icecube neutrino observatoryhalzen/notes/week14-2.pdf · icecube neutrino observatory
TRANSCRIPT
![Page 1: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/1.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Plan of Lectures
I. Standard Neutrino Properties and Mass Terms (Beyond Standard)
II. Effects of ν Mass: Neutrino Oscillations (Vacuum)
III. Neutrino Oscillations in Matter
IV. The Emerging Picture and Some Lessons
![Page 2: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/2.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary I
• In the SM:
– Accidental global symmetry: B × Le × Lµ × Lτ ↔ mν ≡ 0
– neutrinos are left-handed (≡ helicity -1): mν = 0 ⇒ chirality ≡ helicity
– No distinction between Majorana or Dirac Neutrinos
• If mν 6= 0 → Need to extend SM
→ different ways of adding mν to the SM– breaking total lepton number (L = Le + Lµ + Lτ ) → Majorana ν: ν = νC
– conserving total lepton number → Dirac ν: ν 6= νC
• Question: How to search for mν?
Answer: Today
![Page 3: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/3.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary I
• In the SM:
– Accidental global symmetry: B × Le × Lµ × Lτ ↔ mν ≡ 0
– neutrinos are left-handed (≡ helicity -1): mν = 0 ⇒ chirality ≡ helicity
– No distinction between Majorana or Dirac Neutrinos
• If mν 6= 0 → Need to extend SM
→ different ways of adding mν to the SM– breaking total lepton number (L = Le + Lµ + Lτ ) → Majorana ν: ν = νC
– conserving total lepton number → Dirac ν: ν 6= νC
• Question: How to search for mν?
Answer: Today
![Page 4: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/4.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary I
• In the SM:
– Accidental global symmetry: B × Le × Lµ × Lτ ↔ mν ≡ 0
– neutrinos are left-handed (≡ helicity -1): mν = 0 ⇒ chirality ≡ helicity
– No distinction between Majorana or Dirac Neutrinos
• If mν 6= 0 → Need to extend SM
→ different ways of adding mν to the SM– breaking total lepton number (L = Le + Lµ + Lτ ) → Majorana ν: ν = νC
– conserving total lepton number → Dirac ν: ν 6= νC
• Question: How to search for mν?
Answer: Today
![Page 5: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/5.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary I
• In the SM:
– Accidental global symmetry: B × Le × Lµ × Lτ ↔ mν ≡ 0
– neutrinos are left-handed (≡ helicity -1): mν = 0 ⇒ chirality ≡ helicity
– No distinction between Majorana or Dirac Neutrinos
• If mν 6= 0 → Need to extend SM
→ different ways of adding mν to the SM– breaking total lepton number (L = Le + Lµ + Lτ ) → Majorana ν: ν = νC
– conserving total lepton number → Dirac ν: ν 6= νC
• Question: How to search for mν?
Answer: Today
![Page 6: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/6.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Plan of Lecture II
Effects of ν Mass: Neutrino Oscillations (Vacuum)
Lepton Mixing
Direct Probes of Neutrino Mass ScaleWeak decays, ν-less ββ decay, Cosmology
Neutrino Oscillations in Vacuum
Vacuum Neutrino Oscillations Searches and Findings
Alternative Mechanisms for Neutrino Oscillations
![Page 7: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/7.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
• Charged current and mass for 3 charged leptons `i and N neutrinos νj in weak basis
LCC+LM = − g√2
3∑
i=1
`WL,iγ
µνWi W+
µ −3
∑
i,j=1
`WL,iM`ij`
WR,j−
1
2
N∑
i,j=1
νci
W MνijνWj +h.c.
• Changing to mass basis by rotations
`WL,i = V `
Lij`L,j `WR,i = V `
Rij`R,j νWi = V ν
ijνj
V `L
†M`V
`R = diag(me, mµ, mτ ) V νT MνV ν = diag(m2
1, m22, m
23, . . . , m
2N )
V `L,R≡ Unitary 3 × 3 matrices V ν≡ Unitary N × N matrix.
• The charged current in the mass basis
LCC = − g√2`iL γµ U ij
LEP νj W+µ
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
![Page 8: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/8.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
• Charged current and mass for 3 charged leptons `i and N neutrinos νj in weak basis
LCC+LM = − g√2
3∑
i=1
`WL,iγ
µνWi W+
µ −3
∑
i,j=1
`WL,iM`ij`
WR,j−
1
2
N∑
i,j=1
νci
W MνijνWj +h.c.
