non-standard neutrino interactions and the amir khan in...
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IPP15 @ IPM, Tehran
Non-standard Neutrino Interactions and the
Reactor Neutrino Experiments
Amir Khan
COMSATS IIT and IIU, Islamabad
In Collaboration with:
Douglas McKay & John Ralston
(University of Kansas)
F. Tahir (COMSATS IIT)
September 26, 2015
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Contents
An Introduction to Neutrinos
Electroweak (EW) Model and the Elementary Transitions
Status of the Neutrinos Mass in the EW model
Introducing Nonstandard Interactions
(NSIs)- our model for NSIs.
Applying our model to reactor neutrinos Short Baseline
Experiments
Analyzing Daya Bay and TEXONO experiments for NSIs.
Predictions for the future upgrades of the Daya Bay
and TEXONO experiments.
Recap & Conclusions
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Introduction to Neutrinos
Tiniest and most abundant after photons
Produced in Sun, atmosphere in cosmic ray showers,
Supernovae, Big bang, Accelerators and Reactors…
Energy ranges (μeV - PeV)
Based on their characteristic energy range, detected
by the different techniques like,
The Radiochemical Techniques,
Water Cerenkov Technique,
Scintillation Technique,
Tracking and Hybrid Technique.
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H0γ
W±, Z0
W±, Z0
γ
Electroweak Model & Interactions
f 'f
e
L L L L LL
u s t
d c b e
, , , , , , ,R R R R R R R R Ru d s c t b e
EW Interaction Vertex:
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Weak Interactions of Quarks and Leptons
CC
NC
W c:g cosθ (V- A)
III III
e
e
W c:g sinθ (V- A)
Quark Mixings
0Z
l l
l
0Z
l- -μ l l 5
z V A:g γ (c -c γ )
W
usd u
0Z 0Z
l lν νμ 5
z V A:g γ (c -c γ )
W
l
lW:g (V- A)
W
l
W
Lepton Mixings: NO
Lepton Universality
l
l l l l
,
II
u dq ,
I
u dq,u dq ,u dq
I II III
u c t
d s b
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Weak Interactions of Quarks and Leptons
CC
NC
W c:g cosθ (V- A) W c:g sinθ (V- A)
Quark Mixings
0Z
l l
l
0Z
l- -μ l l 5
z V A:g γ (c -c γ )
W
usd u
0Z 0Z
l lν νμ 5
z V A:g γ (c -c γ )
W
l
lW:g (V- A)
W
l
W
Lepton Mixings: NO
Lepton Universality
l
l l l l
2
,u dq 1
,u dq,u dq ,u dq
III III
e
e
I II III
u c t
d s b
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Weak Interactions of Quarks and Leptons
CC
NC
W c:g cosθ (V- A) W c:g sinθ (V- A)
Quark Mixings
0Z
l l
l
0Z
l- -μ l l 5
z V A:g γ (c -c γ )
W
usd u
0Z 0Z
l lν νμ 5
z V A:g γ (c -c γ )
W
l
lW:g (V- A)
W
l
W
Lepton Mixings: NO
Lepton Universality
l
l l l l
2
,u dq 1
,u dq,u dq ,u dq
III III
e
e
I II III
u c t
d s b
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Lu Ru
X
2
u
u
gm
ug
Ll Rl
X
2
l
l
gm
lg
Ld Rd
X
2
d
d
gm
dg
l L
X
2
l
l
gm
lg
l R
Yukawa Interactions:
Leptons:
Quarks:
Status of Neutrino Masses in the SM
Lf
Rf
0X2
2
f
f
gm
fg
gf ≡ Arbitrary dimensionless constant
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Lu Ru
X
2
u
u
gm
ug
Ll Rl
X
2
l
l
gm
lg
Ld Rd
X
2
d
d
gm
dg
l L
X
2
l
l
gm
lg
l R
Yukawa Interactions:
Leptons
:
Quarks:
Status of Neutrino Masses in the SM
Lf
Rf
0X2
2
f
f
gm
fg
gf ≡ Arbitrary dimensionless constant
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Lf
Rf
0X2
2
f
f
gm
fg
Lu Ru
X
2
u
u
gm
ug
Ll Rl
X
2
l
l
gm
lg
Ld Rd
X
2
d
d
gm
dg
l L
X
2
l
l
gm
lg
l R
Yukawa Interactions:
Leptons:
Quarks:
Status of Neutrino Masses in the SM
gf ≡ Arbitrary dimensionless constant
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The SM Observations & Neutrinos Experiments
In the SM
There is Mixing only in the “Quark Sector” but no
mixing in the “Lepton Sector”
“Lepton Flavor Conservation”
There is “Lepton Universality”
Might have connection with “masslessness” of neutrinos!
