Solar Neutrinos: Fluxes

Transcript

1 Solar Neutrinos: Fluxes pp chain Sun shines by : 4 p 4 He + e + + ν e + γ Solar Standard Model Fluxes CNO cycle e + N 13 <E >=0.707MeV He 4 C 1 C 13 p p p p N 15 N 14 He 4 O 15 O 16 e + <E >=0.997MeV O17 p F 17 p e + <E >=0.999MeV

2 Neutrinos in The Sun : MSW Effect

3 Neutrinos in The Sun : MSW Effect Solar neutrinos are ν e produced in the core (R 0.3R ) of the Sun

4 Neutrinos in The Sun : MSW Effect Solar neutrinos are ν e produced in the core (R 0.3R ) of the Sun The solar atter density V CC = G F N e N e N A ev At core: V CC, ev

5 Neutrinos in The Sun : MSW Effect Solar neutrinos are ν e produced in the core (R 0.3R ) of the Sun The solar atter density The energy spectru of solar ν es V CC = G F N e N e N A ev At core: V CC, ev E ν MeV

6 Neutrinos in The Sun : MSW Effect Solar neutrinos are ν e produced in the core (R 0.3R ) of the Sun The solar atter density The energy spectru of solar ν es V CC = G F N e N e N A ev At core: V CC, ev E ν MeV For ν e ν µ(τ), in vacuu ν e = cos θ ν 1 + sinθ ν For 10 9 ev 10 4 ev E ν V CC,0 > cos θ

7 Neutrinos in The Sun : MSW Effect Solar neutrinos are ν e produced in the core (R 0.3R ) of the Sun The solar atter density The energy spectru of solar ν es V CC = G F N e N e N A ev At core: V CC, ev E ν MeV For ν e ν µ(τ), in vacuu ν e = cos θ ν 1 + sinθ ν For 10 9 ev 10 4 ev E ν V CC,0 > cos θ ν can cross resonance condition in its way out of the Sun

8 For θ π 4 : In vacuu ν e = cosθ ν 1 + sinθ ν is ostly ν 1 In Sun core ν e = cosθ,0 ν 1 + sinθ,0 ν is ostly ν

9 For θ π 4 : In vacuu ν e = cosθ ν 1 + sinθ ν is ostly ν 1 In Sun core ν e = cosθ,0 ν 1 + sinθ,0 ν is ostly ν If ( /ev ) sin θ (E/MeV)cos θ Adiabatic transition ν is ostly ν before and after resonance θ draatically at resonance ν e coponent P ee This is the MSW effect µ ν e ν 1 ν µ ν e ν µ ν 1 A R A P ee = 1 [1 + cosθ,0 cos θ]

10 For θ π 4 : In vacuu ν e = cosθ ν 1 + sinθ ν is ostly ν 1 In Sun core ν e = cosθ,0 ν 1 + sinθ,0 ν is ostly ν If ( /ev ) sin θ (E/MeV)cos θ Adiabatic transition ν is ostly ν before and after resonance θ draatically at resonance ν e coponent P ee This is the MSW effect µ ν e ν If ( /ev ) sin θ (E/MeV)cosθ Non-Adiabatic transition ν is ostly ν till the resonance At resonance the state can jup into ν 1 (with probability P LZ ) ν e coponent P ee µ ν e ν 1 ν µ ν e ν µ ν 1 1 ν µ ν e ν µ ν 1 A R A A R A P ee = 1 [1 + cosθ,0 cos θ] P ee = 1 [1 + (1 P LZ)cosθ,0 cos θ]

11 Neutrinos in The Sun : MSW Effect

12 Neutrinos in The Sun : MSW Effect ν does not cross resonance: P ee = 1 1 sin θ > 1

13 Neutrinos in The Sun : MSW Effect ν does not cross resonance: P ee = 1 1 sin θ > 1 ν crosses resonance MSW effect

14 Neutrinos in The Sun : MSW Effect ν does not cross resonance: P ee = 1 1 sin θ > 1 ν crosses resonance MSW effect Adiabatic MSW transition P ee = sin θ < 1

15 Neutrinos in The Sun : MSW Effect ν does not cross resonance: P ee = 1 1 sin θ > 1 Adiabacity breaking Effect of P LZ ν crosses resonance MSW effect Adiabatic MSW transition P ee = sin θ < 1

