α Solar Neutrino Road Map Carlos Pena Garay IAS ~ February 11, 004 NOON004
Be + p-p p p (pep) measurements Why perform low-energy solar neutrino experiments? Amazing progress on how the Sun shines, the determination of neutrino parameters, and tests of new physics in the neutrino sector requires the measurement of two neutrino fluxes Low energy Be : 10 % - 5% + Low energy pp (pep) : 5 % - 1%
BP04 Bahcall, Pinsonneault, astro-ph/040114 pp (10 10 cm - s -1 ) pep (10 8 cm - s -1 ) hep (10 3 cm - s -1 ) Be (10 9 cm - s -1 ) 8 B (10 6 cm - s -1 ) 13 N (10 8 cm - s -1 ) 15 O (10 8 cm - s -1 ) 1 F (10 6 cm - s 1 ) Cl Ga 5.94 (1%) 1.40 (%).88 (16%) 4.86 (1%) 5.8 (3%) 5.1 (36%) 5.03 (41%) 5.91 (44%) 8.5 1.8 SNU 131 11 SNU
BP04 Bahcall, Pinsonneault, astro-ph/040114 Fractional uncertainties in calculated neutrino fluxes Source 3-3 3-4 1-14 Z/X 1- pp Be 8 B 13 N 15 O 0.00 0.03 0.01 0.001 0.001 0.005 0.080 0.05 0.004 0.004 0.000 0.000 0.001 0.118 0.143 0.010 0.080 0.00 0.33 0.35 0.038 S 34 better than 5% (factor improvement) Surface abundances less than 0.0 dex (factor 3 improv.) S 1,14 better than 5%
Data S + K Solar (normalized to BP04) 1 Chorine 0.30 0.03 1 Sage + Gallex/GNO 0.53 0.03 44 Super-Kamiokande 0.403 0.013 SNO I CC* 0.30 0.0 34 SNO I NC* 0.88 0.11 SNO I ES* 0.41 0.04 KamLAND 0.61 0.09 * undistorted spectrum assumed 1 SNO II CC 0.8 0.0 1 SNO II NC 0.89 0.08 1 SNO II ES 0.38 0.05
Global analyses of data : Indep. on SSM fluxes Test of null hypothesis for solar neutrino conversion Spiro-Vignaud, Hata et al, Castellani et al, Including neutrino conversion 1995 : Chlorine, SAGE, GALLEX, Kamiokande Large uncertainties of fluxes from neutrino data Bahcall, Krastev, PRD53 (1996) 001 : Chlorine, SAGE, GALLEX, SK, SNO CC Bayesian Analysis : 5% p-p determination at 90% CL Garzelli, Giunti, PRD65 (00) 001 : pp SSM analysis of pp measurement Nakahata, NOON 001
Luminosity constraint α i If nuclear fusion reactions among light elements are responsible for solar energy generation and using that D and 3 He are in local kinetic equilibrium L SUN 4π (A.U.) i α i Φ i Spiro, Vignaud, PLB (1990) determined from nuclear masses and neutrino energies independent of details of solar model at 1:10 4 Bahcall, PRC (00) 1 0.918 f + 0.069 f + 0. 013 pp Be f CNO
Why perform low-energy solar neutrino experiments? Bahcall, PG, JHEP03 Only neutrinos can enable us to see into the interior of a star f B f pp f Be 0.88 0.04 1.0 0.0 0.4 0.91 + -0.6 Be f pp f Be 1.010 0.005 0.05 1.0 + -0.0 tan θ 1 High precision neutrino flux, annually modulated + 0.05 0.4-0.04 ( + 0.1) -0.14 Be,pp tan θ 1 + 0.0 0.4-0.0 ( + 0.0) -0.06 Test of vacuum matter transition. Explore for new physics
