シンポジウム「スペース太陽物理学の将来展望」

ダイナモモデルの検証のために（表面磁場観測からわかると嬉しいこと）

政田洋平（神戸大学）

＠シンポジウム「スペース太陽物理学の将来展望」
宇宙科学研究所（2014年10月20日-21日）

Solar-Cの時代にわかる「と嬉しい」ことEventually the heirarchy
must culminate
in motions 本当に対流層の底なのか？
①ダイナモ領域.
large enough to sense the②反転周期を決める（に影響を及ぼす）物理.
spherical
geometry androtation

Giant Cells!

Tachocline Dynamo or Distributed Dynamo ?
★Tachocline Dynamo(e.g., Flux-transport Dynamo)★Distributed Dynamo
(Convective Dynamo)

標準モデル

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
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①

②



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磁場増幅はタコクライン
対流は乱流拡散の源.
平均場による移流.










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








磁場増幅は対流層全域
対流によるダイナモ

ダイナモ領域は対流層の底か？対流層内部か？

（ 対流は磁場を拡散だけさせるのか、増幅もするのか？）黒点、コロナ小輝点、コロナホールの差動回転観測★どうやってダイナモ領域の情報を得るか？
→ 磁気要素の差動回転分布の観測（黒点、黒点群、コロナ小輝点、コロナホール等
可視, EUV, X線）

磁束管の根元がどこに繋がっているか？
(ダイナモ領域への制限)

e.g.,Schou +98
Thompson+03※ disconnection from magnetic
roots (Schussler & Rempel 2005)

黒点、コロナ小輝点、コロナホールの差動回転観測
HARA
Vol. 697

Sidereal Rotation Rate ωc (deg day-1)

15Hara (2009)(Yohkoh Soft-Xray)

460

14
440
420

13
Simon & Noyes (1972); EUV BP
Brajsa et al. (2004); EUV BP
This study (southern hemisphere); XBPThis study (northern hemisphere); XBP
Komm et al. (1993); Photospheric magnetic field
Snodgrass & Ulrich (1990); Photospheric Doppler
Weber et al. (1999); Global corona

12

11

0

20

★磁束管の根元が繋がっている場所は？
Table 1
Differential Rotation Rate ωc (8 hr < ∆t < 24 hr)

480

400
380

Rotation Frequency ωc /2π (nHz)

982

360

40 Hiremath & Hegde
60

Latitude θ (deg)4802. Differential rotation rates of XBP for 8 hr < ∆t < 24 hr and H =FigureFirst Rotation Rate (nHz)2
Hiremath & Hegde (2013) χ = 0.202
12,000 km in northern (southern) hemisphere shownin red (blue) color. The
2
χ_Antia= 5.401 magnetic(SOHO/EIT)
rotationfrom EBP by other observations and from photospheric
460 rates

fields are also shown as reference.

440

the rotation velocity. In Figures 1(a)–(e), we show five latitude
bands and the decrease of the modal value is clearly seen fromthe420latitude band near the equator to a higher latitude band.
The detail of the
curve
shown in the nextΩ(θ) differential= 13.63 (±0.01)rotation- 0.64(±0.05)
sin θis deg/day
section.
400
nHz histogramsΩ(θ) = 438.22(±0.28)-20.56(±1.71)
sin θsimilar
In order to estimate
H from the
XBP data,
in 380the equatorial region were made for several longitudinalsegments. TheΩ(θ)
modalvalue ωc ina single longitudinal= 437.55(±4.03)-4.77(±29.55)
sin θ nHz segment isestimated
360 from each histogram f. The slope dωc /dφ is calculated
and is plottedfunction of1(f).
-40 as a -20
0 H in Figure
20
40 In order tosatisfy a constant rotation
rate (deg)with respect to the longitude
Latitude(dωc /dφ = 0), we adopt the characteristic height of XBPs H to222