16 Solar Neutrinos: Data radiocheical Experient Detection Flavour E th (MeV) Data BS05 Hoestake 37 Cl(ν, e ) 37 Ar ν e E ν > ± 0.03 Sage + 71 Ga(ν, e ) 71 Ge ν e E ν > ± 0.03 Gallex+GNO real tie ν e, ν Ka SK ES ν µ/τ x e ν x e σµτ E e > ± σ e 6 SNO CC ν e d ppe ν e T e > ± 0.0 NC ν x d ν x p n ν e, ν µ/τ T γ > ± 0.07 ES ν x e ν x e ν e, ν µ/τ T e > ± 0.05 Borexino ν x e ν x e ν e, ν µ/τ E ν = ± 0.07 All experients easuring ostly ν e observed a deficit Deficit is energy dependent Deficit disappears in NC

17 Solar Neutrinos: Oscillation Solutions RATES ONLY SK and SNO E and t dependence GLOBAL LMA 10-4 LMA [10 ev ] 10-5 SMA LOW VAC SMA, LOW, VAC at > 5σ tan θ Best fit = ev tan θ =

18 Solar ν e ν active [10-5 ev ] KaLAND ν e / ν e [10-5 ev ] tan θ tan θ

19 Solar ν e ν active [10-5 ev ] KaLAND ν e / ν e [10-5 ev ] tan θ tan θ ν e oscillation paraeters copatible with ν e : Sensible to assue CPT: P ee = Pēē 9 [10-5 ev ] = ev tan θ = tan θ

20 Solar+Atospheric+Reactor+LBL 3ν Oscillations U: 3 angles, 1 CP-phase + ( Majorana phases) c 3 s 3 0 s 3 c 3 c 13 0 s 13 e iδ s 13 e iδ 0 c c 1 s s 1 c 1 0 A Two ass schees NORMAL 3 atos 1 INVERTED M solar solar 1 3 ν oscillation analysis 1 = M at ± 3 ± 31

21 Solar+Atospheric+Reactor+LBL 3ν Oscillations U: 3 angles, 1 CP-phase + ( Majorana phases) c 3 s 3 0 s 3 c 3 c 13 0 s 13 e iδ s 13 e iδ 0 c c 1 s s 1 c 1 0 A Two ass schees NORMAL 3 atos 1 INVERTED M solar solar 1 3 ν oscillation analysis 1 = M at ± 3 ± 31 Generic 3ν ixing effects: Effects due to θ 13 Difference between Inverted and Noral Interference of two wavelength oscillations CP violation due to phase δ

22 w/o KaLand Global Analysis: Three Neutrino Oscillations [10-5 ev ] χ tan θ 1 sin θ [10-5 ev ] tan θ 1 31 [10-3 ev ] - χ 10 5 w/o LBL -3 δ CP tan θ Noral sin θ sin θ 13 Inverted sin θ 13 χ [10-3 ev ] sin θ 13 = sin θ 13 = sin θ 13 = δ CP tan θ 3 w/o LBL w/o Chooz sin θ 13

23 The derived ranges for the six paraeters at 1σ (3σ) are: 1 = ( ) 10 5 ev 31 =.37 ± 0.17 (0.46) 10 3 ev θ 1 = 34.5 ± 1.4 ( ) θ 3 = ( ) θ 13 = ( +1.9 ) δ CP [0, 360] U 3σ =

24 The derived ranges for the six paraeters at 1σ (3σ) are: 1 = ( ) 10 5 ev 31 =.37 ± 0.17 (0.46) 10 3 ev θ 1 = 34.5 ± 1.4 ( ) θ 3 = ( ) θ 13 = ( +1.9 ) δ CP [0, 360] U 3σ = with structure U LEP 1 (1 + O(λ)) 1 (1 O(λ)) 1 (1 O(λ) + ǫ) 1 (1 + O(λ) ǫ) 1 1 (1 O(λ) ǫ) 1 (1 + O(λ) ǫ) 1 ǫ λ 0. ǫ 0.

25 The derived ranges for the six paraeters at 1σ (3σ) are: 1 = ( ) 10 5 ev 31 =.37 ± 0.17 (0.46) 10 3 ev θ 1 = 34.5 ± 1.4 ( ) θ 3 = ( ) θ 13 = ( +1.9 ) δ CP [0, 360] U 3σ = with structure U LEP 1 (1 + O(λ)) 1 (1 O(λ)) 1 (1 O(λ) + ǫ) 1 (1 + O(λ) ǫ) 1 1 (1 O(λ) ǫ) 1 (1 + O(λ) ǫ) 1 ǫ λ 0. ǫ 0. very different fro quark s U CKM 1 O(λ) O(λ 3 ) O(λ) 1 O(λ ) λ 0. O(λ 3 ) O(λ ) 1

26 We still ignore: { (1) Open Questions Is θ13 0? How sall? () Is θ 3 = π 4? If not, is it > or <? (3) Is there CP violation in the leptons (is δ 0, π)? (4) What is the ordering of the neutrino states? (5) Are neutrino asses: hierarchical: i j i + j? degenerated: i j i + j? (6) Dirac or Majorana?