Transcript file

Why do we need to continue
to measure solar neutrinos ?
Why a need for low energy
measurements
Direct comparison for 8B neutrinos
great sensitivity to the central temperature so to the detailed
physics of the radiative zone
1988
1993
1998
1999
2001
2003
2004
2004
Flux
Tc
Y initial
3.8 ± 1.1
4.4 ± 1.1
4.82
4.82
4.98 ± 0.73
5.07 ±0.76
3.98. ± 1.1
5.31 ±0.6
15.6
15.43
15.67
15.71
15.74
15.75
15.54
15.75
SM
SM
SM
SM
SM
Problem solved
0.276
0.271
0.273
0.272
0.276
0.277
0.262
0.277
CNO opacity, 7Be(p,g)
Fe opacity, screening
Microscopic diffusion
Turbulence in tachocline
Seismic model
Seismic model +magnetic field
- 30% in CNO composition
Seismic model +magnetic
field+ updated ingredients
SNO results
- 5.44 ± 0.99 (CC+ES 2001)
- 5.09 ±0.44 ±0.45 (NC 2002) 5.27 ±0.27 ±0.38 (2003)
- 4.94 ±0.06 ±0.34 active neutrinos
Aharmim et al, 2005
We have seen the oscillation between electron neutrino and others and we
control now central temperature at 3 per mille
Sylvaine TURCK-CHIEZE Blackburg 2006
Prediction for the other detectors
without or with Neutrino Oscillation parameters
Chlorine detector
Seismic model 2001
Detected neutrinos Detect. Seismic 2004
pep
0.228
57%
0.13
0.13
7Be
1.155
57%
0.66
0.66
8B
5.676
31%
1.76
1.88
13N
0.096
57%
0.054
0.022
15O
0.328
57%
0.187
0.112
total
7.44 SNU (1.1)
2.79 SNU (0.36) 2.76 (0.4) SNU
Measurement 2.56 (0.23) SNU
Gallium detector
pp
pep
7Be
8B
13N
15O
total
Seismic model
69.4
2.84
34.79
11.95
3.48
5.648
128.2 SNU (8)
Detected neutrinos
Detect. Seismic 2004
57%
39.6
39.6
57%
1.62
1.62
57 %
19.83
19.83
31%
3.70
3.95
57%
1.98
0.79
57%
3.22
1.29
69.95 SNU
67.08 (4.4) SNU
Measurement 68.1 SNU (3.75)
LMA solution Dm2= 7 10-5 eV2 (8+0.6-0.4) tg2q12=0.45 BPG2003
Sylvaine TURCK-CHIEZE Blackburg 2006
The Solar Neutrinos
4p ->
-> 44He
He ++ 2e
2e++ +2
+2 nne ++ E
E
4p
e
nn 88B
B
pp
ppchain
chain
7
7
Be
nn Be
n hep
n hep
pp
nn pp
n 17F
n 17F
CNO
CNOcycle
cycle
n 15O
n 15O
radius
radius
radius
radius
nn1313
NN
2 /s
2 /s
/MeV
Flux
(/cm
/MeVoror
Flux(/cm
2
/cm
lines)
forlines)
/cm/2Mev
/ Mevfor
Normalized
(dFx/dr)
flux(dFx/dr)
Normalizedflux
En about 6.4% of the total energy
Neutrino energy (MeV)
Sylvaine TURCK-CHIEZE Blackburg 2006
• Only mean value for decades
• Sum of a lot of components
• 7Be line will be a first step to check
oscillation parameters
• But we need also to look for subleadings
effects: 10% or less
Sylvaine TURCK-CHIEZE Blackburg 2006
What we know ?
- Laboratory cross sections (3He, 3He; 12C, p)
- Opacity calculations
- Acoustic modes=>
Sound speed profile: photospheric 4He,
pp reaction rate,
energy transfer
- Seismic model
compatible with observed
sound speed for determining
neutrino fluxes compatible
with acoustic modes
Turck-Chièze et al. 2001;
Couvidat et al. 2003
Sylvaine TURCK-CHIEZE Blackburg 2006
-
-
CNO abundances ??