Latitude(deg)Southern Hemisphere(deg day−1 )● 短寿命XBPs:
00–05
14.337 ± 0.002

Northern Hemisphere
小規模コロナ構造−1(deg day+ 01,02,04)
e.g., Brajsa

14.360 ± 0.002-1(14.2
deg day ~ Ω@0.99Rs)
05–10 差動回転14.388± 0.00314.317± 0.002
Hara±(2009)10–15
14.328 ± 0.002
14.2900.003
15–20
14.202 ± 0.003
14.237 ± 0.003
20–25
14.034 ± 0.003
14.127 ± 0.003-1(14.4
deg day ~ 13.911
Ω @0.97Rs)
25–30 差動回転13.842± 0.003± 0.004
Hara±(2009)30–35
13.616 ± 0.004
13.631
0.004
35–40
13.316 ± 0.005
13.276 ± 0.005
40–45
13.004 ± 0.006
13.043 ± 0.004
45–50
12.682 ± 0.009
12.613 ± 0.008
50–55
12.046 ± 0.008
12.232 ± 0.010
黒点：差動回転〜XBPsと同程度(Ω
@0.97Rs)
55–60
11.862 ± 0.018
11.790 ±0.014● 長寿命XBPs :● 黒点、黒点群 :e.g, Komm et al. (1993)

Table deg2
黒点群：差動回転 (14.6
day-1 ~ Ω @0.94Rs)
Differential Rotation Parameters (8 hr < ∆t < 24 hr)● コロナホール：A

HemisphereBC-1
剛体回転 (13.6
deg day−2.05~Ω@0.62Rs)South
14.39 ± 0.01
± 0.10−2.20 ± 0.17
Hiremath & Hegde (2013)
North
14.38 ± 0.01
−1.77 ± 0.10
−2.70 ± 0.17
14.39 ± 0.01
−1.91 ± 0.10
● 大規模コロナ構造：

South and North−2.45 ± 0.17

剛体回転 (or 差動回転, 緯度依存性?)

wheree.g.,
A, B,Wagner
and C arefitting parameters,
thoughthe second
75; Timothy+75;
Weber& Sturrock02
term is not orthogonal to the third term. The rotation profiles
shown in Figure 2 are fitted by this function and the result of
the fitting is tabulated in Table 2. The equatorial rotation rate of
コロナホール以外は
2.919µrad s−1 or 14.41 deg day−1 for a July 1996 data set in
磁束管の根元はKarachik
et al.sun(2006)
appears to be coincident
because a muchr > 0.9Rの差動回
larger value in height, ∼80,000 km, is usedin their estimation.
対流層表面？

転分布と一致.

4. SHORT- AND LONG-LIVED XBPS

近年の全球ダイナモ計算が示唆すること
太陽ダイナモを想起させる近年の全球ダイナモ計算：
・LES＋放射層・30年周期, 赤道反対称
・対流層底部
・DNS＋放射強制項
・赤道マイグレーション
・対流層表面
・LES＋高速回転
Figure 2. Spatiotemporal evolution of the zonallyaveraged magnetic field・赤道マイグレーション
in the three-dimensional MHD simulation of Ghizaru et al. (2010). Top
極小期
panel: time–latitude diagram of the zonally・6年周期,
averaged toroidal
magnetic

