News From the Missing Solar ν’s

Michael B. Smy
University of California,
IrvineNovember 2003,
Tokyo Metropolitan University

Solar Neutrino Experiments• Radio-Chemical (CC):
Homestake (Chlorine), Gallex (Gallium),
SAGE(Gallium), GNO (Gallium)• Electron Elastic Scattering (CC+NC):
Kamiokande (Water-Cherenkov),Super-Kamiokande (Water-Cherenkov),Borexino (liquid scintillator; in future)• Cherenkov (CC): SNO (Deuterium)• Cherenkov (NC): SNO (Deuterium)
Michael Smy, UC Irvine

Solar Neutrino Generation/Detection

Michael Smy, UC Irvine

Solar ν Spectrum

Michael Smy, UC Irvine

Solar ν Problem

Michael Smy, UC IrvineNeutrino Sources and Oscillations• Atm. Neutrinos:(high energy)

Mixing Matrix:– e- and µ-type– Probe oscill. for∆m2=0.001eV2– Varying L (zenith
angle) and E– Probe matter
effects• Solar Neutrinos:(low energy)

MatterEffects
Michael Smy, UC Irvine– Only e-type– Probe oscill. for∆m2=10-11 eV2– Varying L (season)
and E– Probe matter
effects (solar
zenith angle)

LMA
SMA

LOW
Gallex/GNO & SAGE
CC RateVAC

Michael Smy, UC Irvine

Homestake Rate

LMA

SMA

LOW
Gallex/GNO & SAGE
CC RateVAC

Michael Smy, UC Irvine

Homestake Rate

LMA

SMA

LOW
Gallex/GNO & SAGE
CC RateVAC

Michael Smy, UC Irvine

LMA
SMA

LOW

VAC

Michael Smy, UC Irvine

CC Rates ofGallex/GNO,
SAGE, and
Homestake

LMA Range (8B)

LOW Range (8B)

VAC Range (8B)
Michael Smy, UC Irvine

Super-K Expected Day/Night

Michael Smy, UC Irvine

Super-K Collaboration

Michael Smy, UC Irvine

Super-K Solar Neutrinos
Oscillation Signatures• 1496 Live Days between
May 31st, 1996 and July 15th,• Suppression of 8B flux
2001
• Appearance of other active• High Statistics
flavors (with SNO)
• Measures 8B, limits hep flux
• Spectral Distortion• 8B flux time variations
8B flux•
Dailyvariationsof• Studies energy spectrum• Anomalous yearly• Some sensitivity to other
8B flux
variationsofthan e-type neutrinos
Michael Smy, UC Irvine

Solar ν Candidates above 5 MeVMichael Smy, UC Irvine

Super-K Solar Neutrino Rate
1496 Day Final Sample:
Expect:• 22,400 solar neutrino events• 18-21 MeV: 4.9±2.7 events• 48,200 solar• Expect ~1 hep neutrino (SSM)
neutrinos (from SSM)
• Expect ~2 hep neutrinos• 16,700 e-type solar(oscillation best fit: ~4x SSM)
neutrinos (from SNO)
• 90% C.L. upper limit of hep• About 5,700 µ/τ-type
3
2
flux: 73x10 /cm s (7.9xSSM)
solar neutrinos
Michael Smy, UC Irvine

Time Dependence of SK Rate

Michael Smy, UC Irvine

Allowed Eccentricity Region

68%

95%
99.73%

Michael Smy, UC Irvine

Time Variations:

Bin Center
TimeCorrect
Livetimeaveraged
time

Like Milsztajn(hep-ph/0301252)
we get large
Lomb Power (~10)
at (13.8d)-1

Lomb Power decreases, if
Correct bin-time is used!!
Michael Smy, UC Irvine

5 Day Sample

8.35 day (63.09%CL)@13.75 day (0.00% CL)

No Significant
Periodicity
Michael Smy, UC Irvine

Sensitivity to Modulations
95% Sensitivity
Contour

10day bin
5 day binMichael Smy, UC Irvine

Anti-Neutrinos
from theSun?