• Changing to mass basis by rotations
`WL,i = V `
Lij`L,j `WR,i = V `
Rij`R,j νWi = V ν
ijνj
V `L
†M`V
`R = diag(me, mµ, mτ ) V νT MνV ν = diag(m2
1, m22, m
23, . . . , m
2N )
V `L,R≡ Unitary 3 × 3 matrices V ν≡ Unitary N × N matrix.
• The charged current in the mass basis
LCC = − g√2`iL γµ U ij
LEP νj W+µ
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
![Page 9: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/9.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
• Charged current and mass for 3 charged leptons `i and N neutrinos νj in weak basis
LCC+LM = − g√2
3∑
i=1
`WL,iγ
µνWi W+
µ −3
∑
i,j=1
`WL,iM`ij`
WR,j−
1
2
N∑
i,j=1
νci
W MνijνWj +h.c.
• Changing to mass basis by rotations
`WL,i = V `
Lij`L,j `WR,i = V `
Rij`R,j νWi = V ν
ijνj
V `L
†M`V
`R = diag(me, mµ, mτ ) V νT MνV ν = diag(m2
1, m22, m
23, . . . , m
2N )
V `L,R≡ Unitary 3 × 3 matrices V ν≡ Unitary N × N matrix.
• The charged current in the mass basis
LCC = − g√2`iL γµ U ij
LEP νj W+µ
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
![Page 10: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/10.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
• Charged current and mass for 3 charged leptons `i and N neutrinos νj in weak basis
LCC+LM = − g√2
3∑
i=1
`WL,iγ
µνWi W+
µ −3
∑
i,j=1
`WL,iM`ij`
WR,j−
1
2
N∑
i,j=1
νci
W MνijνWj +h.c.
• Changing to mass basis by rotations
`WL,i = V `
Lij`L,j `WR,i = V `
Rij`R,j νWi = V ν
ijνj
V `L
†M`V
`R = diag(me, mµ, mτ ) V νT MνV ν = diag(m2
1, m22, m
23, . . . , m
2N )
V `L,R≡ Unitary 3 × 3 matrices V ν≡ Unitary N × N matrix.
• The charged current in the mass basis
LCC = − g√2`iL γµ U ij
LEP νj W+µ
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
![Page 11: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/11.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
• P `ii phase absorved in li
• P νkk phase absorved in νi (only possible if νi is Dirac)
• ULEPU †LEP=I3×3 but in general U †
LEPULEP 6=IN×N
• For example for 3 Dirac ν’s : 3 Mixing angles + 1 Dirac Phase
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
• For 3 Majorana ν’s : 3 Mixing angles + 1 Dirac Phase + 2 Majorana Phases
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
0
B
B
@
1 0 0
0 eiφ2 0
0 0 eiφ3
1
C
C
A
![Page 12: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/12.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
• P `ii phase absorved in li
• P νkk phase absorved in νi (only possible if νi is Dirac)
• ULEPU †LEP=I3×3 but in general U †
LEPULEP 6=IN×N
• For example for 3 Dirac ν’s : 3 Mixing angles + 1 Dirac Phase
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
• For 3 Majorana ν’s : 3 Mixing angles + 1 Dirac Phase + 2 Majorana Phases
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
0
B
B
@
1 0 0
0 eiφ2 0
0 0 eiφ3
1
C
C
A
![Page 13: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/13.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
• P `ii phase absorved in li
• P νkk phase absorved in νi (only possible if νi is Dirac)
• ULEPU †LEP=I3×3 but in general U †
LEPULEP 6=IN×N
• For example for 3 Dirac ν’s : 3 Mixing angles + 1 Dirac Phase
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
• For 3 Majorana ν’s : 3 Mixing angles + 1 Dirac Phase + 2 Majorana Phases
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
0
B
B
@
1 0 0
0 eiφ2 0
0 0 eiφ3
1
C
C
A
![Page 14: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/14.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
• P `ii phase absorved in li
• P νkk phase absorved in νi (only possible if νi is Dirac)
• ULEPU †LEP=I3×3 but in general U †
LEPULEP 6=IN×N
• For example for 3 Dirac ν’s : 3 Mixing angles + 1 Dirac Phase
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
• For 3 Majorana ν’s : 3 Mixing angles + 1 Dirac Phase + 2 Majorana Phases
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
0
B
B
@
1 0 0
0 eiφ2 0
0 0 eiφ3
1
C
C
A
![Page 15: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/15.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Lepton Mixing
ULEP ≡ 3 × N matrix U ijLEP =
3∑
k=1
P `iiV
`L
†ikV νkjP ν
jj
• P `ii phase absorved in li
• P νkk phase absorved in νi (only possible if νi is Dirac)
• ULEPU †LEP=I3×3 but in general U †
LEPULEP 6=IN×N
• For example for 3 Dirac ν’s : 3 Mixing angles + 1 Dirac Phase
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
• For 3 Majorana ν’s : 3 Mixing angles + 1 Dirac Phase + 2 Majorana Phases
ULEP =
0
B
B
@
1 0 0
0 c23 s23
0 −s23 c23
1
C
C
A
0
B
B
@
c13 0 s13eiδ
0 1 0