Some tests of SSM - Data + luminosity constraint R R 33 34 ( SSM ) 0.18 R 34 + 0.16 0.05-0.11 R 33 0.0 Be,pp L CNO (SSM) 1. 6 0.6% R R 34 0.19 33 0.01 L CNO 0. 0 +.8-0.0 ( +.3 )% -0.0 ( Be + 1.1 + 3.9 L 0. 0 )% CNO -0.0-0.0 Bahcall, Gonzalez-Garcia, PG, PRL (003) - Data w/o constraint L v / L γ 1.4 + 0. Be,pp -0.3 L / L 0. 99 v γ 0.0
Why perform low-energy solar neutrino experiments? Bahcall, PG, JHEP03 Only neutrinos can enable us to see into the interior of a star f B f pp f Be 0.88 0.04 1.0 0.0 0.4 0.91 + -0.6 Be f pp f Be 1.010 0.005 0.05 1.0 + -0.0 tan θ 1 High precision neutrino flux, annually modulated + 0.05 0.4-0.04 ( + 0.1) -0.14 Be,pp tan θ 1 + 0.0 0.4-0.0 ( + 0.0) -0.06 Test of vacuum matter transition. Explore for new physics
Be + p-p p p (pep) measurements θ : Significant improvement tan θ : 11% 5% and SSM independent at < 0.01 %
Why perform low-energy solar neutrino experiments? Bahcall, PG, JHEP03 Only neutrinos can enable us to see into the interior of a star f B f pp f Be 0.88 0.04 1.0 0.0 0.4 0.91 + -0.6 Be f pp f Be 1.010 0.005 0.05 1.0 + -0.0 tan θ 1 High precision neutrino flux, annually modulated + 0.05 0.4-0.04 ( + 0.1) -0.14 Be,pp tan θ 1 + 0.0 0.4-0.0 ( + 0.0) -0.06 Test of vacuum-matter transition. Explore for new physics
LMA : Vacuum to adiabatic transition β G n m E F e ν E crit ( 8 B) 1.8 MeV E crit ( Be). MeV E crit (pp) 3.3 MeV
Sterile neutrino with small splitting De Holanda, Smirnov, JCAP03 0 1 m 1 Berezinsky et al (003) Small sterile admixture : No sensitivity in KamLAND reactor Sensitivity in low energy solar neutrino experiments (Borexino/KamLAND sol)
Non-standard neutrino interactions Small flavor diagonal and flavor changing fermi interactions (~0.1G F ) with quarks Friedland, Lunardini, PG, in prep. LMA with modified matter effects What s new : Lower m 1 region Sensitivity in KamLAND reactor Sensitivity in low energy solar neutrino experiments (Borexino/KamLAND sol)
Summary Why perform low-energy solar neutrino experiments? Low energy Be : 10 % - 5% + Low energy pp (pep) : 5 % - 1% Only neutrinos can enable us to see into the interior of a star. Tests on how the Sun shines. High precision neutrino flux, annually modulated, mixing angle determination Test of vacuum-matter transition. Explore for new physics
Low Energy exps : ES, CC Small CS uncertainty [X] ~ P + f (1-P ) ν e ee ee Better sensibility [X] ~ P CC ee
Data S + K Solar (normalized to BP00) 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 0.0 34 SNO I NC* 1.01 0.13 SNO I ES* 0.4 0.05 * undistorted spectrum assumed 1 SNO II CC 0.3 0.0 1 SNO II NC 1.03 0.09 1 SNO II ES 0.44 0.06 KamLAND 0.61 0.09
CHOOZ + ATM : θ 13 P ( ν ν ) cos 4 θ P ( ν ν ) + 3 ν e e 13 ν e e sin 4 θ 13
LMA : Boron free analysis m 1.1 + 0.6-0.4 ( ) + 11.8-1.6 ( ) + 0.0 + 0.3 tan θ 1 0.45-0.06-0.16 f B 1.0 0.06( 0.18) m 1.1 + 0.4-0.4 ( ) +.6-1.6 ( ) + 0.05 + 0.1 tan θ 1 0.4-0.04-0.14 f B 1.0 0.04( 0.13)