Solar-­‐C	
  and	  the	  new	  4m	  class	  solar	
  telescopes	
  	
  

V.	
  Mar'nez	
  Pillet	  	
  Na0onal	
  Solar	  Observatory	
  )V\SKLY:LSLJ[LK(Z5:6»Z
	
  
	
  

Outline	  1. ATST/EST Status
2. Why 4m?
3. Science case: quiet sun magnetism
4. Solar Physics from space: opportunities
5. Solar-C & ATST

11/11/13	
  Solar-­‐C	
  

2	
  

WrapStesting1.-­‐	
  CableATST	
  tatus	
  	
  

Stats
• Cycle 1:
21 proposals submitted: 6 standard, 6 survey, 9 ToO (5 flare ToO)
8 new users (never observed at DST before)
6 PI's were PostDocs (3 new, 3 old)
11 proposals completed (weather issues)
Total data volume: 4.2 TB (science and calibrations)
Grinding begins(fixed tool)!
• Cycle 2:14

18 proposals submitted: 7 standard, 6 survey, 5 ToO (3 flare ToO)
7 new users
1 PI is a PhD student
about 7 PI's are PostDocs7 (~4 new, 3 old)
7 proposals completed, 4 programs in progress (until Oct 22)
Total data volume (up to Oct 18): 8.9 TB (science and calibrations)NISP personnel involved in data distribution!

Oslo 8/8/2013

12

NSB	
  approval	
  of	
  ATST	
  revised	
  project	
  baseline	  11/11/13	
  Solar-­‐C	
  

3	
  

Construc0on	
  at	
  the	  summit	
  !	
  	
  

tory

high
000
11/11/13	
  Solar-­‐C	
  

4	
  

First	  genera0on	
  of	
  instruments	  	  	
  VBI	
  (ROSA):	
  Visible	
  Broad	
  band	  imager	  •Wavelength	
  range:	
  	
  380–900	
  nm	
  •Spa0al	  resolu0on:	
  	
  0.03”	
  @	
  Hα	
  
•Spa0al	
  FOV:	   	  	
  2×2	
  arcmin2	
  •	
  Real-­‐0me	
  speckle	
  	
  ViSP	
  (SPINOR):	
  Visible	
  Spectropolarimeter	
  •Wavelength	
  range:	
  	
  380–900	
  nm	
  
•	
  Up	
  to	
  three	  lines	  simultaneously/fast	
  reconﬁg	  (10	  mins)	
  •Spa0al	  resolu0on:	
  	
  0.03”/pixel	  •Spa0al	
  FOV:	   	  	
  2×2	
  arcmin2	  •Spectral	
  Resolu0on:	
  
	
  R	
  ~	
  	
  3.5	  pm	  at	
  630	  nm	  
	  VTF	  (IBIS):	
  Fabry-­‐Perot	
  tunable	
  Spectropolarimeter	
  •Wavelength	
  range:	
  	
  520–860	
  nm	
  •Spa0al	  resolu0on:	
  	
  0.03”	
  •Spa0al	
  FOV:	   	  	
  1x1	
  arcmin2	  •Spectral	
  Resolu0on:	
  
	
  R	
  ~	
  3.5	  pm	  at	
  630	  nm	  
	
  DL-­‐NIRSP	  (FIRS):	
  DiﬀracGon	
  Limited	
  NIR	  Spectropolarimeter	
  •Wavelength	
  range:	
  	
  900–2300	
  nm	
  •Spa0al	  resolu0on:	
  	
  0.03-­‐1”/pixel	  •Spa0al	
  FOV:	   	  	
  2.4x1.8	
  arcmin2	
  	  	
  Cryo-­‐NIRSP	  (CYRA):	
  Cryogenic	
  NIR	  Spectropolarimeter	
  •Wavelength	
  range:	
  	
  1000–5000	
  nm	
  •Spa0al	  resolu0on:	
  
	
  1”	
  (corona)	
  •Spa0al	
  FOV:	   	  	
  3x4	
  arcmin2	
  	
  11/11/13	
  Solar-­‐C	
  

5	
  

EST	
  (slide	
  provided	
  by	
  M.	
  Collados)	
  	
  

•	
  Conceptual	
  design	
  ﬁnished	  •	
  Detailed	
  design	
  in	
  progress	
  (2013	
  -­‐	  2016)	
  •	
  Construc0on	
  Phase	  (2017	
  –	
  2022)	
  	
  
	
  	
  	
  	
  	
  	
  (funding	  not	
  approved	
  yet)	
  
11/11/13	
  Solar-­‐C	
  

6	
  

2.-­‐	
  Why	
  4m?	  	
  