30% reduction
Contribution of 9Be in
oxygen lines
3D simulations
Asplund et al 2004, 2006
Sylvaine TURCK-CHIEZE Blackburg 2006
Solar composition in C, N, O recently reduced by 30%
Turck-Chièze et al. 2004
If it is true, the Sun is no more an
« enriched » star in heavy
elements: a new problem solved
8B
One needs to add new physics to
understand the sound speed:
Is it a manifestation of dynamical
processes or opacity problems ?
standard model neutrino flux = 4 106 cm-2s-1
8B seismic model = 5.31 106 cm-2s-1
Sylvaine Turck-Chièze, Blacksburg 2006
8
Solar neon abundance ? Probably not
Seismic data may help to solve the problem
In examining the adiabatic exponent G1
Antia & Basu 2006
?
not totally sure Neutrinos can help to verify
Sylvaine Turck-Chièze, Blacksburg 2006
9
Beyond the standard model of
stellar evolution
Sylvaine Turck-Chièze, Blacksburg 2006
10
A new vision of Sun and stars
Neutrino
astronomy
1D and 3D
modelling
Seismic
measurements
where
4 structure
equations will be
replaced by
16 equations
Sylvaine Turck-Chièze, Blackburg 13 th October 2006
Rotation profile constructed with GOLF+MDI / SOHO
acoustic modes and gravity modes
?
?
Montmerle 2000
What we would like to know ?
- The latitudinal rotation of the inner radiative zone
- Is there a relic of the formation of the solar system which
justifies an higher central rotation profile ?
- Could we get real constraints on the magnetic configurations
in the radiative zone and convective zone
- Is there a dynamo in the core ?…
Sylvaine Turck-Chièze, Blackburg 13 th October 2006
Magnetic field and Evolution of stellar modelling
The tachocline plays an important role in the stockage and amplification of the toroidal
magnetic field for the Schwabe cycle 22 ans, one would like to know what phenomena can
justify the possible existence of the Gleissberg cycle (90 year ?) or greater cycles ??
Photosphere
Tachocline
Couvidat et al. 2003 Thompson et al. 1996, Kosovichev 1997
4-5% mass
ZC: 2% M
94%
RZ
CZ
Development of 3D MHD simulations to understand the internal observations
New models of the Sun
Magnetic Solar Cycle 23
(EIT, LASCO & MDI Data)
Source: Soho
Source: NASA
Sylvaine Turck-Chièze
IAU Sydney, July 14th
Butterfly Diagram and Coronal Holes
(HAO/SMM & EIT Data)
Source: Soho
Sylvaine Turck-Chièze
IAU Sydney, July 14th
The DynaMICS*
perspective
Global 3D vision of the Sun
for knowing the origins of the different
solar magnetic cycles and connect the
interior part to the external part
Turck-Chièze, S.1, Schmutz, W.2, Thuillier, G.3, Jefferies, S4, Palle, P.L.5, Dewitt, S.6,
Ballot, J.1, Berthomieu, G.7, Bonanno, A.8, Brun, A. S.1, Christensen-Dalsgaard, J.9,
Corbard, T.7, Couvidat, S.10, Darwich, A. M.5, Dintrans, B. 11, Domingo, V.12, Finsterle,
W.2, Fossat, E.7, Garcia, A. R.1,Gelly, B.5, Gough, D.13, Guzik, J.14 Jimenez, A.5, JimenezReyes, S.J.5, Kosovichev, A.10, Lambert, P.1, Lefebvre, S. 1, Lopes, I.15, Martic, M.3,
Mathis, S.16, Mathur, S.1, Nghiem, P. A. P.1, Piau, L.17, Provost, J.7, Rieutord, M.11,
Robillot, J. M.18, Rogers, T. 19, Roudier, T.20, Roxburgh, I.21, Rozelot, J. P.7, Straka, C.22,
Talon, S. 23, Théado, S.24,Thompson, M.25, Vauclair, S.11, Zahn, J. P.15
1CEA,
FRANCE; 2PMOD/WRC, Davos, SWITZERLAND, 3Service d'Aéronomie, FRANCE, 4Dipartimento di Fisica
University of Hawai, USA, 5IAC, SPAIN,6RMIB, BELGIUM, 7Observatoire Cote d'Azur, FRANCE, 8Osservatorio
Astrofisico di Catania, ITALY, 9Aarhus Universitet, DENMARK; 10HEPL, Stanford, UNITED STATES, 11OMP Toulouse,
FRANCE, 12Universidad Valencia, SPAIN, 13Cambridge, UNITED KINGDOM, 14Los Alamos National Laboratory, USA,
15Istituto Superior Técnico, Lisboa, PORTUGAL, 16LUTH Meudon, FRANCE; 17Dept of A.&A., Chicago, UNITED
STATES, 18Observatoire de Bordeaux, FRANCE, 19AA Department San Diego, USA, 20Laboratoire d'Astrophysique de
Tarbes, 21Queen Mary, University of London, UNITED KINGDOM, 22 Yale, USA, 23Université Montréal, CANADA, 24
Observatoire de Liège, BELGIUM,25University of Sheffield, UNITED KINGDOM.
