why do we need to continue to measure solar neutrinos ?

Why do we need to continue to measure solar neutrinos ?

Why a need for low energy measurements

Sylvaine TURCK-CHIEZE Blackburg 2006

Flux Tc Y initial Problem solved1988 3.8 ± 1.1 15.6 SM 0.276 CNO opacity, 7Be(p,g)1993 4.4 ± 1.1 15.43 SM 0.271 Fe opacity, screening1998 4.82 15.67 SM 0.273 Microscopic diffusion1999 4.82 15.71 SM 0.272 Turbulence in tachocline2001 4.98 ± 0.73 15.74 0.276 Seismic model2003 5.07 ±0.76 15.75 0.277 Seismic model +magnetic field2004 3.98. ± 1.1 15.54 SM 0.262 - 30% in CNO composition- 5.31 ±0.6 15.75 0.277 Seismic model +magnetic

field+ updated ingredientsSNO results1988 5.44 ± 0.99 (CC+ES 2001) 19895.09 ±0.44 ±0.45 (NC 2002) 5.27 ±0.27 ±0.38 (2003)19904.94 ±0.06 ±0.34 active neutrinos Aharmim et al, 2005

Direct comparison for 8B neutrinosgreat sensitivity to the central temperature so to the detailed

physics of the radiative zone

We have seen the oscillation between electron neutrino and others and we control now central temperature at 3 per mille


Prediction for the other detectorswithout or with Neutrino Oscillation parameters

Chlorine detector Seismic model 2001 Detected neutrinos Detect. Seismic 2004pep 0.228 57% 0.13 0.137Be 1.155 57% 0.66 0.668B 5.676 31% 1.76 1.8813N 0.096 57% 0.054 0.02215O 0.328 57% 0.187 0.112total 7.44 SNU (1.1) 2.79 SNU (0.36) 2.76 (0.4) SNU

Measurement 2.56 (0.23) SNU

Gallium detector Seismic model Detected neutrinos Detect. Seismic 2004pp 69.4 57% 39.6 39.6pep 2.84 57% 1.62 1.627Be 34.79 57 % 19.83 19.838B 11.95 31% 3.70 3.9513N 3.48 57% 1.98 0.7915O 5.648 57% 3.22 1.29total 128.2 SNU (8) 69.95 SNU 67.08 (4.4) SNU

Measurement 68.1 SNU (3.75)LMA solution m2= 7 10-5 eV2 (8+0.6-0.4) tg212=0.45 BPG2003


radius

The Solar Neutrinos

radius

No

rmal

ized

flu

x (d

Fx/

dr)

pp chain

CNO cycle

Flu

x (/

cm2 /s

/M

eV o

r /c

m2 /

Mev

fo

r li

nes

)

4p -> 4He + 2e+ +2 e + E

8B

7Be

hep pp

17F

15O 13N

radius

E about 6.4% of the total energy

No

rmal

ized

flu

x (d

Fx/

dr)

pp chain

CNO cycle

Neutrino energy (MeV)

Flu

x (/

cm2 /s

/M

eV o

r /c

m2 /

Mev

fo

r li

nes

)

4p -> 4He + 2e+ +2 e + E

8B

7Be hep

pp

17F

15O 13N

radius


• 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


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


- CNO abundances ?? 30% reduction

- Contribution of 9Be in oxygen lines

3D simulations

Asplund et al 2004, 2006

Sylvaine Turck-Chièze, Blacksburg 2006 8

Solar composition in C, N, O recently reduced by 30%

If it is true, the Sun is no more an « enriched » star in heavy

elements: a new problem solved

8B standard model neutrino flux = 4 106 cm-2s-1

8B seismic model = 5.31 106 cm-2s-1

One needs to add new physics to understand the sound speed:

Is it a manifestation of dynamical processes or opacity problems ?

Turck-Chièze et al. 2004


Solar neon abundance ? Probably not

Seismic data may help to solve the problem

In examining the adiabatic exponent 1 ?

Antia & Basu 2006 not totally sure Neutrinos can help to verify


Beyond the standard model of stellar evolution

Sylvaine Turck-Chièze, Blackburg 13 th October 2006

A new vision of Sun and stars

1D and 3D modelling

Seismic measurements

where

4 structure equations will be

replaced by

16 equations

Neutrino astronomy


Montmerle 2000

?

Rotation profile constructed with GOLF+MDI / SOHO acoustic modes and gravity modes

- 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 ?…

What we would like to know ?

?

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 ??

Development of 3D MHD simulations to understand the internal observations

PhotosphereTachocline 4-5% massCouvidat et al. 2003 Thompson et al. 1996, Kosovichev 1997

ZC: 2% M

CZRZ

94%

New models of the Sun

Sylvaine Turck-Chièze IAU Sydney, July 14th

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

The DynaMICS* perspective

Global 3D vision of the Sunfor 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, Jimenez-Reyes, 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 scalesMillions 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

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.

Schwabe cycle

Gleissberg cycle

Suess cycle

11 years

90 years

200 years

Sum of the components

T( °C)

We must verify and put constraints on the origin of the different cycles…

30% of the total effect ???

Indirect effect not estimated ?

Damon & Jirikowic, 1992

years

Fröhlich & Lean 2004

TSI variation 0.1% through 11 year cycle, long trend ?? Standard model: 10-8 in 100 years

Transport processes in radiation zonesMeridional 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)

Magnetic field

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)

Secular torque(Charbonneau & Mac Gregor 1993,Garaud 2002)

Instabilities(Maeder & Meynet 2004, Braithwaite & Spruit 2005, Brun & Zahn 2006)

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 …

Lockwood 2004

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

Surface Angular Velocity

Present Sun

Mid 1600’s Sun(Maunder Minimum)

Extrapolated Curvefrom 3D Models

• a magnetic energy of about 5-7% of the kinetic energy leads to a correct slowing down

•Eddy et al. (1976) showed that during the Maunder minimum the Sun was rotating 4% faster than today

Brun 2004, Solar Physics

SDO, PICARD, Solar Orbiter and DynaMICS1.B – Convective dynamics.

1.C – Global Circulation

1.D – Irradiance Sources

1.H – Far-side Imaging

1.F – Solar Subsurface Weather

1.E – Coronal Magnetic Field

1.I – Magnetic Connectivity

1.J – Sunspot Dynamics

1.G – Magnetic Stresses

1.A – Interior Structure

NOAA 9393

Far-side

Chromosphere

Magnetism Radiative region

Rotation of the core

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

why do we need to continue to measure solar neutrinos ?

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