October 3, 2003IFIC, UVEG-CSIC A road map to solar fluxes, osc. param., and test for new physics Carlos Pena Garay IAS ~

October 3, 2003 IFIC, UVEG-CSIC

A road map to solar fluxes, osc. A road map to solar fluxes, osc. param., and test for new physicsparam., and test for new physics

Carlos Pena Garay

IAS

~

Why perform low-energy solar neutrino experiments?

Update : SNO 2nd phase data included

StrategyStrategy

- Global analyses of data : Indep. on SSM fluxes

Bahcall, Krastev, PRD53 (1996)

Garzelli, Giunti, PRD65 (2002)

1995 : Chlorine, SAGE, GALLEX, Kamiokande Large uncertainties of fluxes from neutrino data

2001 : Chlorine, SAGE, GALLEX, SK, SNO CC Bayesian Analysis : 5% p-p determination at 90% CL

2001 : pp SSM analysis of pp measurementNakahata, NOON 2001

Neutrino spectrumNeutrino spectrum

%1

%10%10

%5.1

%16%20

?

e

S + K

Solar + KamLAND : DataSolar + KamLAND : Data

1 Chorine 0.34 0.03 1 Sage + Gallex/GNO 0.54 0.03 44 Super-Kamiokande 0.465 0.015 SNO I CC* 0.35 0.02 34 SNO I NC* 1.01 0.13 SNO I ES* 0.47 0.05

• KamLAND 0.61 0.09

* undistorted spectrum assumed

1 SNO II CC 0.32 0.02 1 SNO II NC 1.03 0.09 1 SNO II ES 0.44 0.06

)f,,,m(1312

2

i

SSMi

i

,

if

CNO B, Be,pep, pp,i

8 7

S + K : Global analysesS + K : Global analyses

Global analyses : Variations on a theme

- B free- B , Be free- All free - All free + lum- - Cl , - Ga

7 8

8

LMA : Boron free analysisLMA : Boron free analysis

0.13)( 0.04 1.0 fB

0.42 tan 0.21

0.14-

0.05

0.04-

2

7.1 6.2

1.6-

0.4

0.4-

2

21

m

0.18)( 0.06 1.0 fB

0.45 tan 0.37

0.16-

0.07

0.06-

2

7.1 8.11

1.6-

0.6

0.4-

2

21

m

2

22

m

EnGeF

LMALMA

MeV8.1B)( 8 critE

MeV2.2Be)( 7 critE

MeV3.3(pp) critE

CHOOZ + ATM : CHOOZ + ATM : 13

13

4

213

4

3 sin cos )ν(P)ν(P

eeee

If nuclear fusion reactions among light elements are responsible for solar energy generation

i

ii

2

SUN

(A.U.)4

L

Spiro, Vignaud, PLB (1990)

determined by differences of nuclear masses independent of details of solar model at 1:104i

Bahcall, PRC (2002)

Luminosity constraintLuminosity constraint

CNO014.0

Be070.0

pp916.01

Global : Variations on a themeGlobal : Variations on a theme

0.47

0.75-

0.18

0.25-pp

1.27

0.13-

0.41

0.13-Be1.38 f ; 0.13 f

- S + K : All free + lum

0.06

0.06-

0.02

0.02-pp

0.80

0.93-

0.25

0.63-Be1.02 f ; 0.93 f

Amazing result ! Large uncertainty !

Luminosity constraint is relevant !

- S+ K : All free

LMA : Other analysesLMA : Other analyses

- S + K : All free + lum – Ga

0.09

0.08-

0.04

0.02-pp

0.76

1.24-

0.31

1.24-Be1.00 f ; 1.24 f

0.04

0.10-

0.02

0.04-pp

1.43

0.33-

0.64

0.33-Be1.05 f ; 0.33 f

Data don’t understand Be neutrinos !

- S + K : All free + lum – Cl

Do we really understand Be neutrinos?