2

component at the core–envelope interface (r/R⊙ = 0.718); middle panel: corresponding radius–latitude diagram, extracted ・対流層中部
at latitude −45◦ in the southern hemisphere. The dashed line indicates the core–envelope interface; bot・LES
tom panel: time–latitude diagram of the zonallyaveraged surface radial field(r/R⊙ = 0.96), with magnetic half-cycles numbered from each minimum to・準周期的反転. 浮上磁場？
the next as with the sunspot cycles. The color scale codes the magnetic fieldstrength in Tesla.
Augustson et al. ・対流層底部|θ | ! 40◦ ) suggested by the butterfly diagram, but does show
多くがDistributed
Dynamoa tendency for equatorial
migration as each half-cycle
unfolds.
On a time–latitude diagramsuch as Figure 2を示唆
(top panel), this is(対流ダイナモ)seen in the strong toroidal field concentrations, which take anelongated, elliptical shape, with the “major axis” tilted toward
the equator as the Solar-Cで進展が見込めるか
cycle is followed in time. In other words,
throughout a cycle the latitude of the peak large-scale toroidal
e 1. Temporal sequence of the toroidal magnetic component extracted atと問われると・・・(原さんの話)
magnetic
field occurs
at decreasing latitudes, until
the cycle
et al.
(2010)
Augustson
et al. (2013)
re–envelopeGhizaru
interface (r/R
= 0.718)
in the three-dimensional
MHD⊙

Figure 1. Nature of the toroidal magnetic field Bφ . (a) Snapshot of the horizontal structure of Bφ at 0.95 R⊙ shown in Mollweide projection,

ダイナモの反転周期を決める（に影響を及ぼす）物理
3層ポリトロープモデル: 上部放射層（冷却層）, 中部対流層 & 下部放射層
Masada & Sano (2014a) PASJ
Masada & Sano (2014b) ApJL
冷却層
（彩層・コロナ）

Ω

g

Con
ve

ctio
n Zo
ne
Rad
iativ
e Zo
ne

Ro = vrms/2Ω0d~ 0.03 @対流層

上部境界：開放境界条件
下部境界：完全導体境界条件

圧縮性MHD (回転系)
Pr = 1.2, Pm = 4,
Ra = 4×106

磁場の反転周期が冷却層の磁気拡散時間に依存
DNS
MF modelτdiff = 2dRZ,tW/η0dRZ,t: 冷却層の厚み
W : ボックス幅
η0 : 微視的磁気拡散係数

depth (z)