On the other hand
There are several experiments for neutrinos of any
type (Solar, Atmospheric, Accelerator, Reactor) which
give evidence that neutrinos are massive!
“Neutrino Oscillations Experiments” (NOEs).
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W
ν aν
W
a aν =U ν
Source Detector
e p e n
e e
How does a NOE Work?
e
l
n pe
l
l l
-
βl
ν
l
U Mass Mixing Matrix
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-
-
-
n pe ν (NSIcase)
n
n pe ν ( case)
pe ν (NSIcase)
e
SM
Search For NSIs in Neutrino Interactions
At Source
ν p e (NSIcase)
ν p e (NSIcase)
ν ν e (
ν p e ( case)
, case)
ν ν e ( , NSIcase)
e
e
e
n
SM
S
n
n
M
At Detector
s λ †αF αβ αβ λ L βa a LL =-2 2G (δ +K )( γ P U ν )(dγ P u) +h.c.l
Model For NSIs in SL
NSIs
GF =
Fermi
Constant
K = Flavor Mixing
Matrix, violating CC,
LFC and LU in SL.
U = Standard Mixing
Matrix PL =Left-hand
helicity Projector
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NU FC
μαF μ R L L ααR αL
α
eP λαF αβ λ L β
α,β
L =L +L
L =-2 2G (eγ (g P +(g +1)P e)(ν γ P ν )
-2 2G ε (eγ Pe)(ν γ P ν )
l l l
l
2 eR 2 eL
W αα W αααR αL
1where, g =sin θ +ε and g =sin θ +ε
2
GF =
Fermi
constant
ε = Flavor Mixing
Matrix violating LFC
and LU in Lepton Sec.
P=PL ,PR
α,β=e, μ, τ
Search For NP in Neutrino Interactions
Model For NSIs in Pure Leptonic Processes
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I: Daya Bay Case
Experiment:
2 2
31θ Δmee 2
13L P 1- sin sin (1.267 )
E
2
13sin (2 ) 0.089 0.01(stat.) 0.005(syst.)
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A Little Digression:
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2 2ee 31 21 31 21 31
2 4 3 3 2
21 13 13 12 12 23 - 13 13 12 23 +
2 2 2
21 12
2
ij 2 2 2
ij ij i
31
3 13 1
32 3221
21
j
3
1
2
Δm Lx = and Δm =m -m
1P =1-[( +cos(2x ) )sin x +( + )sin x sin(2x )sin(2 x )]
2
=sin
P
(2θ )c +4c sin(2θ )cos(2θ )c K -4c s sin (2θ )c K
=sin
P
P (2θ )c -
P
P
P
4s
E
P
4
c 2
3 12 23 - 12 13 13 23 +
2 2 2 2
13 12 13 13 12 23 - 12 13 13 23 +
23 + eμ eμ 23 eτ eτ 23
23 eμ eμ 23 eτ eτ 23
32
sin(2θ )c K +4c cos(2θ )sin(2θ )c K
=sin (2θ )s +4s c sin(2θ )c K +4s cos(2θ )sin(2θ )c K
c K K cos(δ+ )s + K cos(δ+ )c
c K
P
K cos c - K cos s
eμ eμeτ a eτi -ii -2ix -i* * *
ee ea eμ μa eτ τa ea eμ μa eτ τaA =(U + K e U + K e U )e (U + K e U + K e U )
Oscillation Amplitude:
Oscillation Probability:
I. NSIs in Oscillation Experiments:
A handle on MH
A. N. Khan et al, Phys. Rev. D 88, 113006 (2013)
Only Two NSI Parameters!