Low and High Energy Solar Peak5 – 6.5 MeV

10 – 20 MeV

Search for Solar
Antineutrinos

Michael Smy, UC Irvine

Solar Antineutrino 90% Upper Limit
Before Spallation Subtraction

SSM Spectrum ν’s

Using angular
distribution
After Spallation
Subtraction

B Spectrum ν’s

8Michael Smy, UC Irvine

Monochromatic ν’sSignal and
D/N Asymmetry
Extraction inSuperKamiokande

“Solfit”: Ext. Max. Likelihood
L=e−(∑ B + S )ii# Background
Events in 21 bins
N bin

# Signal
EventsEvent Event
Energy “Time”ni(B ⋅ u (cν ) + m S ⋅ p(cν , Eν ) × z (tν ) )
∏∏
ν
i =1

=1

i

i

i

21 Energy bins

i

MCi
mi =
∑ j MC j
Background Shape
Solar ν Flux
Time-Variation

Solar Signal Shape
Michael Smy, UC Irvine

Time Dependence Factor z(t)Scale " Time"-Dependent rate r1 (t )(expected from ν oscillation) by α ,using livetime distribution l (t ) :

+τ

+τ

1
Rα = ∫ rα (t )l (t )dt with L = ∫ l (t )dt
L −τ
−τ
τ

0

1
1
(
)
(
)
,
Pα =
r
t
l
t
dt
M
rα (t )l (t )dt
=
α
α
L+ ∫0
L− −∫τ

rα (t ) 1 + α × (z1 (t )(1 + a1 ) − 1) L+− = L+ − L − , aα = 1 Aa × 1 L+− = α × a1
1 (L+ + L− )zα (t ) ==2
2
2
1 + α × a1
RαAα =Example:• r1(t)=1+0.1sin(t):l(t)=0.99/π (t<0) with τ=π/2
l(t)=1.01/π (t>0) so→R=1.001, L=1,
L+-=0.02, A1=0.2/π,
a1=0.001• rα=1+0.1αsin(t)Michael Smy, UC Irvine

AveragePα − M α= α × A1 , Rα = R1
1 (Pα + M α )2

Solar ν Candidates above 5 MeV

6/cm2sLMA ν Oscillation: Φν=4.87±0.05+0.17
10-0.16
tan2 θ=0.55
+1.3
2
5
2
∆m =6.3 10 eV
ADN=-1.8±1.6 -1.2 %Michael Smy, UC Irvinetan2 θ=0.55∆m2=6.3 10-5eV2

Michael Smy, UC Irvine

(D-N)/0.5(D+N)

tan2 θ=0.55∆m2=6.3 10-5eV2

Michael Smy, UC Irvine+1.3
ADN=-1.8±1.6 -1.2 %Oscillation-induced Spectral Distortions

Daily Variation of SK Rate

Michael Smy, UC Irvine

Zenith Spec.: Oscillation Solutions

Michael Smy, UC Irvine

Zenith Spec.: Data & Solutions

Michael Smy, UC Irvine

D/N of Oscillation Solutions

Michael Smy, UC Irvine

Amplitude Fit (SK Solutions)
SK Bestfit
Solutions∆m2 [eV2]tan2θ
As. [%]

Large Mixing

Low ∆m2

Angle

(LMA)

(LOW*)

6.3x10-5
0.55-2.1

2.9x10-8
0.72-0.3

Quasi-Vacuum(quasi-VAC)

6.49x10-10
1.0
-0.6

Small Mixing
Angle(SMA*)

3.5x10-7
0.013
+0.03

Rate [SSM*] 1.001±0.010 0.997±0.010 0.996±0.010 0.996±0.010

As. [%]-1.8±1.6 +0.3±1.4 -0.3±0.7 -0.4±0.8

Scaling f. α

0.86±0.77-0.9±5.0

0.6±1.2-14±26

φ8B [106/cm2s]
φhep [103/cm2s]

4.84
33

4.20
27

4.12
0

3.87
20

χ2 (20 dof; pχ2) 17.3 (63.2%) 19.8 (47.3%) 17.1 (64.9%) 25.3(18.8%)∆χ2(2 dof;p∆χ2) 0.3 (88.2%) 2.7 (25.9%) 0.0 (100% ) 8.3 (1.6% )Dependence on Mixing