0.4
0.8
1.2
1.6
2.0
0

(a)
200

400

600

800

t/τcv

1000
-0.05

1200
0.05

0.0
0.4
0.8
1.2
1.6
2.0
0

– 6–
– 6 –

(b)
1

3

2

5

4

t/τdiff

6

7

-0.04

0.04

Fig. 2.— Time-depth diagram of ⟨Bx ⟩h for the reference model in (a) the DNS and (b) the MF model√
coupled with the DNS. The orange (blue) tone denotes the positive (negative) ⟨Bx ⟩h normalized by dg0 ρ0 .
The horizontal dashed lines show the interface between the convection zone and the stable zones.
electromotive force (e.g., Ossendrijver et al. 2002). The coeﬃcients α, γ, and η represent the α-eﬀect,
turbulent pumping, and turbulent magnetic diﬀusivity, respectively. All the terms related to ⟨u⟩h and ⟨Bz ⟩hcan be ignored in considering the symmetry of the system. All the variables, except for η0 , depend on thetime (t) and depth (z).
Fig.
The time seriesof ⟨B⟨By ⟩⟩v forfor
thethereferencemodel. The
cyan[orange]solid line
denotesv and ⟨B
Fig. 3.— The 3.—
time
of ⟨B
⟩vx ⟩andmodel.
Thecategory.
cyan[orange]line
denotesxv
The series
MF dynamo
described
byy equation(2)reference
falls into theα2 -type
The MFsolid
theorypredicts
⟨B
⟩
[⟨B
⟩
]
in
the
DNS.
The
red
dashedandblue
dash-dotted
lines
are
those
in
the
MF
model.
The
time model. The timexvy v DNS.
2⟨Bx ⟩v [⟨By ⟩vthat
] in
the
The
red
dashedandblue
dash-dotted
lines
are
those
in
the
MF
the α mode can generate a large-scale magnetic field with an oscillatory nature (e.g., Baryshnikova &is normalized
by the turbulent
magnetic diﬀusion
diﬀusion time.
is normalized
by the 1987;
turbulenttime.
Shukurov
Rädlermagnetic& Bräuer 1987;
Brandenburg
et al. 2009). A key ingredient for the oscillatory modeis the nonuniformity of the α-eﬀect, which can arise naturally as an outcome of rotating stratified convectionin the stellar interior. Using the rigidly rotating system studied here, the α2 dynamo wave was excited,
inwhichour model,
where Hdonly= −dz/dln⟨⟨ρ⟩⟩
the density scaleheight.asHere,the subscript“k” etreferstheh is direction.
propagatesin ln⟨⟨ρ⟩⟩
the
depth
However,shown
by Käpylä
al. to(2013b),in the global
in our model,
where
Hd = −dz/dh is the density scale height. Here, the subscript “k” refers to theunquenched
coeﬃcient,which
iscalculatedfrom
DNS
resultsofthesaturatedconvective
turbulence.
it canwhich
travel also
in the latitudinal
direction
due ofto thethe strong
antisymmetryof theα-eﬀect acrossunquenchedsystem,
coeﬃcient,is calculated
from DNS
results
saturatedconvective
turbulence.
the equator.
In the first-order smoothing approximation (FOSA), the unquenched coeﬃcients αk , γk and ηk in
In the first-order smoothing approximation (FOSA), the unquenched coeﬃcients
αk , γk and ηk inanisotropic
are given by (e.g.,Käpylä
et al. 2006,2009b),force that tends to “quench” the turbulent motions and
The forms
dynamo-generated
MF
producesa Lorentz
anisotropic forms are given by (e.g., Käpylä et al. 2006, 2009b),
control the nonlinear evolution and saturation of the system. Since there is no definitive model to describe
αk (z) = (e.g.,−τc [⟨⟨uRogachevskii∂y Kleeorinuz ⟩⟩h ] ≡ −τ2001;(7)z ∂x uy ⟩⟩h + ⟨⟨ux&
c Heﬀ ,Blackman & Brandenburg
the magnetic quenching2002) as yet,(7)αk (z) eﬀect= −τc [⟨⟨u∂ u ⟩⟩h +2 ⟨⟨uzx ∂y uz ⟩⟩h ] ≡ −τc Heﬀ ,2 x y
we adopt the prototypical
α-quenching,algebraicγandη-quenchingofγk (z) models,= −τc ∂zwhich⟨⟨uz ⟩⟩2h are≡ −τthe,(8)c ∂z udynamicalrms
γk (z) = −τc ∂2z ⟨⟨uz ⟩⟩h2 ≡ −τc ∂z u2
(8)
rms ,
the catastrophic-type;ηk (z) = τc ⟨⟨uz2⟩⟩h ≡ τc urms ,2(9)
ηk (z) = τc ⟨⟨uz ⟩⟩!h ≡ τc u
(9)
"
rms ,
∂α
α⟨Bh ⟩2h − η (∇ × ⟨Bh ⟩h ) · ⟨Bh ⟩hα − αk2=eﬀ is−2η
kc+(4)
where τc is the correlation time, H
thekeﬀective
helicity, and urms
is the root-mean-squarevelocity., The2∂t 2 eﬀ is the eﬀective
Beq
ReM
where τc is verticalthe correlationtime,
helicity,anduis theroot-mean-squarevelocity. The
rms
profiles of Heﬀ
and uHinthereference
DNS
model
are
shown
in
Figure
1b
by
solid
and
dashedrms
γk
vertical profilesof Heﬀ and u2
model are shown in Figure 1b by solid and dashedγ in=the reference DNS(5)rms
lines, respectively.
2 /B 2 ,
1
+
Re
⟨B
⟩
M
h
eq
h
lines, respectively.
ηk
The correlation time shouldandη =be zero in the top cooling, bottom stable layers since the convective
(6)
2 /B
2
The correlation
timeshouldbethuszero
theand bottom
stablelayersthe convective
1α
+ in
Re
⟨B
⟩=
eq
h 0 coolingturbulence is not
fully
developed;= γM= ηhtop
there.
Assuming
the Strouhal
numberis unitysincein

