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
~
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
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
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
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 !