neutrino)physics,)where)will)it)go? · summaryof)neutrino)mixing)pdg201814.neutrino mixing 49 table...

Neutrino Physics, Where Will It Go?

Xiao-Gang He

Department of Physics, NTU, 2th April 2019

Neutrino Physics, Where Will It Go?

Xiao-Gang He

Department of Physics, NTU, 2th April 2019

Neutrino Physics, Where Did It Came From?Neutrino Physics, Where Did It Came From?

In 1899, Ernest Rutherford separated radioactive emissions into two types: alpha and beta (now beta minus), based on penetration of objects and ability to cause ionization.

In 1900, Paul Villard identified a still more penetrating type of radiation, which Rutherford identified as a fundamentally new type in 1903 and termed gamma rays.

In 1900, Becquerel measured the mass-to-charge ratio (m/e) for beta particles by the method of J.J. Thomson used to study cathode rays and identify the electron. He found thatm/e for a beta particle is the same as for Thomson's electron, and therefore suggested that the beta particle is in fact an electron.

The surprising energy conservation crisisand the postulation of neutrino

The surprising energy conservation crisisand the postulation of neutrino

Modern History of NeutrinosModern History of Neutrinos

66

Neutrino Physics, Where Is It Now?Three types of active light neutrinosNeutrino Physics, Where Is It Now?Three types of active light neutrinos

higgs Hhiggs H

# of Neutrinos, BBN also -> #=3# of Neutrinos, BBN also -> #=3

Neutrino is every whereNeutrino is every where

Neutrino MixingNeutrino Mixing

B. Pontecorvo (1957). "Mesonium and anti-mesonium". Zh. Eksp. Teor. Fiz. 33: 549–551. B. Pontecorvo (1967). "Neutrino Experiments and the Problem of Conservation of LeptonicCharge". Zh. Eksp. Teor. Fiz. 53: 1717

Z. Maki, M. Nakagawa, and S. Sakata (1962). "Remarks on the Unified Model of ElementaryParticles". Progress of Theoretical Physics 28 (5): 870.

9/28/2015 Bruno Pontecorvo 1950s3 - Bruno Pontecorvo - Wikipedia, the free encyclopedia

https://en.wikipedia.org/wiki/Bruno_Pontecorvo#/media/File:Bruno_Pontecorvo_1950s3.jpg 1/2

S.#Sakata#1911H1970

Z.#Maki#1929H2005#

M.#Nakagawa#1932H2001#

Courtesy#of#Sakata#Memorial#Archival#Library

Mixing and non-zero neutrino massMixing and non-zero neutrino mass

Three generation mixing in quarks and leptonsThree generation mixing in quarks and leptons

Summary of neutrino mixing PDG2018Summary of neutrino mixing PDG201814. Neutrino mixing 49

Table 14.7: The best-fit values and 3σ allowed ranges of the 3-neutrinooscillation parameters, derived from a global fit of the current neutrino oscillationdata (from [174]) . The values (values in brackets) correspond to m1 < m2 < m3(m3 < m1 < m2). The definition of ∆m2 used is: ∆m2 = m2

3 − (m22 +m2

1)/2. Thus,∆m2 = ∆m2

31 − ∆m221/2 > 0, if m1 < m2 < m3, and ∆m2 = ∆m2

32 + ∆m221/2 < 0

for m3 < m1 < m2.

Parameter best-fit (±1σ) 3σ

∆m221 [10−5 eV 2] 7.54+0.26

−0.22 6.99 − 8.18

|∆m2| [10−3 eV 2] 2.43 ± 0.06 (2.38 ± 0.06) 2.23 − 2.61 (2.19 − 2.56)

sin2 θ12 0.308 ± 0.017 0.259 − 0.359

sin2 θ23, ∆m2 > 0 0.437+0.033−0.023 0.374 − 0.628

sin2 θ23, ∆m2 < 0 0.455+0.039−0.031, 0.380 − 0.641

sin2 θ13, ∆m2 > 0 0.0234+0.0020−0.0019 0.0176− 0.0295

sin2 θ13, ∆m2 < 0 0.0240+0.0019−0.0022 0.0178− 0.0298

δ/π (2σ range quoted) 1.39+0.38−0.27 (1.31+0.29

−0.33) (0.00 − 0.16) ⊕ (0.86 − 2.00)