SSM

Michael Smy, UC IrvineDependence on ∆m2

Kam
LAND

Michael Smy, UC Irvine

SSM
+1.3
ADN=-1.8±1.6 -1.2 %

Kam
LAND
Michael Smy, UC Irvineχ

2 for Oscillation Analysis+τ

Scale " Time"-Dependent rate r1 (t )+τ1Rα = ∫ rα (t )l (t )dt with L = ∫ l (t )dt
L −τ−τ(expected from ν oscillation) by α ,τ0using livetime distribution l (t ) :

1
1
(
)
(
)
,
Pα =
r
t
l
t
dt
M
rα (t )l (t )dt
=
α
α
L+ ∫0
L− −∫τ

∆logLtimevar = logLα =1 − logLα =0

Aα =rα (t ) 1 + α × (z1 (t )(1 + a1 ) − 1) L+− = L+ − L − , aα = 1 Aa × 1 L+− = α × a1
zα (t ) ==1 (L+ + L− )2
22Rα
1 + α × a1
Pα − M α= α × A1 , Rα = R1
1 (Pα + M α )2

Biosc (∆m 2 , tan 2 θ )hepiosc (∆m 2 , tan 2 θ )Data ibi = 8 SSM
,
h
=
,
d
=
i
i
8 SSM
8 SSM
Bi + hepiSSM
Bi + hepiSSM
Bi + hepiSSM
8f i (δ Β , δ S , δ R ) = f i (δ Β ) × f i (δ S ) × f i (δ R ), ρ i =
B

N bin

χ2 = ∑i =1

SR

βbi + ηhifi

ρi
, mi =∑j ρ jtimevar

2
(
)
β −1
+

(d i − ρi )2 + δ B2 + δ S2 + δ R2 − 2∆logL

Michael Smy, UC Irvine

σ i2

σ B2

σ S2

σ R2

σ 2B
8

SSM

3σ
2σ
1σ

1σ 2σ 3σMichael Smy, UC Irvine

Michael Smy, UC Irvine

Combined
Oscillation Fits
with Other Solar
Experiments

LMA
SMA
LOW
CC Rates ofGallex/GNO,
SAGE, and
Homestake

qVAC
VAC

Michael Smy, UC Irvine

LMA
SMA
LOW

qVAC
VAC

Michael Smy, UC Irvine

CC Rates ofGallex/GNO,
SAGE, and
HomestakeGallex/GNO, SAGE,
Homestake & SK

LMA 95% C.L.

SMA
LOW

qVAC
VAC

Michael Smy, UC Irvine

CC Rates ofGallex/GNO,
SAGE, and
Homestake

LMA 95% C.L.

Gallex/GNO, SAGE,
Homestake & SK
SMA

LOW
KamLAND

qVAC
VAC

Michael Smy, UC Irvine

CC Rates ofGallex/GNO,
SAGE, and
Homestake

LMA 95% C.L.

Gallex/GNO, SAGE,
Homestake & SK
SMA

LOW
KamLAND

Ga+Cl+SK+KL

qVAC

CC Rates ofGallex/GNO,
SAGE, and
Homestake

VAC

Michael Smy, UC Irvine

KamLAND Analysis from: hep-ph/0302230v2 (A. Ianni)

KamLAND
Solar
LMA-I
3σ

Michael Smy, UC Irvine

KamLAND Analysis from:
hep-ph/0302230v2 (A. Ianni)

KamLAND
Solar
LMA-I
3σ

Michael Smy, UC Irvine

KamLAND Analysis from:
hep-ph/0302230v2 (A. Ianni)

Fits/Param.