Masada & Sano (2014b)

35000
30000

τcyc [cycle period]

τcyc ~ τdiff

0.0

depth (z)大局的磁場の反転周期

– 5 –

25000
20000
15000

k

k

k

turbulence theis notfullyzone
developed;
αkthe=vertical
γk = profileηk = of0 τthere.
Assuming
the Strouhal number is unity inconvection(St = τc urmsthus
kc = 1),byc is given(see Brandenburg & Subramanian
2005, for the quenching),
where ReM = ηk /η0 . The dependence of the MF
the convection zone (St = τc urms kc = 1), !the verticalprofile
of
τ
is
given
by
" discussed#$ ! in detail" c in #$model on the quenching formulabesubsequent paper, however, at least the
1 shouldz"− zb
zt − z a"!
#$!
τc (z) =remain
1
+
erf
1
+
erf
, − z #$ models.
(10)The characteristic
conclusions of this Letter
independentfromthechoiceofthet
4u1rms kc 1 + erf h z − zb
h erf zquenching
τ
(z)
=
1
+
, and B (z) = ⟨⟨ρu 2 ⟩⟩(10)cwavenumber kc andthe equipartition
fieldstrength
B
are
given
by
k
(z)
=
2π/H
c h
d
eq
z
h
4urms kc
h eq
where zi (i = t, b) represents the location of the boundaries between regions with and without fully developed
where zi (i turbulence.
= t, b) represents
location
the whereboundaries
betweenregionsand
withand without
We define thezt andzb as theofdepthHeﬀ achieves
the maximum
minimum
values, fully developed
turbulence.respectively
We definezt andthe depthHeﬀ parameter
achieves
maximumand(see Figure1b). zThetransition
width h whereis an arbitrary
andtheassumedhere as h =2∆z minimum values,b as
respectivelywith(seetransition
width hinis
arbitraryparameter
and∆zFigure= 2d/Nz1b).
. The The
uncertaintyof h is discussed
thean
next
section. All
the coeﬃcients(τcassumed, Beq , Hd , here as h = 2∆zwith ∆z =α2d/N
The uncertaintyof h isnextfrom
section.
the coeﬃcients (τc , Beq , Hd ,for the MF modelingcandiscussed
subsequentlyin
be thecomputed
the DNSAllresults.
k , γk , ηzk.) required
αk , γk , ηk ) required for the MF modeling can subsequently be computed from the DNS results.

10000

5000

Masada & Sano (2014c) in prep.
（天文学会2014秋季年会発表：M34a）

0

3.2.

Comparison with DNS

0 3.2.5000
10000 15000
20000 25000 30000 35000
Comparison
with DNS

Given all the coeﬃcients in equations (2)–(10) from the reference DNS model, the MF equations can
フレアやCMEとダイナモの繋がりを示唆
the second-order
central diﬀerence.
time theintegration,
the fourth-order
Runge-Kutta
Given beallsolved
the usingcoeﬃcientsin equations(2)–(10)For
fromreference
DNS model,
the MF equations can

2dRZ,t W/η0

method theis used.
We adopt the same
parameters
used in theFor
DNS:time
the calculation
domain of
0 ≤fourth-orderz ≤ 2d, thebe solved using
second-order
centraldiﬀerence.
integration,
theRunge-Kutta

Convective Dynamo Experiment with additional MH loss
開放境界＊テストモデル：磁場の境界条件を変更

境界条件を変更＊upper ：Open B.C., bottom：Closed B.C.
＊ y：Periodic B.C. x : Open & Closed B.Cs.

動径方向＊upper ：Open B.C., bottom：Closed B.C.
＊horizontal：Periodic B.C.

向
方
経度
緯度方向

動径方向＋緯度方向のマイグレーション. 反転周期の短縮 (周期境界モデルの3/4).