((0.00− 0.02) ⊕ (0.70 − 2.00))

phases in the neutrino mixing matrix is available. Thus, the status of CP symmetry inthe lepton sector is unknown. With θ13 = 0, the Dirac phase δ can generate CP violationeffects in neutrino oscillations [43,55,56]. The magnitude of CP violation in νl → νl′ andνl → νl′ oscillations, l = l′ = e, µ, τ , is determined, as we have seen, by the rephasinginvariant JCP (see Eq. (14.19)), which in the “standard” parametrisation of the neutrinomixing matrix (Eq. (14.78)) has the form:

JCP ≡ Im (Uµ3 U∗e3 Ue2 U∗

µ2) =1

8cos θ13 sin 2θ12 sin 2θ23 sin 2θ13 sin δ . (14.79)

Thus, given the fact that sin 2θ12, sin 2θ23 and sin 2θ13 have been determinedexperimentally with a relatively good precision, the size of CP violation effects inneutrino oscillations depends essentially only on the magnitude of the currently not welldetermined value of the Dirac phase δ. The current data implies |JCP |! 0.040 | sin δ|,where we have used the 3σ ranges of sin2 θ12, sin2 θ23 and sin2 θ13 given in Table 14.7.For the best fit values of sin2 θ12, sin2 θ23 and sin2 θ13 and δ we find in the case of∆m2

31(2) > 0 (∆m231(2) < 0): JCP

∼= − 0.032 (− 0.029). Thus, if the indication that

δ ∼= 3π/2 is confirmed by future more precise data, the CP violation effects in neutrinooscillations would be relatively large.

As we have indicated, the existing data do not allow one to determine the sign of∆m2

A = ∆m231(2). In the case of 3-neutrino mixing, the two possible signs of ∆m2

31(2)correspond to two types of neutrino mass spectrum. In the widely used conventions ofnumbering the neutrinos with definite mass in the two cases, the two spectra read:

August 29, 2014 14:37

CP phase δ = - π/2? θ23 = π/4?CP phase δ = - π/2? θ23 = π/4?

Neutrino MassesNeutrino Massesmνe from β decay : < 2. 05 eV, 2.3 eV (2.0eV)

Troitzk, Mainz (Katrin)Mass hierachies: Not known

Normal m1 <m2 <m3Inverted m3 < m1 <m2 JUNO, DUNE…

Cosmology & Astrophysics: Σi mi <0.17 eV

mνe from β decay : < 2. 05 eV, 2.3 eV (2.0eV)Troitzk, Mainz (Katrin)

Mass hierachies: Not known Normal m1 <m2 <m3Inverted m3 < m1 <m2 JUNO, DUNE…

Cosmology & Astrophysics: Σi mi <0.17 eV

Neutrinoless Double βdecay

KamLAND-Zen

GERDA

CUORE

Is neutrino a Majorana or Dirac particle? Not knownMore efforts: PandaX, CDEX, CUPID, NvDEX…Is neutrino a Majorana or Dirac particle? Not knownMore efforts: PandaX, CDEX, CUPID, NvDEX…

Other types of neutrinos?Other types of neutrinos?

Other neutrino related anomalies:Reactor neutrino flux anomaly: Predicted/Observed = 0.943(0.023). 2σ effect. Gallium radioactive source anomaly:Prediction/Observation = 0.86. 3σ effect

Other neutrino related anomalies:Reactor neutrino flux anomaly: Predicted/Observed = 0.943(0.023). 2σ effect. Gallium radioactive source anomaly:Prediction/Observation = 0.86. 3σ effect

Neutrinos oscillates into sterile neutrinos?Neutrinos oscillates into sterile neutrinos?

Theoretical Models for Neutrinos Theoretical Models for Neutrinos

I. INTRODUCTION

Dirac neutrino mass term

L = LL

Y

HR

+H.C ,! L

m

R

,! m

= vp2Y

m

e

< 0.3 eV, ! Y

e

/Ye

< 105, very much fine tuned!

Assuming neutrinos are Majorana particles,

L = 1

2L

m

C

L

m

= VPMNS

m

V T

PMNS

, .

m

= diag(m1,m2,m3) with mi

= |mi

|exp(i↵i

).