* Dynamics and Magnetism from the inner Core to the chromosphere of the Sun
We are going from the large scales
Millions or billions of years
To
Centuries or even low variabilities
Where all the instabilities due to rotation or
magnetic field or gravity waves are present
This is useful not only for the Sun but for any stellar
system, binary systems presupernovae
Sylvaine Turck-Chièze, Blackburg 13 th October 2006
DynaMICS with SDO will aim at revealing the different sources of dynamo
down to the core, the interplay of internal magnetic fields and a better
knowledge of the transition region between photosphere and chromosphere.
It must result an improved understanding of the solar activity cycles, including
large minima and maxima with predictions for the next century and a better
description of the Sun’s potential impact on earth’s climate change.
We must verify and put constraints on
the origin of the different cycles…
30% of the total effect ???
DT( °C)
Suess cycle
Gleissberg cycle
200 years
90 years
Schwabe cycle
11 years
Sum of the components
years
Damon & Jirikowic, 1992
Indirect effect not estimated ?
Fröhlich &
Lean 2004
TSI variation 0.1% through
11 year cycle, long trend ??
Standard model: 10-8 in 100 years
Transport processes in radiation zones
Meridional circulation (diff. rot. and A. M. transport) (ADVECTION)
(Busse 1981, Zahn 1992, Maeder & Zahn 1998,
Garaud 2002, Rieutord 2004)
Turbulence (shear of the diff. rot.) (DIFFUSION)
(Talon & Zahn 1997, Garaud 2001, Maeder 2003)
Secular torque
(Charbonneau & Mac Gregor 1993,
Garaud 2002)
Magnetic field
Instabilities
(Maeder & Meynet 2004, Braithwaite &
Spruit 2005, Brun & Zahn 2006)
Internal waves
(Talon et al. 2002,
Talon & Charbonnel
2003-2004-2005,
Rogers et al. 2005)
excited at the borders with C. Z.
propagating inside R. Z.
A. M. settled where they are damped
(Goldreich & Nicholson 1989)
New questions
What type (s) of global dynamo(s) exist in the Sun
Role of Meridional Circulation flows in the radiative zone?
What kind of magnetic instabilities exist in the radiative zone ?
What are the interactions between « fossil » inner field and the
dynamo generated in the convective zone?
The real role of the gravity waves
Astrophysical Consequences :
- important consequences on the other stars (PNPS),
presupernovae
- role of dark matter, research of sterile neutrino or
sub leading properties of neutrinos …
DynaMICS will put constraints on the energetic balance in
the radiative zone and in the convective zone
first milestone to improve the earth climate modelling
Lockwood 2004
Surface Angular Velocity W
Extrapolated Curve
from 3D Models
Mid 1600’s Sun
(Maunder Minimum)
Present Sun
Brun 2004, Solar Physics
•Eddy et al. (1976) showed that during the Maunder minimum the Sun was rotating 4%
faster than today
• a magnetic energy of about 5-7% of the kinetic energy leads to a correct slowing down
SDO, PICARD, Solar Orbiter and DynaMICS
1.B – Convective dynamics.
1.C – Global Circulation
1.J – Sunspot Dynamics
1.I – Magnetic Connectivity
1.A – Interior Structure
Chromosphere
1.D – Irradiance Sources
Rotation
of the
core
1.H – Far-side Imaging
1.E – Coronal Magnetic Field
Magnetism
Radiative
region
NOAA
9393
Farside
1.G – Magnetic Stresses
1.F – Solar Subsurface Weather
DynaMICS observables
• The objectives require continuity and stability to measure low signals and
small variability of important global quantities
– gravity modes to improve the core and the tachocline dynamics
– acoustic modes to follow the variability of the rotation in the
convective zone and below the tachocline and the latitudinal
dependence
– time evolution of radius (if measurable)
– shape deformations if measurable
– solar irradiance at different wavelengths from visible to far UV
simultaneously.
– global magnetic field evolution from the photosphere up to the
chromosphere or above through lines deformations
In this perspective
• Low neutrinos spectrum will play an
important role
• 13N, 15O, pp are important indicators
For potential variabilities