−s13e−iδ 0 c13
1
C
C
A
0
B
B
@
c21 s12 0
−s12 c12 0
0 0 1
1
C
C
A
0
B
B
@
1 0 0
0 eiφ2 0
0 0 eiφ3
1
C
C
A
![Page 16: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/16.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass
• Neutrino masses can have kinematic effects
• Also if neutrinos have a mass the charged current interactions of leptons are notdiagonal (same as quarks)
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
j
W+
l_
i
ν
W+
_
i
uj
d
• SM gauge invariance does not imply U(1)Le× U(1)Lµ
× U(1)Lτsymmetry
• Total lepton number U(1)L = U(1)Le+Lµ+Lτcan be or cannot be still a
symmetry depending on whether neutrinos are Dirac or Majorana
![Page 17: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/17.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass• Neutrino masses can have kinematic effects
• Also if neutrinos have a mass the charged current interactions of leptons are notdiagonal (same as quarks)
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
j
W+
l_
i
ν
W+
_
i
uj
d
• SM gauge invariance does not imply U(1)Le× U(1)Lµ
× U(1)Lτsymmetry
• Total lepton number U(1)L = U(1)Le+Lµ+Lτcan be or cannot be still a
symmetry depending on whether neutrinos are Dirac or Majorana
![Page 18: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/18.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass• Neutrino masses can have kinematic effects
• Also if neutrinos have a mass the charged current interactions of leptons are notdiagonal (same as quarks)
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
j
W+
l_
i
ν
W+
_
i
uj
d
• SM gauge invariance does not imply U(1)Le× U(1)Lµ
× U(1)Lτsymmetry
• Total lepton number U(1)L = U(1)Le+Lµ+Lτcan be or cannot be still a
symmetry depending on whether neutrinos are Dirac or Majorana
![Page 19: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/19.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass• Neutrino masses can have kinematic effects
• Also if neutrinos have a mass the charged current interactions of leptons are notdiagonal (same as quarks)
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
j
W+
l_
i
ν
W+
_
i
uj
d
• SM gauge invariance does not imply U(1)Le× U(1)Lµ
× U(1)Lτsymmetry
• Total lepton number U(1)L = U(1)Le+Lµ+Lτcan be or cannot be still a
symmetry depending on whether neutrinos are Dirac or Majorana
![Page 20: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/20.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass• Neutrino masses can have kinematic effects
• Also if neutrinos have a mass the charged current interactions of leptons are notdiagonal (same as quarks)
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
j
W+
l_
i
ν
W+
_
i
uj
d
• SM gauge invariance does not imply U(1)Le× U(1)Lµ
× U(1)Lτsymmetry
• Total lepton number U(1)L = U(1)Le+Lµ+Lτcan be or cannot be still a
symmetry depending on whether neutrinos are Dirac or Majorana
![Page 21: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/21.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
• To fully determine the lepton flavour sector we want to know:
* How many, N , neutral states νi and their masses mi
* Their mixing: # angles =
1 for N = 2
3 for N = 3
6 for N = 4
* Their CP properties:
Dirac: νC 6= ν # phases =
0 for N = 2
1 for N = 3
3 for N = 4
Majorana: νC = ν
UMajαj = UDir
αj × e−iηj
# phases =
1 for N = 2
3 for N = 3
6 for N = 4
![Page 22: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/22.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
• To fully determine the lepton flavour sector we want to know:
* How many, N , neutral states νi and their masses mi
* Their mixing: # angles =
1 for N = 2
3 for N = 3
6 for N = 4
* Their CP properties:
Dirac: νC 6= ν # phases =
0 for N = 2
1 for N = 3
3 for N = 4
Majorana: νC = ν
UMajαj = UDir
αj × e−iηj
# phases =
1 for N = 2
3 for N = 3
6 for N = 4
![Page 23: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/23.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
• To fully determine the lepton flavour sector we want to know:
* How many, N , neutral states νi and their masses mi
* Their mixing: # angles =
1 for N = 2
3 for N = 3
6 for N = 4
* Their CP properties:
Dirac: νC 6= ν # phases =
0 for N = 2
1 for N = 3
3 for N = 4
Majorana: νC = ν
UMajαj = UDir
αj × e−iηj
# phases =
1 for N = 2
3 for N = 3
6 for N = 4
![Page 24: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/24.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
g√2W+
µ
∑
ij
(
U ijLEP `i γµ L νj + U ij
CKM U i γµ L Dj)
+ h.c.