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I:Constraining sin2(2θ13) and NSI in SBLEs
2
3 3 12 311 ( )sinee PP xP
1-2 km SBLEs (Daya Bay, RENO, D-Chooz)
determine the coefficient of sin2 x31
e.g. Daya Bay sin2(2θ13)=0.089±0.011
2
13 13 13 231 32 3( ) sin (2 ) 4cos(2 )sin(2 )
0.089 0.011
P cP K
In our Model
In SM
2
1
2
33 1sin (21 sin)eeP x
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I: The Event Rate
max
th
Epeeν + - IBD ν E2 E
ν
12 2
2
E
N T ddN(E )= dE P (L, E, K , K )σ (E)G(E-E , σ (a,b)),
dE 4πL dE
awhere σ (a,b)=E +b Detector Energy Resolution
E
Gaussian SmearingInverse β-decay X-SectionReactor Neutrino Flux
Systematic UncertaintyStatistical Uncertainty
L. Zhan et al, Phys. Rev. D79 (2009) 073007
Shao-Feng Ge et al, JHEP 1305 (2013) 131
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The Spectrum Study: NSIs Vs. SMM parameters
K+= K- =-0.04
K+= K-=0
K+=-0.04
K-=+ 0.04
NH
IH
a=0.06, b=0
NH
IH
a=0.06, b=0
K+= K-=0
Sin22θ12 - 1σ
Sin22θ12
Sin22θ12 + 1σ
Central values of all input parameters
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Spectrum Study: Effects of Sin22θ12 Uncertainty
NH
IH
a=0.06, b =0
K+ = K- = +0.04
Sin22θ12 - 1σ
Sin22θ12 +1σ
NH
IH
K+= K- = 0
K+= -0.04
K-= + 0.04
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Statistical Analysis
2
2 ( ) "
NSI SMM
iSMM
i
i
dN dN
dE dEE
dN
dE
pull"
Define a χ2- measure of sensitivity to NSIs
where
Energy range: 1.8 MeV< E < 6 MeV &
Bin width=0.01MeV
Rate labeled “SMM”=“data”
Rate labeled “NSIs”=“model”
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I. Δχ2 -Distributions
K+ = 0, sin22θ12 = 0.881sin22θ12 = 0.857 K+ = K- = 0
a=0.06, b=0 a=0.06, b=0
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I. Dependence on K+ ?
There is no dependence on K+
3Dim. Δχ2 surface above K+- K- plane
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I. Mass Hierarchy in event rates:
Difference between the NH and IH
K+= -0.04, K-= -0.04, P32 is Minimal
K+=0, K-=0
a=0.06, b=0 a=0, b=0
K+= -0.04, K-=+ 0.04, P32 is Maximal
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2
1( )
NH IH
N
MH ii IH
i
dN dN
dE dEE
dN
dE
Model=NH with Ks
Data= IH without Ks
Landscape of the Ratio: χ2NSI / χ2
SMM
I. Statistical Discrimination of MH
a=0.06, b=0Sensitivity to
MH is greater
(P32 maximal)
Sensitivity to
MH is smaller
(P32 minimal)
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II: Scattering SBLEs: The TEXONO Case
The sources are Accelerators & Reactors
Baselines are of the ranges- few meters
(e.g. TEXONO)
The baselines are short enough that the neutrino
oscillation effects can be safely neglected and flux of
each flavor is controlled by the NSI parameters
Designed for the scattering cross section.
Material used CsI(Tl) of total mass 187 kg for
detection.
Average neutrino flux KSNR= 6.4 × 1012 cm-2 s-1 .
Actual neutrino energy range is (0- 8)MeV, but the
range of interest is (3- 8) MeV.
e e
K
e
A.N. Khan et al, Phys. Rev. D 90, 053008 (2014)
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222e F e
SM+NSI
222 2
2
2G mdσ(ν e)[g
dT π
((g 1) ) 1
(g (g 1) [( ) ]]
eR
eeR
e
eL
eeL
e
eR eL ee eeR eL
e
T
E
m T
E
,[( ) ] cos( ),eR eL eR eL eL eR eL R
e e e e e e e where are the NSI phases
II: The Three Differential Cross Sections
222μ F e
SM+NSI
2
22
2
2G mdσ(ν e)= [g
dT π
((g ) 1
(g g [( ) ]]
eR
R
eL
L
eR eL eR L
T
E
m T
E
For scattering replacing μ by τ.e
1
2
3
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22 2e μ τ
ee SM+NSI eμ SM+NSI eτ SM+NSI
dσ(ν e) dσ(ν e) dσ(ν e)F= 1+K [ ] + K [ ] + K [ ]
dT dT dT
II: Total Differential Rate
maxνE
νXe ν ν
νT
d (E )dR=ρ F(E ) dE
dT dE
T(i+1)i XX
T(i)
dRR = Expectedevent rate
dT
Our2 Model
2
2i i
E X
ii stat
R R
where,
i
ER Experimental event rate
Total Differential Cross Section:
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6ν n
nn=0ν ν
d (E ) a=
dE (E )
Kue- Sheng Reactor neutrino spectrum
Fit Parameters Values
a0 -1.2 10^12
a1 3.7 10^13
a2 -4.4 10^14
a3 2.5 10^15
a4 -7.4 10^15
a5 1.1 10^16
a6 -6.7 10^15
II: The Neutrino Spectrum
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II: The Leptonic Case @ 90% C.L.