All Solar &KamLAND
0.38
0.38
4.8x10-5 7.2x10-5

tan2θ
∆m2 [eV2]∆χ2/CL[%] 14.7/0.06(LOW)

13.1/0.1(LMA-II)

φ8B/φhep[106/cm2s]

5.45/0.033 5.21/0.030

SK/SNO ADN[%]-2.3/-3.8 -1.6/-2.6

KamLAND
Solar
LMA-I
3σ

Michael Smy, UC Irvine

KamLAND Analysis from:
hep-ph/0302230v2 (A. Ianni)

Solar Data + KamLAND
Global Solution

LMA-I

LMA-II∆m2 [eV2], tan2θ

7.2x10-5, 0.38

1.4x10-4, 0.40

0.0 (100%)13.1 (0.1% )∆χ2 (2 d.o.f; p∆χ2)∆χ2SK-Spec / KamLAND
4.2 ( 1.5σ) / 0.6 ( 0.3σ) 4.9 ( 1.7σ) / 4.2 ( 1.5σ)-1.7±1.6 /-1.6 (+0.0σ)
SK ADN: Fit/expect [%]-2.3±1.4 /-0.3 (+1.5σ)
SK Rate [%]/SNO ADN [%] 45.3 (-0.9σ) /-2.6 (+0.9σ) 45.1 ( -1.0σ)/-0.3 (+1.3σ)
SNO CC / NC [% SSM]
33.4 (+0.9σ)/ 103 (+0.1σ) 35.5 (+2.0σ)/ 88 ( -1.6σ)
Ga Rate / Cl Rate [SNU]
71.8 (+0.8σ)/2.96 (+1.8σ) 72.1 (+0.8σ)/3.10(+2.4σ)
φ8B [106/cm2s]/φhep[103/cm2s]
5.21 (+0.2σ) / 30
4.43 (-0.8σ) / 23
8B Spectrum/SK E-sc/resol.
-0.5σ / -0.7σ / -0.2σ-0.7σ / -1.0σ / -0.2σ

Solar 8B ν Spectral Distortion??
Chlorine CC Rate??
Michael Smy, UC Irvine

Combined
Oscillation Fits
with SNO

LMA

SMA
LOW
SNO pure
D2O Day
and Night
SpectrumqVAC
VAC

Michael Smy, UC Irvine

LMA

SMA
LOW
SNO pure
D2O Day
and Night
SpectrumqVAC
VAC

Michael Smy, UC Irvine

KamLAND

SK/SNO

Michael Smy, UC Irvine

KamLAND
SK+SNO+KL

Michael Smy, UC Irvine

KamLAND Analysis from:
hep-ph/0302230v2 (A. Ianni)

SK Bestfit
Solutions∆m2 [eV2]tan2θ
As. [%]

Large Mixing

Low ∆m2

Angle

(LMA)

(LOW*)

6.3x10-5
0.55-2.1

2.9x10-8
0.72-0.3

Quasi-Vacuum(quasi-VAC)

Small Mixing
Angle(SMA*)

6.49x10-10
1.0
-0.6

3.5x10-7
0.013
+0.03

χ2 (20 dof; pχ2) 17.3 (63.2%) 19.8 (47.3%) 17.1 (64.9%)∆χ2(2 dof;p∆χ2) 0.3 (88.2%) 2.7 (25.9%) 0.0 (100% )∆χ2(Spectrum) 2.7 ( 1.1σ)
2.8 ( 1.2σ) 0.1 (0.05σ)
As.-Fit [%]-1.8 (+0.2σ) +0.3 (+0.4σ) -0.3 (+0.3σ)
φ8B [106/cm2s] 4.84 ( -0.3σ) 4.20 ( -1.0σ) 4.12 (-1.2σ)33
27
0
φhep [103/cm2s]
8B Spectrum
-0.1σ
+0.2σ
+0.0σ
SK E-scale
-0.1σ
+0.3σ
-0.0σ
SK E-resol.
-0.1σ
-0.2σ
+0.0σ

25.3(18.8%)
8.3 (1.6% )
7.4 ( 2.2σ)-0.4 (-0.6σ)
3.87 (-1.5σ)
20
+0.9σ
+1.3σ
-0.2σ

Global Solution

Large Mixing
Angle(LMA)

Low ∆m2(LOW)

Vacuum(VAC)