• To fully determine the lepton flavour sector we want to know:
* How many, N , neutral states νi and their masses mi
* Their mixing: # angles =
1 for N = 2
3 for N = 3
6 for N = 4
* Their CP properties:
Dirac: νC 6= ν # phases =
0 for N = 2
1 for N = 3
3 for N = 4
Majorana: νC = ν
UMajαj = UDir
αj × e−iηj
# phases =
1 for N = 2
3 for N = 3
6 for N = 4
![Page 25: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/25.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Tritium β Decay
• Fermi proposed a kinematic search of νe mass from beta spectra in 3H beta decay3H →3 He + e + νe
• For “allowed” nuclear transitions, the electron spectrum is given by phase space alone
K(T ) ≡√
dNdT
1Cp E F (E) ∝
√
(Q − T )√
(Q − T )2 − m2ν
T = Ee − me, Q= maximum kinetic energy, (for 3H beta decay Q = 18.6 KeV)
• mν 6= 0 ⇒ distortion from the straight-line at the end point of the spectrummν = 0 ⇒ Tmax = Q
mν 6= 0 ⇒ Tmax = Q − mν
νm
K (T)
QT
– At present only a bound:meff
νe≡
√
∑
m2j |Uej |2 < 2.2 eV (at 95 % CL)
(Mainz & Troisk experiments)
– Katrin proposed to improve present sensitivity to mβeff ∼ 0.3 eV
![Page 26: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/26.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Tritium β Decay
• Fermi proposed a kinematic search of νe mass from beta spectra in 3H beta decay3H →3 He + e + νe
• For “allowed” nuclear transitions, the electron spectrum is given by phase space alone
K(T ) ≡√
dNdT
1Cp E F (E) ∝
√
(Q − T )√
(Q − T )2 − m2ν
T = Ee − me, Q= maximum kinetic energy, (for 3H beta decay Q = 18.6 KeV)
• mν 6= 0 ⇒ distortion from the straight-line at the end point of the spectrummν = 0 ⇒ Tmax = Q
mν 6= 0 ⇒ Tmax = Q − mν
νm
K (T)
QT
– At present only a bound:meff
νe≡
√
∑
m2j |Uej |2 < 2.2 eV (at 95 % CL)
(Mainz & Troisk experiments)
– Katrin proposed to improve present sensitivity to mβeff ∼ 0.3 eV
![Page 27: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/27.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Tritium β Decay
• Fermi proposed a kinematic search of νe mass from beta spectra in 3H beta decay3H →3 He + e + νe
• For “allowed” nuclear transitions, the electron spectrum is given by phase space alone
K(T ) ≡√
dNdT
1Cp E F (E) ∝
√
(Q − T )√
(Q − T )2 − m2ν
T = Ee − me, Q= maximum kinetic energy, (for 3H beta decay Q = 18.6 KeV)
• mν 6= 0 ⇒ distortion from the straight-line at the end point of the spectrummν = 0 ⇒ Tmax = Q
mν 6= 0 ⇒ Tmax = Q − mν
νm
K (T)
QT
– At present only a bound:meff
νe≡
√
∑
m2j |Uej |2 < 2.2 eV (at 95 % CL)
(Mainz & Troisk experiments)
– Katrin proposed to improve present sensitivity to mβeff ∼ 0.3 eV
![Page 28: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/28.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Tritium β Decay
• Fermi proposed a kinematic search of νe mass from beta spectra in 3H beta decay3H →3 He + e + νe
• For “allowed” nuclear transitions, the electron spectrum is given by phase space alone
K(T ) ≡√
dNdT
1Cp E F (E) ∝
√
(Q − T )√
(Q − T )2 − m2ν
T = Ee − me, Q= maximum kinetic energy, (for 3H beta decay Q = 18.6 KeV)
• mν 6= 0 ⇒ distortion from the straight-line at the end point of the spectrummν = 0 ⇒ Tmax = Q
mν 6= 0 ⇒ Tmax = Q − mν
νm
K (T)
QT
– At present only a bound:meff
νe≡
√
∑
m2j |Uej |2 < 2.2 eV (at 95 % CL)
(Mainz & Troisk experiments)
– Katrin proposed to improve present sensitivity to mβeff ∼ 0.3 eV
![Page 29: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/29.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Tritium β Decay