LMA : Other determinationsLMA : Other determinations

- S + K : All free - luminosity from neutrino data

0.16R

R 0.18

0.16-

0.05

0.11-

33

34 0.174)(R

R

33

34 SSM

% 00. L 3.7

0.0-

8.2

0.0-CNO

Bahcall, Gonzalez-Garcia, CPG, PRL (2003)

1.4L/ L 7.0

0.6-

2.0

0.3-

v

- S + K : All free + lum

LMA : Predictions for Borexino LMA : Predictions for Borexino

- S + K : All free + lum

(SSM) 0.06 0.66][B 0.02

0.02- e

0.14

0.23-0.58][B e

Do we really understand Be neutrinos?

- S + K : B free

S + K 3 yrS + K 3 yr

25.0

62.0Be93.0f

02.0

02.0pp02.1f

24.0

6.0

2 eV3.7

m

04.0

04.0

2 41.0tan

22.0

2.0

2 eV3.7

m

04.0

03.0

2 41.0tan

Expected at BorexinoExpected at Borexino

10.0

11.0Be07.1f

008.0

008.0pp009.1f

[Be] = 0.66 10%

[Be] = 0.66 5%05.0

07.0Be09.1f

005.0

005.0pp008.1f

0.010

0.014-

33

34 0.19R

R 13.0701.L/ L v

2

22

m

EnGeF

Unexpected at low energy ?Unexpected at low energy ?

-NC NSI : Modified matter effects

Fogli et al (2002)

Berezhiani et al (2001)

Davidson et al (2003)

-Sterile : With low mass scale

Berezinsky et al (2003)

de Holanda, Smirnov (2003)

Expected : pp measurementExpected : pp measurement

[pp]= 0.70 5%

[pp]= 0.70 1%

0.41 tan 0.15

0.09-

0.04

0.03-

2

04.0990.L/ L v

0.42 tan 0.07

0.06-

0.02

0.02-

2

02.0990.L/ L v

SummarySummary

7 Experiments; 34 years; 0.01% of the flux.

A solar neutrino “opportunity”; not a problem.

Free fluxes: with luminosity constraintFree fluxes: with luminosity constraintFree fluxes: with luminosity constraintFree fluxes: with luminosity constraint

CNO014.0

Be070.0

pp916.01

i ii2

SUN (A.U.)4L

)(1 0.02 1.01 pp

)(1 0.97 0.25

0.63

Be

)(1 0.04 1.01 B

Why measure low-energy solar `s?

0.25

0.63-

7 0.93 )( Be• (today)

Unique test of stellar fusion reactions•

Test for vacuum-matter transition•

• Measure solar luminosity via `s Explore for new physics (steriles, NSI)•

• precisely Measure 12

pp Be7

ConclusionsConclusions

Next I SNO 2nd phase

- Status of maximal mixing

- Matter effects Next I KamLAND reactor : determination

Next II Low energy : challenge

- 99.99 % of solar neutrinos E < 5 MeV

- Redundancy + improvement : Identify the unexpected

- Vacuum av. osc.

- Luminosity constraint + [ Be] 5% + [p-p] 1-3%

7

12

2m

:Significant improvement

But…

SSM dependent

+ p-p (pep) measurement : SSM+ p-p (pep) measurement : SSM

Nakahata, NOON 2001

02.002.1f/

peppp

S + K 3 yr :

S + K 3 yr + [Be] 5 %005.0

006.0/009.1f

peppp

Larger unc. than SSM

Smaller unc. than SSM !!!

Higher sensitivity to pp/pep:

CNOBepepppf01.0f08.009.1f

/

Luminosity constraintLuminosity constraint

: Significant improvement

and…

SSM independent at < 0.01 %

% 5 % 11 :tan 2

+ p-p (pep) measurement+ p-p (pep) measurement

7 7 Be measurement at 5 %Be measurement at 5 %

06.0

07.0Be08.1f

005.0

006.0pp009.1f

,2mNot improved

But !

Better sensibility

Small CS uncertainty

[X] ~ P CC ee

e[X] ~ P + f (1-P ) ee ee

Low Energy exps : ES, CCLow Energy exps : ES, CC