With = /2 and 23 = /4,

m

has the following form

m

=

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A , (1)

Note that in the most general case, because non-zero Majorana

phases, the parameters a, b, c, d, and are all complex.

a = m1c212c

213 +m2s

212c

213 m3s

213 ,

b = 1

2

m1(s

212 + c212s

213) +m2(c

212 + s212s

213)m3c

213

,

c = 1p2(m1 m2)s12c12c13 ,

d =1

2

m1(s

212 c212s

213) +m2(c

212 s212s

213) +m3c

213

,

=1p2s13c13

m1c

212 +m2s

212 +m3

,

= (m1 m2)s12c12s13 .

One has the degrees of freedom to redefine the neutrino fields phases

the most general form of the above mass matrix can be rewritten as

m

=

0

@eip1 0 00 eip2 00 0 eip3

1

A

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A

0

@eip1 0 00 eip2 00 0 eip3

1

A , (2)

where the phases pi

are arbitrary. One can choose some particular values for pi

to obtain formsof m

for convenience of analysis. For example the “-” sign for the “13” and “31” entries can be

2

To have Dirac mass, need to introduce right handed neutrinos νR: (1,1)(0)

Neutrino Physics: Where Will It Go?Solve unsolved problems and have new discoveries. But what are the problems?

Neutrino Physics: Where Will It Go?Solve unsolved problems and have new discoveries. But what are the problems?

If one does not care about the fine tuning problem of neutrino having small Dirac mass. Then problem left are

1. The mixing pattern

2. mass hierarchy: normal or inverted?

Experiments decide and theories try to explain.

If one does not care about the fine tuning problem of neutrino having small Dirac mass. Then problem left are

1. The mixing pattern

2. mass hierarchy: normal or inverted?

Experiments decide and theories try to explain.

Some models trying to explain why neutrino masses are so much smaller than their charged partners

Loop generated neutrino masses:The Zee Model(1980);; Zee-Babu Model (zee 1980;; Babu, 1988)

Other loop models: Babu&He;; E. Ma;; Mohapatra et al;; Geng et al

Seesaw Models:

Type I Introduce singlet neutrinos

Some models trying to explain why neutrino masses are so much smaller than their charged partners

Loop generated neutrino masses:The Zee Model(1980);; Zee-Babu Model (zee 1980;; Babu, 1988)

Other loop models: Babu&He;; E. Ma;; Mohapatra et al;; Geng et al

Seesaw Models:

Type I Introduce singlet neutrinos

9/25/2015 板片_百度百科

http://baike.baidu.com/picture/617058/15547261/0/6648d73dfd3026f99e3d621a.html?fr=lemma&ct=single#aid=0&pic=6648d73dfd3026f99e3d621a 1/1

1/2 跷跷板信息原图

As the general model is expected to be able to fit data, it may be more instructive to analysesome simplified versions than just providing with numbers. We provide more details of Model Aand Model B discussed earlier next to see how additional assumptions restrict the level of modelagreement with data.

B. Model A predictions

Type-III: Introduce triplet lepton representations : (1,3,0) )

(Foot, Lew, He and Joshi, 1989).

L = L

(Y

/p2)

R

+ c

R

MR

The predictions for and 23 are ±/2 and 23 = /4,

Additional information for fixing the sign of CP

. Since should be close to /2, should takec2 > s2.

s13 = (1 2cs)1/2/p3 is not predicted.

Fix cs = 0.497± 0.018 to predict s212 = 0.334± 0.004 for both NH and IH cases.

Note that V 2e2 = (s12c13)2 = 1/3.

The s13 and |Ve2| agree with data within 1.

But s23 outside 1, can be consistent with data at 2 level.

It is remarkable that neutrino mixing matrix in this model with just one free parameter can bein reasonable agreement with data. This may be a hint that it is the form for mixing matrix, atleast as the lowest order approximation, that a underlying theory is producing. One should takethis mass matrix seriously in theoretical model buildings.

If the parameters in the set P are complex,

therefore a new phase appears in the model.

can be used to improve agreement of the model with data.

In both NH and IH cases,

fixing cs and cos to be 0.468 and 0.992, respectively.

s23 and are determined to:

0.534 and 1.426, respectively.

These values are in agreement with data at 1 level.

For the case with c = s, the model is more restrictive. In this case sin = 0. With more precisedata on the CP violating angle , this may rule out this simple case with high confidence level. If = 0, the model is already ruled out at high precision from s13 measurement. However, with anon-zero , the mixing angles can still be made to in agreement at 2 level. In Figure.(??) we shows12, s23, s13 as functions of . When chose cos = 0.93, we can get s12 = 0.58, s23 = 0.78, s13 = 0.15which agree with the experimental data within 2 range.