	  100	  km	
  is	
  photon	
  mean	
  free	
  
path	
  &	
  Hp	
  (scale	
  height)	
  

D=

λ
φ

100	
  km	
  (	
  φ ~0.1	
  arcsec)	
  requires	
  	
  	
  

D ≥	
  1m	
  
texp ∝

φ/2
à	
  25	
  seconds.	
  Polarimetry	
  forces	
  it	
  to	
  be	
  25/4	
  ≈	
  6	
  s	
  
vc

Science	  requires	
  SNR ≈104	
  	
  	
  	
  (mo=	  -­‐10.7	
  magnitudes/arcsec2,	
  	
  	
  φ	
  	
  px	
  	
  	
  	
  =	
  	
  	
  	
  φ	
  	
  	
  	
  /	
  	
  2	
  	
  	
  )	
  

D=

11/11/13	
  SNR
0.7N10−0.4m	  2
τΔλQtexpφ px

Solar-­‐C	  à D ≈ 4.6m	
  	
  	
  
	
  

Forget	  the	
  diﬀrac0on	
  limit	
  (keep	  the	
  photons!)	
  
7	
  

10-­‐3:	
  requirement	
  or	
  performance?	
  
	
  

V
BLON (G) = 4759
Ic
1/2

!
2
2 $
Q +U &BTRA (G) = 2526#
Ic
#"
&%

11/11/13	
  •10-­‐3	
  sensi0vity	
  	
  gives	
  a	
  BLON	
  sensi0vity	
  of	
  5	
  G	
  

•

10-­‐3	
  sensi0vity	
  	
  gives	  a	
  BTRA	  sensi0vity	
  of	
  80	
  G	
  

•

This	
  provides	
  a	
  fundamentally	
  biased	
  view	
  of	
  solar	
  magne0sm	
  

•

To	
  have	
  a	
  5	
  G	
  sensi0vity	
  in	
  BTRA	
  we	
  need	  to	
  reach	
  4	
  10-­‐6	
  	
  	
  	
  

•

The	
  Sun	
  doesn't	
  know	
  anything	
  about	
  10-­‐3…	
  	
  Solar-­‐C	
  

8	
  

We	
  are	
  star0ng	
  to	
  explore	
  the	
  10-­‐4	
  limit	
  	
  

±	
  5	
  10-­‐4	
  11/11/13	
  

±	
  5	
  10-­‐3	  Solar-­‐C	
  

9	
  

8

Manfred Schüssler

the energy-carrying eddies of the flow (i.e., the integral scale of the turbulence). Although
there is some dependence on the value of the magnetic Prandtl number (ratio of kinematic
viscosity to magnetic diﬀusivity), SSD action probably occurs in all turbulent flows of
suﬃciently high magnetic Reynolds number (see Brandenburg et al. 2012, and references
therein). While direct numerical simulations demonstrated SSD action in various settings
since the 1980s (e.g., Meneguzzi et al. 1981; Cattaneo 1999; Bushby et al. 2012), theeﬀect was also found in large-eddy simulations (Boussinesq or anelastic) in sphericalshells carried out to model the solar convection zone (Gilman & Miller 1981; Glatzmaier
1985; Brun et al. 2004). A. Vögler and M. Schüssler: A solar surface dynamo
L45
Comprehensive simulations of solar near-surface convection indicate that the observed
turbulent field could indeed be a product of a SSD action driven by the turbulent intergranular downflows (Vögler & Schüssler 2007; Pietarila Graham et al. 2010; Moll et al.
2011b). The characteristic properties of a magnetic field generated by a SSD can explain
the observed strong horizontal fields observed in the middle photosphere (Schüssler & Vögler2008) and the weak signals detected with sensitive polarimeters (Pietarila Graham et al.
2009; Danilovic et al. 2010a,b). While most of the field due to the SSD is of mixed polarity on small scales and has a strength of some tens to a few hundred Gauss, occasionallyenough unipolar flux is being assembled by the granular flows to form a kG flux concentration appearing as a bright point in the visible light. Therefore, observations of such
Vogler	
  et	
  al	
  	
  	
  2007	
  features in quiet internetwork areas on the Sun are consistent with SSD action.