太陽磁場・磁気ヘリシティの消失ルートは恐らく３つ★Possible Routes for Magnetic Field and Helicity loss：①極域への磁束輸送（極域の反対極性磁場による磁場・磁気ヘリシティ消失）②赤道域への磁束輸送（南北半球間の磁場・磁気ヘリシティ消失）③表面からの磁場の散逸（フレアやCMEによる磁場・磁気ヘリシティ消失）■ ①と②に関しては、子午面循環流が恐らくリコネクションのinflowの役割.
■ ③に関しては、頻度が小さく、現在の太陽では恐らくマイナーな効果.
（ただし、昔の太陽になるともしかするともう少し効くかも）

大小の磁気要素が緯度方向への輸送過程を理解するのは極めて重要（→ 飯田さんのお話）Cameron, Jiang, Schussler & Gizon (2014)1984) . The equation for the radial component of the field Br at r = R⊙ is then1∂
★Surface flux transport simulation ： ∂B∂t = − R 1sin θ ∂φ∂ (uB ) − R sin(!B sin θ)θ ∂θr（子午面循環流 [極への磁束輸送] が周期をコントロール）- 表面の大局的動径磁場成分の進化計算（運動学的）.
- 観測結果【表面平均場速度 (vθとvφ)]を仮定.

r

⊙

⎡
⎢⎢
+ ηH ⎢⎣⎢

r

⊙

⎤
$
%
∂
∂2 Br ⎥⎥⎥
1
∂Br
1
⎥⎦
sin θ
+ 2 2
∂θ
R2⊙ sin θ ∂θR⊙ sin θ ∂φ2e.g., + D(Br ) + S (θ, φ, t),
DeVora+ 84, 85; Sheeley +85; Schrijver 01;
10.1002/2013JA019498
whereu(φ, θ, t) is the velocity in the longitudinal (φ̂) direction, !(φ, θ, t) is the v- 観測結果（浮上磁束）をソース項としてインプット.
Sheeley Jr Research:
05; Wang & Sheeley
09;
Journal of GeophysicalSpace
in the latitudinal (θ̂) direction,
ηH is the horizontal diﬀusivity
at thePhy
surface
Jiang+10;
Cameron&Schussler
12（※非線形性を与える種として活動領域へのinflowも考慮）we have assumed is uniform), D is some operator representing the removal
van Ballegooijen and Mackay 07
from the surface, and S is a source term describing the emergence of new fluxof Rn⊙
from below,between
φ and θ aresolar longitude and colatitude respectively and
The strong correlation
thethe(simuradius.
cros
lated) (Fn−1∕2 solar+ Fn+1∕2)∕2 and the observed
In principle, both the the surface velocity, u(φ, θ, t)φ̂ + !(φ, θ, t)θ̂, andthenot(Sn + Sn+1 )∕2 component
indicates thatthemagnetic
SFT modelof thefield are structured on all scales from tens ofWe
to thesize ofpartSun,ofandon time scales of seconds for the small sc
without inflows
capturestheevolves
physics.
conyears for the largest scales. This renders the full problem intractable. For alm
What is not reproducedis the observed
problems, however, the full range of scales do not need to be dealt with, tran
and a
Nor
proportionality
betweentheopenvaluesof u and! canbe flux
used,andwith smaller unresolved velocities being treateCamenhanced
diﬀusivity
ηH the. Thereor
subsequent levelof solaractivity:
y is no single best choice of what temporaltheaveraging should be done: diﬀerent temporal and spatial averaging allowdiintercept (−41.7
±
19.52
)
is
not
consistenttotsciencequestions
to beaddressed.
Add thesigned fluxdue
to four specific events to the SFT simulation
te
in
terms
of step-function
specificwith zero (at theresults
2 the
sigma
level).
As shownInfollowing
sections
we changes
will addat flesh
to times:Eq. (1) by describing in
in de
cific
physical including
processes andin Figure 3, a relevant
SFT simulation
the the ways in which they can be modeled. W
×with a deeper exposition of the basis for the surface flux transport model−2
in S
inflows
towardthe activity
beltssome
repro2. Then
weofdescribeof theways in whichthethesourceterm S can be andcons
Figure 10. Evolution
the netsignedmagnetic
flux in
Northern
Figure 9. Synoptic magnetogram from the National Solar Observatoryc.f.,model
byma
t
in
Section3, andasthe
flows
and
diﬀusivity
Section
4.Cameron
The removal
Hemispherefromobservations(blackcurve),
frominthe
SFT(blue of thethe high
correlation
well
as theKPNO/VT for Carrington
rotation 1686 (September 1979). The grey scale indi- duces①基本的には極域への循環流による磁束輸送が磁場の反転周期を規定& The
Schussler
12usingmat
curve), and fromthe theSFTsolarmodel withadditional
injectionsof results
flux atfrom
theflux fromis reviewed
in Section
5.
the scates the strength of the magnetic field. The red circle shows flux associated observed
proportionality
withsurface
a y plumes
intercept
times whencross-equatorial
flux
were found in Cameron et al.
flux transport model will be presented in Section 6. Section 7 concludes ourreulat[2013]. The arrows indicate the times of flux injections (September 1979,
with an active region which has emerged across the equator, giving rise tonal of Geophysical Research: Space Physics②イレギュラーな南北半球間の磁場・磁気ヘリシティの流出入を考慮
of 0.87 ± 17.95, which is consistent with