Small Mixing
Angle (SMA)∆m2 [eV2]
tan2θ

4.8x10-5
0.38

9.1x10-8
0.55

6.65x10-11
3.0

4.4x10-6
0.0021

χ2 (24 dof; pχ2) 22.3 (56.4%)∆χ2(2 dof; p∆χ2) 0.0 (100%)37.0 (4.4%)
14.7 (0.06% )43.2 (0.9%)
50.7 (0.1%)
21.0 (0.003% ) 28.5(0.0001% )∆χ2SK-Spec (p∆χ2)
SK ADN [%]SNO ADN [%]Ga Rate [SNU]
Cl Rate [SNU]
SK Rate [%]SNO CC [%]SNO NC [%]3.3 ( 1.3σ)-3.3 ( -0.9σ)-5.6 ( +0.3σ)
70.6 (+0.4σ)
2.90 (+1.5σ)45.2 ( -1.0σ)
32.9 (+0.7σ)
108 (+0.5σ)

3.4 ( 1.3σ)-2.6 ( -2.0σ)-3.6 (+0.7σ)
61.5 ( -2.3σ)
2.90 (+1.5σ)44.8 ( -1.3σ)
36.1 (+2.3σ)
93 ( -1.1σ)

18.0 ( 3.8σ)-0.9 (+0.3σ)
0.0 (+1.4σ)
70.0 (+0.2σ)
2.99 (+1.9σ)
44.5 ( -1.6σ)
35.0 (+1.7σ)
102 ( -0.2σ)

15.3 ( 3.5σ)-2.2 ( -1.8σ)-2.7 (+0.9σ)
67.0 (-0.7σ)
2.25 ( -1.4σ)43.8 ( -2.1σ)
38.3 (+3.4σ)
96 ( -0.8σ)

φ8B [106/cm2s]
φhep [103/cm2s]
8B Spectrum
SK E-sc/resol.

5.45 (+0.4σ)
33-0.3σ-0.4σ /-0.2σ

4.70 (-0.4σ)
22+0.1σ+0.1σ /-0.3σ

5.14 (+0.1σ)
2+0.9σ+1.1σ /-0.0σ

4.84 (-0.3σ)
10+1.1σ+1.5σ /-0.4σwith Hep

w/o Hep

No Correlated Uncertainties! With Correlated Uncertainties!

Michael Smy, UC Irvine

SNO Salt CC/NC Ratio

Michael Smy, UC Irvine

Amplitude Fit (Global Solutions)GlobalSolution

Large Mixing

Low ∆m2

VacuumAngle

Small Mixing
Angle

(LMA)

(LOW)

(VAC)

(SMA)

∆m2 [eV2]tan2θ
As. [%]

4.8x10-5
0.38-3.3

9.1x10-8
0.55-2.6

6.65x10-11
3.0
-0.9

4.4x10-6
0.0021-2.2

Rate [SSM]

1.027±0.010 1.038±0.010 1.056±0.011

1.040±0.011

As. [%]-1.7±1.6 +0.2±1.4 -1.1±1.0 -0.3±1.1
0.49

Scaling f. α
φ8B [106/cm2s]
φhep [103/cm2s]

0.53±0.51-0.08±0.53

1.4±1.1

0.13± 0.48

5.45
33

4.70
22

5.14
2

4.84
10

43.2(0.9%) 50.7 (0.1%)
χ2 (23 dof; pχ2) 22.3(56.4%) 37.0(4.4%)∆χ2(2 dof;p∆χ2) 0.0(100%) 14.7(0.06%) 21.0(0.003) 28.5(0.0001%)

Impact of SK Solar Data on ν Oscillation
Before Super-Kamiokande:

After Super-Kamiokande:

9 Active Oscillation! (June 2000)• Really Oscillations?
9 Large Angle! (June 2000)• Active or Sterile¾ Not VAC, SMA! (June 2000)
Oscillations?
¾ Not LOW! (December 2001)• SMA, VAC, LMA, LOW? ¾ LMA-I (September 2003)
9 Really Osc.! (with SNO: 2001)
December 2001,
Kashiwa

September 2003,
Seattlehep-ex/0309011

June 2000,
Sudbury
Ga+Cl+SK+SNO Rateand SK Zenith Spectrum

Michael Smy, UC Irvine