3.-­‐	
  Science	  Case:	
  Quiet	  Sun	
  magne0sm	
  	
  
25	
  G	
  

3	
  G	
  

Intergranular	
  lanes	
  ﬁlled	
  with	  SSD	
  ﬁelds	  Fig. 2. Snapshot from the dynamo run C, taken about 5 h after introducing the seed field. The vertically emerging bolometric intensity (brightness,left panel) reveals a normal solar granulation pattern. The other panels show the vertical component of the magnetic field on two surfaces of
constant (Rosseland) optical depth, τR . Near the visible surface (middle panel, τR = 1, grey scale saturating at ±250 G), the magnetic field shows
an intricate small-scale pattern with rapid polarity changes and an unsigned average flux density of 25.1 G. About 300 km higher, at the surface
τR = 0.01 (right panel, grey scale saturating at ±50 G), the unsigned average flux density has decreased to 3.2 G and the field distribution has
become considerably smoother, roughly outlining the network of intergranular downflow lanes (darker areas on the left panel).

intermittency of the magnetic field at all heights. The strongest
magnetic features occasionally reach vertical field strengths beyond 1 kG near τR = 1.
Energy spectra for the vertical components of the nearsurface magnetic field and velocity as a function of horizontal
wave number, kh , are given in Fig. 4. The spectral magnetic energy shows a broad peak at kh ≃ 30, which corresponds to awavelength of about 200 km. At the high-wavenumber end of
the spectra, the magnetic and kinetic energies become less disparate. The remaining deviation from equipartition is due to theanisotropy resulting from the strong stratification.
We find that convective downward pumping of flux in fact
has a significant eﬀect on the energy balance of the dynamo, as
conjectured by Stein & Nordlund (2003). At any given height,
the time dependence of the horizontally averaged magnetic energy density, emag , is governed by the equation ∂t emag = WL −WJ −∂Pz /∂z. WL is the rate of work against the Lorentz force, WJ
is the Joule heating rate, and Pz is the vertical component of the
Poynting flux, the advective part of which measures the drainingof magnetic energy due to convective pumping. All quantities aremeant to be horizontal averages. The advective Poynting flux is
Fig. 3. Probability density function (PDF) for the vertical field component at three diﬀerent geometrical height levels. Dashed curve: z = negative throughout the convectively unstable parts of the sim−370 km (about 450 km below the visible surface); solid curve: z = ulation domain, confirming that any growth of magnetic energy
80 km (roughly corresponding to the average level of τR = 1); dotted in the system must have its source inside the domain. The diﬀuPz is foundaction
to be negligible
the convecting
layer.
Figurefroma ofsimulationof small-scalein theinsolar
near-surface
curve:
z = 4005.
kmSnapshot(about the averagelevel
τR = 0.01). Shownare sive part ofdynamo
timeaveragesover computational
about 20 minutes aroundt ≃ 4.5
In theandabsenceconvective
the diﬀerence
L − WJ
layers.
Thebox
is h.12 × 12 Mm2 wide
6.1ofMmdeep.pumping,
The panels
show Whorizonwould be a measure for the growth of the magnetic energy durtal cuts of the vertical field component (upper ing
panels;black andnegativeandthe exponential
growthwhitephase. indicates
In our case, morethan 80%
positivepolarity,
respectively)
and
of
the
verticalflowvelocity(lowerpanels;light
shadesindiofthis
diﬀerenceisindeedcarrieddownwards
by
means
of
the
surface τR = 0.01, about 300 km higher in the atmosphere,−∂Ptakenleavesthe box ofthroughbottomboundary.
cates
upflows,
dark
downflows).
Theandcutstermwere
a depth∼ 5 theMm(leftpanels)z /∂z andatthespatialdistributionof theshades
field is significantly
smoother
reduces
the growth
butas
does
more
associatedto the intergranular
downflow
lanes.
The However,andclosely
2.5 Mm(middlepanels) below
theaverageheighttheof eﬀectthe only
opticalsurface,as rate
well
atnot
the
dynamo action if the magnetic Reynolds number ismeanflux density
has(right
decreased
to about 3The
G. Thisstrong de- shut downfield
opticalsurfacepanels).
dynamo-generatedisassociatedwiththedownflowsin
suﬃciently
large.
crease indicates the absence of significant dynamo driving in the

11/11/13	
  Solar-­‐C	  The	
  dynamo-­‐generated	
  ﬁeld	  is	
  associated	
  with	  the	
  downﬂows	
  in	
  
the	
  deeper	
  parts	
  of	
  the	
  domain	  and	
  thus	  exhibits	  a	
  ’mesogranular’	
  pauern	
  at	
  the	  surface.	
  	
  
	
  
Schussler	
  et	
  al	
  	
  	
  2013	  10	
  Quiet	  Sun	
  magne0sm:	
  Hanle	  vs.	
  Zeeman	  	
  • Hinode/SP	
  has	
  mapped	
  QS	
  magne0c	
  ﬁelds	
  with	  unprecedented	
  spa0al	
  resolu0on	
  (0.3	  “),	  polarimetric	
  sensi0vity	
  (10-­‐3)	
  and	
  spectral	
  coverage.	
  	