flux
cen
2 Observational Basis for Solar Surface Flux Transport
et a
the inflow parameters c0 = 6.9 m s−1 G−1hemispherecorresponds to a change in the polar fields and the
◦
and
𝜎
=
22.5
.
This
value
cthat
The
part
of theofmagnetic
field at events
the Sun’sare
surfacethat dominates
the sig
0 impliesat minima.
Wesuggestthese
a possible
explanatsuch
as obserthoserecordedby the24.
MDI instrument (Scherrer et al.
weakofpolar
fieldsbetweencycles23 anda longitudinally averaged inflow of about 6.4 m/s for an active region
1022magnetograms,Mx,consistent
with
March 1986, 1991, and 2000, the latter two consisting of a cluster ofa cross-equatorial flux plume (Credit: Cameron et al, A&A, 557, A141, 2013,(cross-equatorial
flux
plumes" in Figure 9.
small
events).
The
specific
event
in
1979
is
shown
zero. The example
shown corresponds
toreproduced with permission©ESO.)→ サイクル24の磁気活動性の低下も説明
c.f., Cameron +14[cross-equatorialtransport])※表面の緯度方向磁束輸送を理解することは重要（→ 飯田さんの話）まとめ〜ダイナモモデルの検証のために〜

Solar-C時代にわかる「と嬉しい」こと：①ダイナモ領域は対流層の底か？対流層全体か？

→ 表面とコロナの磁気要素の差動回転観測（全球面の情報が必要）（黒点、コロナ小輝点、コロナホール ..etc…）
過去の観測：表面付近の差動回転とダイナモの関連を示唆②反転周期を決める（に影響を及ぼす）物理.

- 極域への磁束輸送（極域の反対極性磁場による磁場・磁気ヘリシティ消失）- 赤道域への磁束輸送（南北半球間の磁場・磁気ヘリシティ消失）- 表面からの磁場の散逸（フレアやCMEによる磁場・磁気ヘリシティ消失）→ 緯度方向の大小スケールの磁束輸送を理解することは重要（飯田研究である程度は進展するかも？）①と②ともに、磁気要素の移動から大局的移流を理解する研究
・グローバルダイナモの理解のためには、全球的な磁場・流れの情報が必要.
・微細構造の定量理解を目指す(全面像の無い)Solar-Cではなかなか難しい.
・それでも何かできないか・・・. 何かしたい. 今後継続的に検討.乞うinput.