More precise experimental data are required to distinguish the model with complex model pa-rameters from that with the real parameters and other models, or to rule out the above simplescompletely.

15





L = L

(Y

v/p2)

R

+ c

R

MR

R

/2

M

=

0 Y

v/p2

Y T

v/p2 M

R

. (41)






Note that V 2e2 = (s12c13)2 = 1/3.













15





L = L

(Y

v/p2)

R

+ c

R

MR

R

/2

M

=

0 Y

v/p2

Y T

v/p2 M

R

. (41)






Note that V 2e2 = (s12c13)2 = 1/3.













15

The later models mentioned previously have much more fun to work with for several reasonsThe later models mentioned previously have much more fun to work with for several reasonsNeutrinos are necessarily Marorana particles.Consequences: a. Neutrinoless double β decay. Test!

b. Majorana mass term violate lepton number by 2 units. Through leptogenesis mechanism, translates lepton number violation to baryon number violation, explain why our univrsehas more matter than anti-matter!

Neutrinos are necessarily Marorana particles.Consequences: a. Neutrinoless double β decay. Test!

b. Majorana mass term violate lepton number by 2 units. Through leptogenesis mechanism, translates lepton number violation to baryon number violation, explain why our univrsehas more matter than anti-matter!

Even with small VlN Type-III seesaw can be tested at the LHCTong Li and Xiao-Gang He, arXiv:0907.4193[hep-ph]Even with small VlN Type-III seesaw can be tested at the LHCTong Li and Xiao-Gang He, arXiv:0907.4193[hep-ph]

c. New heavy particle lead to possible signature at collidersc. New heavy particle lead to possible signature at colliders

CMS search limit for Type III seesaw particlesarXiv:1210.1797

CMS search limit for Type III seesaw particlesarXiv:1210.1797

Depending on the considered scenarios, lower limits are obtained on themass of the heavy partner of the neutrino that range from 180 to 210GeV.These are the first limits on the production of type III seesaw fermionictriplet states reported by an experiment at the LHC.

Depending on the considered scenarios, lower limits are obtained on themass of the heavy partner of the neutrino that range from 180 to 210GeV.These are the first limits on the production of type III seesaw fermionictriplet states reported by an experiment at the LHC.

Model has only 11 real parameters plus 7 phases

Babu, Mohapatra (1993)Fukuyama, Okada (2002)Bajc, Melfo, Senjanovic, Vissani (2004)Fukuyama, Ilakovac, Kikuchi, Meljanac, Okada (2004)Aulakh et al (2004)

Bertolini, Frigerio, Malinsky (2004)Babu, Macesanu (2005)Bertolini, Malinsky, Schwetz (2006)Dutta, Mimura, Mohapatra (2007)Bajc, Dorsner, Nemevsek (Jushipura, Patel (2011)2009)

SO(10) Yukawa couplings:

Minimal SO(10) Model without 120

Understand Mixing patternSO(10)Grand Unification

θ13 in Minimal SO(10)

Model Building with θ23=π/4 and δCP = 3π/2(-π/2)

Structure of the mass matrix (charged lepton is already diagonal)

Model Building with θ23=π/4 and δCP = 3π/2(-π/2)

Structure of the mass matrix (charged lepton is already diagonal)I. INTRODUCTION


L = 1

2L

m

C

L

m

= VPMNS

m

V T

PMNS

, .

m


= |mi

|exp(i↵i

).

With = /2 and 23 = /4,

m


m

=

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A , (1)



a = m1c212c

213 +m2s

212c

213 m3s

213 ,

b = 1

2

m1(s

212 + c212s

213) +m2(c

212 + s212s

213)m3c

213

,

c = 1p2(m1 m2)s12c12c13 ,

d =1

2

m1(s

212 c212s

213) +m2(c

212 s212s

213) +m3c

213

,

=1p2s13c13

m1c

212 +m2s

212 +m3

,

= (m1 m2)s12c12s13 .