  • Much	  debated	
  in	
  the	
  last	  years:	
  noise	  and	
  its	
  impact	  | BTapp |≈5app| BL |
Lites	  et	
  al.	
  2008	  88

OrozcoOrozcoSuárez
Suárez&&Bellot
BellotRubio
Rubio• Hinode/SP	
  at	
  10-­‐4	
  obtains	
  (67	  s):	  	
  | BT |≈ 3.1| BL |
Orozco	  Suarez	
  et	
  al.	  2012	  Figure7.7.High-precision
High-precisionmagnetic
magneticfield
fieldstrength
strengthandandinclination
inclinationdistributions
distributionsfor
forIN
INregionsregionsderived
derived fromfrom data
data set
set #2.
#2. The
The PDFs
PDFs are based on the inversion of
Figurepixelswhose
whoseStokes
StokesQQororUUamplitudes
amplitudesexceed
exceed4.5σ
4.5σQ,U
Theyrepresent
represent27.4%
27.4%ofofthe
thesurface
surfacearea
areacovered
covered byby thethe IN.
IN. About
About 90.3%
90.3% of those pixels show circular
pixels. .They
Q,Upolarizationsignals
signalsabove
abovethethenoisenoisethreshold.
threshold.
polarization• 30%	  of	
  the	  	
  pixels	
  with	  clear	
  Q	
  and	  U	  signals,	
  ME	
  inversions	  • QS	
  ﬁelds:	
  hectogauss	
  (220	  G),	  transverse,	
  random	
  orienta0ons	
  	
  tan γ = 2 tan γ real
• Long	  integra0on	
  0mes	  result	
  in	
  larger	
  inclina0ons	
  11/11/13	
  Solar-­‐C	
  Figure8.8. Distribution
Distributionofofmagnetic
magneticfilling
fillingfactors
factorsretrieved
retrievedfrom
fromthetheinverinverFigure
sionofofthe
thehigh
highS/NS/Ntimetimeseries
seriesincluding
includingonly
onlypixels
pixelswhose
whoseStokes
StokesQQororUU
sion
amplitudes
exceed
4.5σ(solid).
For
comparison,we
also
representtheQ,U(solid). For comparison, we also represent theamplitudes exceed 4.5σQ,Udistribution corresponding to all pixels whose Stokes Q, U, or V amplitudes

Our results
results partiallypartially agree
agree with
with the MHD simulations of
Our
Steineretetal.
al. (2008),(2008), in
in whichwhich thethe magnetic field dynamics is
Steinermainlydriven
drivenbyby flux
flux expulsion
expulsion andand overshooting convection.
mainlySteineretetal.
al. (2008)(2008) computed
computed the horizontally and tempoSteiner
rallyaveraged
averaged absoluteabsolute verticalvertical andand horizontal magnetic fieldrally
components as
as functions
functions ofof height
height for two different simulacomponents
tionrunsrunsand
andfoundfound aa maximum
maximum horizontal/vertical field comtion
ponentratio
ratio ofof about
about 2.5
2.5 atat 500500 km (see Figure 1 in their paponentper). This
Thisisiscomparable
comparablewith
with thethe value we have obtained from
per).
11	
  horizontal
the inversions.
inversions. However,
However, thethe average
averagehorizontal andand verticaltheverticalmagneticfield
field strengths
strengths they
they find
find areare still
still smaller
smaller than
than ours.
magnetic
ours.
Recently, Danilovic
Danilovic etet al.
al. (2010)(2010) have
have presented
presented aa set
Recently,
setof local
local dynamo
dynamo simulations
simulations andand have
have compared
compared themof
themwith thethe results
results ofof Lites
Lites etet al.
al. (2007,(2007, 2008)2008) (see(see also
with
also
BelloGonzález
González etet al.
al. 2009
2009 forfor aa comparison
comparison between
between groundBelloground-Quiet	  Sun	
  magne0sm:	
  Hanle	  vs.	
  Zeeman	
  	
  
•
•
•
•
	
  

Hanle	
  “hidden”	
  turbulent	
  ﬁelds	
  (Stenﬂo,	
  Faurobert-­‐Scholl,	
  etc.):	
  >10	  G	  	
  Small	
  signals	
  observed	
  with	  no	
  spa0al	
  resolu0on	
  and	
  long	  integra0ons	  	
  Measurements	
  typically	
  made	
  at	
  10-­‐4.	
  Interpreta0on	
  is	
  model	  dependent.	
  
Sr	
  I	
  4607	
  Å,	
  	
  C2	
  5140	  Å	
  molecular	
  lines.	
  
