1. October 14th, 2006LONU-LENS, Virginia Tech Solar Luminosity by Neutrinos Solar Luminosity by Neutrinos Carlos Pena Garay IFIC, Valencia ~

2. SK, SNO ClGa Solar Neutrinos : 40 years of theor. efforts

3. Solar Neutrinos : 40 years of exp. efforts

4. SM + mass, Solar + KamLAND exps.

5. SSM + LMA is the new standard

6. If nuclear fusion reactions among light elements are responsible for solar energy generation and Spiro, Vignaud, PLB (1990) determined from nuclear masses and neutrino energies independent of details of solar model at 1:10 4 Bahcall, PRC (2002) Luminosity constraint D and 3 He are in local kinetic equilibrium

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8. pp chain pp chain 99,77% p + p  d+ e + + e 0,23% p + e - + p  d + e 3 He+ 3 He  +2p 3 He+p  +e + + e ~2  10 -5 %84,7% 13,8% 0,02%13,78% 3 He + 4 He  7 Be +  7 Be + e -  7 Li + e 7 Be + p  8 B +  d + p  3 He +  7 Li + p ->  +  pp I pp III pp II hep hep 8 B  8 Be*+ e + + e 2 

9. 99,77% p + p  d+ e + + e 0,23% p + e - + p  d + e 3p  3 He+   (pp,pep)=  p -M( 3 He)- (pp,pep) d + p  3 He +  3 He production

10. 3 He+ 3 He  +2p  33 =2M( 3 He)-M  -2M p 3 He + 4 He  7 Be +  7 Be + e -  7 Li + e 7 Li + p ->  +  pp I pp II 3 He+p   ( 7 Be)=M p +M( 3 He)-M  - ( 7 Be) 3 He burning

11. Local kinetic equilibrium

12. Summary Bahcall, PRC (2002) includes corrections: -thermal motion -average ionization states -temperature profile

13. 12 C + p  13 N +  13 N  13 C + e + +  ( 13 N)=M( 12 C)+M p -M( 13 C ) - ( 13 N) CNO cycle 13 C + p  14 N +  14 N + p  15 O +  15 O  15 N + e + + 15 N + p  12 C +   ( 15 O)=M( 13 C)+3M p -M  -M( 12 C ) - ( 15 O)

14. )

15. Infer flux from measured rate : Energy distribution (<1%, 10000 SSMs) Solar density, neutrino production distributions Neutrino parameters (~3%) Neutrino cross sections ( <3%) Neutrino flux determination

16. If nuclear fusion reactions among light elements are responsible for solar energy generation and D and 3 He are in local kinetic equilibrium

17. Low Nu experiments : Total luminosity + 7 Be,pp Solar + KamLAND neutrino data: How well do (will) we know solar neutrino fluxes ? Are nuclear reactions the unique source of power in the Sun ?

18. Conclusions Luminosity constraint becomes a key test to accurately probe energy generation of stars. Test independent (1:10 4 ) of solar model details Presently, large uncertainty Needed 7 Be, pp(pep), CNO experiments Few percent accuracy is within reach

20. New Physics : SM +  mass 3  ranges  Solar + KamLAND Atmospheric + K2K CHOOZ Different pattern for leptons and quarks

21. The Neutrino Matrix : SM +  mass ALL oscillation neutrino data BUT LSND 1  ranges 

22. Where are Solar e ? Could they go into other form of  ? As  and   indistinguishable in solar neutrinos experiments