One has the degrees of freedom to redefine the neutrino fields phases and the most general formof the above mass matrix can be rewritten as

m

=

0

@eip1 0 00 eip2 00 0 eip3

1

A

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A

0

@eip1 0 00 eip2 00 0 eip3

1

A , (2)

where the phases pi


to obtain formsof m

for convenience of analysis. For example the “-” sign for the “13” and “31” entries can beremoved by choosing p1 = p2 = 0 and p3 = , the resultant matrix can be written in a more familiarforms

m

=

0

@a c+ i (c i)

c+ i d+ i b(c i) b d i

1

A , (3)

2

I. INTRODUCTION


L = 1

2L

m

C

L

m

= VPMNS

m

V T

PMNS

, .

m


= |mi

|exp(i↵i

).

With = /2 and 23 = /4,

m


m

=

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A , (1)



a = m1c212c

213 +m2s

212c

213 m3s

213 ,

b = 1

2

m1(s

212 + c212s

213) +m2(c

212 + s212s

213)m3c

213

,

c = 1p2(m1 m2)s12c12c13 ,

d =1

2

m1(s

212 c212s

213) +m2(c

212 s212s

213) +m3c

213

,

=1p2s13c13

m1c

212 +m2s

212 +m3

,

= (m1 m2)s12c12s13 .


m

=

0

@eip1 0 00 eip2 00 0 eip3

1

A

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A

0

@eip1 0 00 eip2 00 0 eip3

1

A , (2)

where the phases pi


to obtain formsof m


m

=

0

@a c+ i (c i)


1

A , (3)

2

I. INTRODUCTION


L = 1

2L

m

C

L

m

= VPMNS

m

V T

PMNS

, .

m


= |mi

|exp(i↵i

).

With = /2 and 23 = /4,

m


m

=

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A , (1)



a = m1c212c

213 +m2s

212c

213 m3s

213 ,

b = 1

2

m1(s

212 + c212s

213) +m2(c

212 + s212s

213)m3c

213

,

c = 1p2(m1 m2)s12c12c13 ,

d =1

2

m1(s

212 c212s

213) +m2(c

212 s212s

213) +m3c

213

,

=1p2s13c13

m1c

212 +m2s

212 +m3

,

= (m1 m2)s12c12s13 .


m

=

0

@eip1 0 00 eip2 00 0 eip3

1

A

0

@a c+ i (c i)

c+ i d+ i b

(c i) b d i

1

A

0

@eip1 0 00 eip2 00 0 eip3

1

A , (2)

where the phases pi


to obtain formsof m


m

=

0

@a c+ i (c i)


1

A , (3)

2

Predictions: |Vi2| =1/√ 3J = Im(V11V*12V*21V22) = (s2-c2)/6√3independent of ρ

Predictions: |Vi2| =1/√ 3J = Im(V11V*12V*21V22) = (s2-c2)/6√3independent of ρ

Diagonalizing the mass matrices, we have

VPMNS

=1p3

0

@c+ sei 1 cei sc+ !sei !2 !cei sc+ !2sei ! !2cei s

1

A , (30)

tan = Im(yw1 + yw3)/Re(yw

1 + yw3),

s = sin and c = cos ,

tan 2 =2|yw

1 + w3y|

|w1|2 |w3|2. (31)

Majorana phases ↵i

of mi

↵1,3 = Arg(wi

(1± cos 2) + w2ei2(1 cos 2)± 2 sin 2yei , ↵2 = Arg(w2) . (32)

Translate into standard parameterization

s12 =1p

2(1 + cs cos )1/2, s23 =

(1 + cs cos +p3cs sin )1/2

p2(1 + cs cos )

12

,

s13 =(1 2cs cos )1/2p

3. (33)

and

sin = (1 +4c2s2 sin2

(c2 s2)2)1/2(1 3c2s2 sin2

(1 + cs cos )2)1/2

1 , if c2 > s2 ,+1 , if s2 > c2 .

(34)

It is clearly that if sin is not zero,

|| and 23 deviate from /2 and /4, respectively.

In the limit goes to zero, that real parameter set P

= ±/2 and 23 = /4.

There are two interesting features for this model worth mentioning. One of is that |Ve2| to be

1/p3 which agree with date. s12 is always larger or equal to 1/

p3 which is a decisive test for this

model. Another is that although the Dirac phase depends on the phase , the Jarlskog parameterJ which is independent of given by J = (c2 s2)/6

p3. This implies that CP violation related

to neutrino oscillation is still purely due to intrinsic CP violation. This model can be made inagreement with data at 1 level.