No. 2, 2007
SCATTERING POLARIZATION OF Sr i l46
Trujillo	
  Bueno	  et	
  al.	
  2004	  Trujillo	
  Bueno	  et	
  al.	
  2007	
  Stenﬂo	
  1982	  Figure 1• Average	
  ﬁeld	  is	
  
≈	
  130	  G.	
  Granules	
  10	
  G	
  &	
  interganular	
  lanes	
  >	
  200	  G.	
  • Non	  ver0cal	
  (isotropic),	
  hectoGauss	
  ﬁelds	
  needed	
  for	  Hanle	  depolariza0on.	
  Hinode/SP	
  Quiet	  Sun	
  (Zeeman)	
  ﬁelds	  ≅	
  Hidden	
  turbulent	
  (Hanle)	
  ﬁelds	
  ?	
  
20

11/11/13	
  Fig. 1.—Emergent Q/I (top panels) and U/I (bottom panels) at the line
center of the SrSolar-­‐C	
  i l4607 line calculated for three lines of sight in a 3D snapshotof a realistic hydrodynamical simulation of solar surface convection and accounting for the diffraction limit effect of a 1 m telescope. The positive reference direction for Stokes Q lies along the vertical direction of the corresponding panel, which for the m p 0.1 and m p 0.5 cases coincides with theFig. 2.—Emergent Q
line calculated for a line
but taking into accountbulent magnetic field m12	
  bution.4 In the absen
between about 1%
m p 0.5 lies betwe

Quiet	  Sun	
  magne0sm:	
  Hanle	  vs.	
  Zeeman	
  	
  
•
•
•
•
•
•
	
  

Urgent:	
  Similari0es	
  between	
  the	
  Zeeman	
  QS	
  and	  Hanle	  QS	
  ﬁelds?	
  Shed	
  light	
  into	  their	
  origin:	
  Small-­‐Scale	
  Dynamo	
  (non-­‐helical)	
  Average	
  proper0es	
  are	
  similar:	
  there	  must	  be	
  a	
  rela0on	
  Zeeman-­‐inferred	
  QS	
  ﬁelds	
  are	
  episodic	
  (mesogranular)	
  Hanle-­‐inferred	
  QS	
  ﬁelds	
  are	  pervasive	
  in	
  0me	
  and	
  space	  (microturbulent?).	
  	
  Resolve	  Hanle	  QS	
  ﬁelds:	
  A	
  target	
  for	
  large	
  aperture	
  solar	
  telescopes.	
  
•

	
   •

10-­‐4	
  sensi0vity	
  in	
  Stokes	
  Q	
  &	
  U	
  	
  
Spectral	  resolu0on	
  50	
  mÅ	
  

No. 2, 2007•

Resolve	
  granular	
  evolu0on	
  (tens	
  of	
  seconds).	
  	
  

•

Resolve	
  granula0on	
  (Hinode	
  resolu0on	
  may	  be	  OK)	  •Zeeman	  (5250	  Å)	
  and	  Hanle	
  (Sr	  &	  C2)	
  lines	  simultaneously	
  

•

In	
  the	
  blue	  !	
  11/11/13	
  Solar-­‐C	  SCATTERING POLARIZATION OF13	
  4.-­‐	
  Solar	  Physics	
  from	  space:	
  opportuni0es	
  
	
  	
  
CDS (Coronal Diagnostic Spectrometer)
EIT (Extreme ultraviolet Imaging Telescope)
GOLF (Global Oscillations at Low Frequencies)
LASCO (Large Angle and Spectrometric
Coronagraph)
MDI (Michelson Doppler Imager)
SUMER (Solar Ultraviolet Measurements of Emitted
Radiation)
SWAN (Solar Wind Anisotropies)
UVCS (Ultraviolet Coronagraph Spectrometer)
VIRGO (Variability of Solar Irradiance and Gravity
Oscillations)

11/11/13	
  Solar-­‐C	  SOHO mission book(531 pages)14	  Measure	
  magne0c	
  ﬁelds	
  at	
  all	
  heights	
  	
  SOHO/MDI magnetograms described in 1 paragraph and 1 image
11/11/13	
  Solar-­‐C	
  

15	
  

CaII	  H	  imaging:	
  a	
  Hinode	
  success	
  story	
  	
  	
  

Dynamism of chromosphere is a major
Hinode discovery. Chromospheric
dynamics may generate disturbance tocorona: new implication to coronal heating(courtesy of Yukio Katsukawa)

The variation of Cn2 (h) with altitude is usually divided into two distinct "layers":

1. Ground Layer: ground-level effects like wind-surface interactions, diurnal solar heating,and various man-made effects at the telescope (e.g., "dome seeing")
2. Free Atmosphere: everything above the ground layer. An increase in the freeatmosphere Cn2 often seen at ~10km is due to strong wind shear at the Tropopause.
This plot above is the basis for saying that Mt. Graham, like many astronomical sites, has asignificant component "ground layer seeing".

