important is the origin of nonthermal
broadening.
 Is it due to upflows from the footpoints（Hara et al. 2008 ApJL; McIntosh & De
Pontieu 2009 ApJL; De Pointieu et al.
2009 ApJL) or waves in flux tubes(Fujimura & Tsuneta 2009) ?

 So is it due to nanoflares? But EIS

observations of moss show only weaktime variability （Brooks & Warren 2009ApJL).
 Loops in the core of active region seen
with EIS 0.4-2.5MK +XRT are in a cycle ofheating and cooling（Ugarte-Urra et al.
2009 ApJ).
(Cf. Nagata et al. 2003 ApJ
Hot loops and cool loops are mutuallyexclusive）	

Distribution Function of Small Flare Events

 Yohkoh SXT

slope −1.5
<20% of required
heat input
 How about
Hinode XRT?	

Shimizu 1995 PASJ

Magnetic Coupling between theSurface and the Corona	 many studies on flare energy build-up andNLFFF modeling based on SP vector fielddata flux emergence, cancellation, and theireffects on the corona: needs wide FOV
and high time cadence, ideally by NFI.

Yohkoh SXT hot loops (>2MK) andEIT, TRACE cool loops (<1MK)	

TRACE 171Å
cool loops(1 MK)

TRACE“moss”
structure:footpoints ofhot loops

Yohkoh/SXT
hot loops (> 2 MK)

Katsukawa and Tsuneta (2005)

cool loops

difference in magnetic
filling factor?	
hot loops

Loosely packed fluxtubes are easier tobe moved and moreenergy is supplied,
leading to hot loops.	

低温ループ	

Tightly packed flux
tubes are harder to be
moved and lessenergy is supplied,
leading to cool loops.	

SOT + EIS (Brooks et al. 2008 ApJL) chromospheric/TR transient events
 mixed polarity, dynamic areas with flux

cancellation
 hot coronal loops moss region, unipolar XBPs are made ofseveral smaller
loops (Kotoku et al.
2007 PASJ).
 At the footpoints of
XBPs there aremany Ca H and GBand bright points(Perez-Suarez etal. 2008 A&A).

Flux Emergence and Heating of theChromosphere and Corona
 flux emergence → dark lanes in G-bandand Ca H (Ohtsuji et al. 2007 PASJ) activity in the sequence of B→Ca H→XRT（Li et al. 2007 PASJ）
 B→Ca H: high correlation, but less tightcorrelation with G-band (Guglielmino et al.
2008 ApJL)Coronal Heating Problem: What to Do?	
 to discriminate between wave heating andnanoflare heating（or decide the ratio of contributions）
 data are available, (only) one step further（wisdom?）	

Origin of the Solar Wind	 XRT outflow (Sakao et al. 2007 Science)
 EIS outflow (Harra et al. 2008 ApJL) polar-region activity (Tsuneta et al. 2008

ApJ; Shimojo & Tsuneta 2009 ApJL)	

Physics of Elementary Flux Tubes
 convective collapse discovery (one event) by Nagata et al. 2008ApJL statistics (49 events) by Fisher et al. 2009
A&A

Physics of Elementary Flux Tubes	
 motion, diffusion
 rms motion 1.56 km/s (de Wijn et al. 2008ApJ)
 diffusivity 0.9 km2/s (Chae et al. 2008 ApJ)
 vortex flows
life time longer than 1 hour (Attie et al. 2009A&A)

Chae et al. 2008 ApJ	

Attie et al. 2009 A&A	

Ubiquitous Horizontal Field (Ishikawa etal. 2008 A&A)	
 A classical picture of ‘canopy’ has been

replaced by a dynamic process.
 Ubiquitous (Ishikawa & Tsuneta 2009A&A)? Then they may not be the main
contributor to coronal heating.	

Missing Physics of Flux Tubes	 decay process interaction with convection
 behavior of weak intra-network field;

needs deep magnetograms by NFISunspots	 convection in umbrae（Umbral Dots) structure of penumbrae sources and sinks of Evershed flow physical mechanism still not clear decay process removal by MMF
 internal destruction by light bridge

 formation process is less clear yet	Helioseismology	 sunspot oscillation (Nagashima et al. 2007PASJ) not so new results?

 3D structure of supergranules(K.Nagashima, thesis）
 smaller and deeper near the poles	Summary Many unexpected discoveries,

110 points out of 100.
 However, topics that should have beenstudied are left untouched.
80 points
 In overall, 95 points out of 100.