If = 0 and c = s = 1/p2, the mixing pattern is the tribi-maximal. However, if is not zero,

even if c = s = 1/p2, s13 can be non-zero,s12 and s23 are also modified from their tribi-maximal

values

s12 =1

(2 + cos )1/2, s23 =

1p2(1 +

p3 sin

2 + cos )1/2 , s13 =

(1 cos )1/2p3

. (35)

J is exactly zero which implies sin = 0.

12

Diagonalizing the mass matrices, we have

VPMNS

=1p3

0

@c+ sei 1 cei sc+ !sei !2 !cei sc+ !2sei ! !2cei s

1

A , (30)

tan = Im(yw1 + yw3)/Re(yw

1 + yw3),

s = sin and c = cos ,

tan 2 =2|yw

1 + w3y|

|w1|2 |w3|2. (31)

Majorana phases ↵i

of mi

↵1,3 = Arg(wi

(1± cos 2) + w2ei2(1 cos 2)± 2 sin 2yei , ↵2 = Arg(w2) . (32)

Translate into standard parameterization

s12 =1p

2(1 + cs cos )1/2, s23 =

(1 + cs cos +p3cs sin )1/2

p2(1 + cs cos )

12

,

s13 =(1 2cs cos )1/2p

3. (33)

and

sin = (1 +4c2s2 sin2

(c2 s2)2)1/2(1 3c2s2 sin2

(1 + cs cos )2)1/2

1 , if c2 > s2 ,+1 , if s2 > c2 .

(34)

It is clearly that if sin is not zero,

|| and 23 deviate from /2 and /4, respectively.

In the limit goes to zero, that real parameter set P

= ±/2 and 23 = /4.

There are two interesting features for this model worth mentioning. One of is that |Ve2| to be

1/p3 which agree with date. s12 is always larger or equal to 1/

p3 which is a decisive test for this

model. Another is that although the Dirac phase depends on the phase , the Jarlskog parameterJ which is independent of given by J = (c2 s2)/6

p3. This implies that CP violation related

to neutrino oscillation is still purely due to intrinsic CP violation. This model can be made inagreement with data at 1 level.

If = 0 and c = s = 1/p2, the mixing pattern is the tribi-maximal. However, if is not zero,

even if c = s = 1/p2, s13 can be non-zero,s12 and s23 are also modified from their tribi-maximal

values

s12 =1

(2 + cos )1/2, s23 =

1p2(1 +

p3 sin

2 + cos )1/2 , s13 =

(1 cos )1/2p3

. (35)

J is exactly zero which implies sin = 0.

12

Model Buildings

X-G He, Chin. J Phys. 53, 100101(2015);; Phys. Lett. B750(2015)620.

Model Buildings

X-G He, Chin. J Phys. 53, 100101(2015);; Phys. Lett. B750(2015)620.

New model building guidelineNew model building guideline

First order: θ23 =π/4 and δCP=3π /2, A non-zero θ13.

A4 family symmetry model provide an example to fully realize such mixing pattern. This class of A4models also provide direction for modifying the pattern, with complex Yukawa coefficients.

New experimental data will provide more clue about what the mixing pattern is and how theoretical model should be constructed.

First order: θ23 =π/4 and δCP=3π /2, A non-zero θ13.

A4 family symmetry model provide an example to fully realize such mixing pattern. This class of A4models also provide direction for modifying the pattern, with complex Yukawa coefficients.

New experimental data will provide more clue about what the mixing pattern is and how theoretical model should be constructed.

Oscillation neutrino mass vs. Cosmological bound

> 0.059 eV

> 0.099 eV

Cosmology: Σi mi < 0.17 eV

Run into conflict? Cosmology is so precise?

Oscillation neutrino mass vs. Cosmological bound

> 0.059 eV

> 0.099 eV

Cosmology: Σi mi < 0.17 eV

Run into conflict? Cosmology is so precise?

Sterile neutrinos?Sterile neutrinos?

MiniBoone data may not imply sterile neutrino. But what is it? More data.MiniBoone data may not imply sterile neutrino. But what is it? More data.

Dark Matter detection connectionDark Matter detection connection

Coherent neutrino scattering detected.Coherent neutrino scattering detected.

New from AstrophyscisNew from Astrophyscis

Detection of Cosmic background neutrino?Detection of Cosmic background neutrino?

Conclusion

New surprises in neutrino physics?!

Conclusion

New surprises in neutrino physics?!

neutrino)physics,)where)will)it)go? · summaryof)neutrino)mixing)pdg201814.neutrino mixing 49 table...

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