6

Using the parameterization of Fried, the phase structure function can be written
DI (r ) 6.88 r / r05/ 3

r0 is the Fried Parameter (also called the "coherence length"), defined as
r00.185O 6 / 5 cos3/ 5 ] ª¬ ³ Cn2 (h)dh º¼

3/ 5

where ] is the zenith angle (]=0 at the zenith and S/2 at the horizon), O is the wavelength, and his the height above the ground. The Fried parameter is a measure of the aperture over which
there is approximately 1 radian of rms phase aberration, so it is a crucial parameter for describing
the "seeing" through a turbulent atmosphere.

The blue is hard from the ground: AO has a much harder job
11/11/13	
  Solar-­‐C	
  

16	
  

Measuring	
  B	
  at	
  the	  TR	  &	
  Corona:	
  Oﬀ	
  Disk	  • P.	
  Cargill@ISSI	
  (2008)	
  “moderate”	
  op0mism	
  on	
  Coronal	
  ﬁeld	  measurements:	  § `the	
  generality	
  of	
  the	
  sole	  SOLARC	
  published	
  result	
  	
  is	
  unclear´	  	  § `work	
  needs	
  to	
  be	
  done	  on	
  both	  the	
  details	
  of	
  the	
  atomic	
  physics,	
  and	
  how	  any	
  observaGons	
  would	
  be	
  interpreted	
  [ref.	
  Hanle]´	  • Both	  have	  happened	
  to	
  a	
  large	
  extent	  • Forbidden	
  line	  FeXIII	  10747	
  Å	
  oﬀ	
  disk,	  Hanle	  saturated.	
  Stokes	
  V	
  from	  Zeeman	  • 10-­‐4	
  was	
  needed	
  for	
  observa0ons	
  with	  arcsecs	  (texp	
  minutes	
  !)	
  • Eﬀorts	
  in	
  Sac	
  Peak+SOLARC+CoMP	  à	  ATST	
  (High	
  Resolu0on)	
  	
  Part I: direct coronal magnetic field measurement using NIR lines
The best
consistence
SOLARC	  	
   shown at layer 120

11/11/13	
  

CoMP	
  	
  

Solar-­‐C	
  

17	
  

Measuring	
  B	
  at	
  the	  TR	  &	
  Corona:	
  On	
  Disk	  The	
  list	  of	
  valid	
  windows	
  to	
  observe	
  TR	
  and	
  Coronal	
  ﬁelds	
  is	
  increasing	
  rapidly	
  	
  UV:	
  space	
  observaGons	
  Scauering	
  polariza0on,	
  Hanle	  eﬀect,	
  3D	
  transfer,	
  PRD,	
  etc	  included	
  in	
  modeling.	
  Magnetic field in the transition region
Outside	  Hanle	  satura0on,	
  full	  vector	  measurements	  are	
  possible	
   0.0
0.0
Ly-α:
-0.1
10 –
	
  On-­‐disk	
  measurements	
  are	  possible	
  (oﬀ-­‐disk	
  p-0.2
roved	  by	
  SUMER/SOHO)	
  -0.1
Hanle effect10 –in 90° scattering-0.3&	
  TR.	
  Stokes	
  V	
  expected	
  large.	
  k	
  
MgII	
  h	
  &	
  k	
  line	  (2795	  Å):	  	
  upper	
  candhromosphere	
  forward-0.2-0.4
scatteringclose todiskline	
  sensi0ve	
  to	
  Hanle	  eﬀect:	
  10-­‐100	
  G	
  ﬁetelds.	
  limb (µ=0.1)
center
-0.5(Trujillo Buenoal.
-0.3
2011, ApJ 738, L11)
1215.6
1216.01215.6
1216.01215.2
Scatteringpolarization(with RT in a semi-empirical atmosphere model) 1215.2• TheC	
  atmosphericIV	
  (1548	  Å):	
  “heights
Transi0on	
  region.	
  Stokes	
  V	
  measured	  in	
  wavelengththe	
  past.	
  
	
  
[Å]
wavelength [ Å ]of formation”
as the height
which
depth
Theoretical
Q/I profileof theh and alongk Linesthe LOS is unity)	  Mg• (definedNeed	
  beuer	
  tathan	  10the-­‐3	
  opticalfor	
  IIreliable	  d(1548):
iagnosis.	
  C IV
Zeeman-effect
•
•
•
•
•
•

6

6

56$6#

3

3

56$7

56$%

56$#

6
!6
"6
76
%6
#6
!66
#66

56$!

89:12;456$"

89:12;4

Q/I [%]

56$!

6
!6
"6
76
%6
#6
!66
#66

56$!#

56$"

56$"#

B [G]

B [G]

56$7

§ 6%

a

!"!#$&!"!#$'!
()*+,+-./01234"
Line CORE region!%&&&"' "&" (%&&&"' " "
%
%&
%&& "
)*+,-./0"$/12*,-."3-*04-2,*28-,9"-2":";<"=%!>?"@A/,"567,7586*+-."0*)*0
27+$/0-B*4",7"$*4-/2")/0C*kb!"!#$%

"

§ 2%

"

PRD
signaturehSign-reversal""!"#$ "

!"!&

&P&&>

subordinate lines (a and b) originate in the low chromosphere.