-0.15<εeRee <0.08
-1.79<εeLee <0.41
-0.18<εeRαe <0.18
-0.76< εeLαe <0.76
-0.19<εeRαe <0.19
-0.84< εeLαe <0.84
-0.14<εeRee <0.08
-1.53<εeLee <0.38
sin2θW =0.251±0.031
sin2θW =0.251±0.031
TEXONO Result
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II: Interplay: SL & Leptonic
NSIs
@ 90% C.L.
-1.35<ImKee<1.35
-0.17<εeRee <0.07
-0.72<ImKee<0.72
-0.18< εeRαe <0.18
-0.72<ImKee<0.72
-0.76<εeLαe <0.76
-0.72<ImKe α <0.72 -0.72<ImKe α <0.72 -0.72<ImKe α <0.72 -0.72<ImKe α <0.72
εeRμ μ , εeR
ττ εeLμ μ εeL
ττ,εeR
αμ,εeRβτ, εeL
αμ,εeLβτ are unbounded
-0.90<ImKee<0.90
-1.4<εeLee <0.34
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II: Future Prospects: Leptonic Case
-0.0023<εeRee <0.0023
-0.04<εeLee <0.04
-0.03<εeRαe <0.03
-0.19< εeLαe <0.19
(α=μ,τ)
@ 90% C.L.
If the statistical uncertainty is improved to “±0.0013”
as reported by the TEXONO Collaboration
(M. Deniz et al, J. Phys. Conf. Ser. 375, 042044 (2012))
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II: Future Prospects: Leptontic Case
If the statistical uncertainty is improved to “±0.0013”
as reported by the TEXONO Collaboration
(M. Deniz et al, J. Phys. Conf. Ser. 375, 042044 (2012))
-0.0023<εeRee <0.0023
-0.04<εeLee <0.04
-0.03<εeRαe <0.03
-0.19< εeLαe <0.19
(α=μ,τ)-0.15<εeR
ee <0.08
-1.79<εeLee <0.41
-0.18<εeRαe <0.18
-0.76< εeLαe <0.76
@ 90% C.L.
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II: Interplay : NU SL & Leptonic NSIs @ 90% C.L.
-0.33<ImKee<0.33
-0.013<εeRee <0.002
-0.14<ImKee<0.14
-0.05<εeLee <0.04
-0.13<ImKee<0.13
-0.03< εeRαe <0.03
-0.13<ImKee<0.13
-0.18<εeLαe <0.18
-0.06<ReKee<0.05
-0.01<εeRee <0.02
-0.01<ReKee<0.01
-0.04<εeLee <0.04
-0.06<ReKee<0.01
-0.09< εeRαe <0.09
-0.02<ReKee<0.01
-0.25< εeLαe <0.25
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II: Interplay : NU SL & Leptonic NSIs @ 90% C.L.
-0.33<ImKee<0.33
-0.013<εeRee <0.002
-0.14<ImKee<0.14
-0.05<εeLee <0.04
-0.13<ImKee<0.13
-0.03< εeRαe <0.03
-0.13<ImKee<0.13
-0.18<εeLαe <0.18
-0.06<ReKee<0.05
-0.01<εeRee <0.02
-0.01<ReKee<0.01
-0.04<εeLee <0.04
-0.06<ReKee<0.01
-0.09< εeRαe <0.09
-0.02<ReKee<0.01
-0.25< εeLαe <0.25
-1.35<ImKee<1.35
-0.17<εeRee <0.07
-0.72<ImKee<0.72
-0.18< εeRαe <0.18
-0.72<ImKee<0.72
-0.76<εeLαe <0.76
-0.90<ImKee<0.90
-1.4<εeLee <0.34
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II: Future Prospects: FC Case
-0.1<K eα <0.1 -0.1<K eα <0.1 -0.1<K eα <0.1 -0.1<K eα <0.1
εeRμ μ , εeR
ττ εeLμ μ εeL
ττ,εeR
αμ,εeRβτ, εeL
αμ,εeLβτ are unbounded
(α=e,τ, β= e, μ)
Ks are real or imaginary
@ 90% C.L.
-0.72<ImKe α <0.72 -0.72<ImKe α <0.72 -0.72<ImKe α <0.72 -0.72<ImKe α <0.72
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Planned high precision reactor, solar neutrino oscillation
experiments and high precision accelerator experiments
can improve the NSI parameter space upto factor 5.
High precision medium baseline reactor experiments may
hint on the phases of NSIs also.
These can also give information on the MH and NP
which confuses each other’s effects.
High precision reactor scattering experiments can
probe deeper into the parameter space for some of NSI
parameters upto several order of magnitude and upto a
factor 5 to 10 and can hint on the phases of NSIs.
Recap & Conclusion
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Thank You All!