!"!#$"!"!#$%!"!#$&!"!#$'!
()*+,+-./01234!"!&!"!&$":";<"=%!>?"@AH
892,6*8-B*4"Q,7M*8"V&P&&&-2,*1+/,*4-2"%P!"J"%P!"#$I"=0*3,"R7J*8A7)*+"%I"$-2!&P&&I!&P&&>"

11/11/13	
  Solar-­‐C	
  According to this rough estimation of the “height of formation”,
the Mg II

!"!#

&P&&I

,75")-*D"73"5/+,"73"EF"#GF"8-$C0/,-72H"I?"#$"J"I?"#$
Solar magnetism eXplorer (SolmeX)

Physics involved:
The cores of the Mg IITrujillo	  h & k lines“originate”
at the bottom of the solar
Bueno’s	
  gTwo-Termroup	
  transition
while
the cores of the CaModel
II H &atom
K lines “originate” in• Partialregion,
frequency
redistribution
significantly
deeper layers of the solar atmosphere.
• J-state interference!"!&$"

27-8*"0*)*0H"&P&&%
!I&

&
I&
>&
D/)*0*21,6"86-3,""LM$N8O– arXiv 1108. 5304

K&H.	
  Peter	  (2012)	
  
18	
  

hp et al. (2011)

Overall pattern!"!#$"

Q,7M*8"V"N"$/J=Q,7M*8"IA!"!#

Measuring	
  B	
  at	
  the	  TR	  &	
  Corona:	
  On	
  Disk	  • HI	
  Lyα	  (1215	
  Å)	
  oﬀ	
  disk	  will	  provide	  full	  vector	
  in	
  the	
  range	
  10-­‐100	
  G	
  for	  1	  Rsun	
  	
  	
  
• HI	
  Lyα	  (1215	
  Å)	
  on	
  disk	  transi0on	
  region:	
  full	  vector	
  in	
  the	
  range	
  10-­‐100	
  G	
  	
  
• HeII	  Lyα	  (304	  Å)	
  on	
  disk	  transi0on	
  region:	
  full	  vector	
  in	
  the	
  range	  100-­‐1000	
  G	
  Magnetic
field
in coronal loops
• Fe	
  X	
  (174	  Å):	  on	  disk.	
  Hanle	  satura0on	
  but	  orienta0on	
  
can	
  
be	
  direction
obtained.	
  ► Upward collisional transfer of optically-pumped ground-level polarization→ linear polarization• Japanese	
  led	
  CLASP	
  eﬀort	  	
  ► Hanle effectsensitive to the magnetic field orientation→ modifies linear polarization
Magnetic field in the transition region► works also on disk !
(in ground-level saturation regime)

0.06

-0.3

56$7

56$%
-0.4

!"!#

!"!#$"

56$!#

56$"
-0.2

close tolimb (µ=0.1)

B [G]1215.2

6
!6
"6
76
%6
#6
!66
#66

!"!#$&!"!#$'!"!&!"!&$"
1215.6
1216.0()*+,+-./01234
wavelength [ Å ]!"!#$%

!

56$"#

!"
disk
center

B [G]

56$7
-0.3
!"!#

!"!#$"

1215.2""!"#$ "

Manso Sainz & Trujillo Bueno (2009)

Solar magnetism eXplorer (SolmeX)&P&&>:";<"=%!>?"@AH
892,6*8-B*4"Q,7M*8"V

Manso	
  Sainz’s	
  
idea	
  

– arXiv 1108. 5304

&P&&I
&P&&&
!&P&&I!&P&&>-2,*1+/,*4-2"%P!"J"%P!"#$I"=0*3,"R7J*8A7)*+"%I"$-2
27-8*"0*)*0H"&P&&%

hp et al. (2011)

"

0.001
106
107
108
109
Ne (cmN-3e) [ cm–3 ]electron density

TRACE
17.1 nm

Q,7M*8"V"N"$/J=Q,7M*8"IA

"

10-3

!

C IV (1548): Zeeman-effect"!%&&&"' "&" (%&&&"' " "
%
%&
%&& "
)*+,-./0"$/12*,-."3-*04-2,*28-,9"-2":";<"=%!>?"@A/,"567,7586*+-."0*)*0
27+$/0-B*4",7"$*4-/2")/0C*

0.100

surface
(h=0)

0.010

!"!#$&!"!#$'!"!&!"!&$"
1215.6
1216.0()*+,+-./01234
wavelength [ Å ]!"!#$%

1.000

h / RSun=0.2
0.1
0.05

4•108 cm-3

6
!6
"6
76
%6
#6
!66
#66

10 –3

56$!
-0.1
89:12;4

89:12;4

56$"
-0.2

56$#
-0.5

(Trujillo Bueno et al.
2011, ApJ 738, L11)

10 –3

Q/I (%)– 13 –

56$!
-0.1

Q/I [%]

Ly-α:
Hanle effectin 90° scatteringand forward
scattering

10.000

56$6#

Stokes Q / I [ % ]0.06

Fig. 4.— The sensitivity to the Hanle eﬀect of the scattering polarization amplitudes in" 11/11/13	
  !I& line of& He ii (solidI&>& Left K&
theLy-α line of H i (dotted lines) and in the Ly-αlines).
panel:
Solar-­‐C	  ,75")-*D"73"5/+,"73"EF"#GF"8-$C0/,-72H"I?"#$"J"I?"#$
D/)*0*21,6"86-3,""LM$N8O
horizontal magnetic field with random azimuth for a close to the limb scattering geometry
Solar magnetism eXplorer (SolmeX) – arXiv 1108. 5304
(with µ = 0.3). The positive reference direction for Stokes Q is the parallel to the nearest
limb. Right panel: horizontal field with fixed azimuth for the case of forward scatteringgeometry (µ = 1). The positive reference direction for Stokes Q is along the magnetic field.

Trujillo	
  Bueno	  et	
  al.	
  
19	
  

How	
  do	
  we	
  best	  combine	  Solar	  Physics	
  eﬀorts?	
  	
  ⽇日⽶米共同・国際観測ロケット実験
Chromospheric Lyman-Alpha
SpectroPolarimeter (CLASP)
ミッション提案書

Solar magnetism eXplorer (SolmeX)
Exploring the magnetic fieldin the upper atmosphere of our closest star

CLASP  チームpreprint at

arXiv 1108.5304(Exp.Astron.)or search for“solmex” in ADS

Hardi Peter& SolmeX teampreProposal in response to the 2010 callfor a medium-size mission opportunity
in ESA’s science programme
for a launch in 2022.
Solar magnetism eXplorer (SolmeX) – arXiv 1108. 5304

11/11/13	
  Solar-­‐C	
  

20	
  

5.-­‐	
  Solar	  C	
  &	
  ATST	  	
  	
   Observing Modes of ATST: DST, Hinode, AIA"
Access	  Mode	  Service	  Mode	  Facility	  Mode	  • PI present"• Dedicated time"• PI runs facility"• Proprietary data"• PI at remote site"• Dynamic scheduling"• RA runs queue "• Open data policy"• No PI"• Dynamic scheduling"• RA selects program "• Open data policy"

Install New Instrument"
Inst. Scientist Training"""

Nominal Science Mode"

Unscheduled Time"
Test/Develop new Programs"
Poor weather/seeing"~ 10%"~ 80%"

"
"
"
"

"
"

~10% ??"

ATST operates ~ space missions: ATST+Solar-C common TAC?
11/11/13	
  Solar-­‐C	
  

21	
  

	
  Conclusions	  1. ATST construction is running at full speed: 2019
2. Spectropolarimetry will do lots of science above
the diffraction limit.
3. Keep emphasizing observations of the vector
magnetic field
4. The blue side of the spectrum will always be hardfrom the ground
5. Maximize collaborations among major projects
6. Solar-C+ATST common Time Allocation Committee?

11/11/13	
  Solar-­‐C	
  

22	
  

有難う 御座います

11/11/13	
  Solar-­‐C	
  

23	
  

11/11/13	
  Solar-­‐C	
  

24	
  

We	
  are	
  star0ng	
  to	
  explore	
  the	
  10-­‐4	
  limit	
  	
  

From	
  a	
  mixed-­‐polarity	
  ﬁeld	  ﬁlling	
  the	
  interiors	
  of	
  supergranular	  cells	
  to…	  11/11/13	
  Solar-­‐C	
  

25	
  

We	
  are	
  star0ng	
  to	
  explore	
  the	
  10-­‐4	
  limit	  	
  …ﬁelds	
  with	  a	
  dominant	
  transverse	
  component	
  evolving	
  in	
  granular	
  0mescales	
  	
  11/11/13	
  Solar-­‐C	
  

26	
  

We	
  are	
  star0ng	
  to	
  explore	
  the	
  10-­‐4	
  limit	  	
  Network	
  persists,	
  internetwork	
  evolves	
  with	  granula0on	
  and	  has	
  granular-­‐size	
  loop-­‐emergence	
  as	
  a	
  key	
  ingredient	
  11/11/13	
  Solar-­‐C	
  27