• Fermi proposed a kinematic search of νe mass from beta spectra in 3H beta decay3H →3 He + e + νe
• For “allowed” nuclear transitions, the electron spectrum is given by phase space alone
K(T ) ≡√
dNdT
1Cp E F (E) ∝
√
(Q − T )√
(Q − T )2 − m2ν
T = Ee − me, Q= maximum kinetic energy, (for 3H beta decay Q = 18.6 KeV)
• mν 6= 0 ⇒ distortion from the straight-line at the end point of the spectrummν = 0 ⇒ Tmax = Q
mν 6= 0 ⇒ Tmax = Q − mν
νm
K (T)
QT
– At present only a bound:meff
νe≡
√
∑
m2j |Uej |2 < 2.2 eV (at 95 % CL)
(Mainz & Troisk experiments)
– Katrin proposed to improve present sensitivity to mβeff ∼ 0.3 eV
![Page 30: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/30.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Other Channels
Muon neutrino mass• From the two body decay at rest
π− → µ− + νµ
• Energy momentum conservation:
mπ =√
p2µ + m2
µ +√
p2µ + m2
ν
m2ν = m2
π + m2µ − 2 + mµ
√
p2 + m2π
• Measurement of pµ plus the preciseknowledge of mπ and mµ ⇒ mν
• The present experimental result bound:
meffνµ
≡√
∑
m2j |Uµj |2 < 190 KeV
Tau neutrino mass• The τ is much heavier mτ = 1.776 GeV⇒ Large phase space ⇒ difficult precisionfor mν
• The best precision is obtained fromhadronic final states
τ → nπ + ντ with n ≥ 3
• Lep I experiments obtain:
meffντ
≡√
∑
m2j |Uτj|2 < 18.2 MeV
⇒ If mixing angles Uej are not negligibleBest kinematic limit on Neutrino Mass Scale comes from Tritium Beta Decay
![Page 31: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/31.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Other Channels
Muon neutrino mass• From the two body decay at rest
π− → µ− + νµ
• Energy momentum conservation:
mπ =√
p2µ + m2
µ +√
p2µ + m2
ν
m2ν = m2
π + m2µ − 2 + mµ
√
p2 + m2π
• Measurement of pµ plus the preciseknowledge of mπ and mµ ⇒ mν
• The present experimental result bound:
meffνµ
≡√
∑
m2j |Uµj |2 < 190 KeV
Tau neutrino mass• The τ is much heavier mτ = 1.776 GeV⇒ Large phase space ⇒ difficult precisionfor mν
• The best precision is obtained fromhadronic final states
τ → nπ + ντ with n ≥ 3
• Lep I experiments obtain:
meffντ
≡√
∑
m2j |Uτj|2 < 18.2 MeV
⇒ If mixing angles Uej are not negligibleBest kinematic limit on Neutrino Mass Scale comes from Tritium Beta Decay
![Page 32: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/32.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Other Channels
Muon neutrino mass• From the two body decay at rest
π− → µ− + νµ
• Energy momentum conservation:
mπ =√
p2µ + m2
µ +√
p2µ + m2
ν
m2ν = m2
π + m2µ − 2 + mµ
√
p2 + m2π
• Measurement of pµ plus the preciseknowledge of mπ and mµ ⇒ mν
• The present experimental result bound:
meffνµ
≡√
∑
m2j |Uµj |2 < 190 KeV
Tau neutrino mass• The τ is much heavier mτ = 1.776 GeV⇒ Large phase space ⇒ difficult precisionfor mν
• The best precision is obtained fromhadronic final states
τ → nπ + ντ with n ≥ 3
• Lep I experiments obtain:
meffντ
≡√
∑
m2j |Uτj|2 < 18.2 MeV
⇒ If mixing angles Uej are not negligibleBest kinematic limit on Neutrino Mass Scale comes from Tritium Beta Decay
![Page 33: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/33.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: Other Channels
Muon neutrino mass• From the two body decay at rest
π− → µ− + νµ
• Energy momentum conservation:
mπ =√
p2µ + m2
µ +√
p2µ + m2
ν
m2ν = m2
π + m2µ − 2 + mµ
√
p2 + m2π
• Measurement of pµ plus the preciseknowledge of mπ and mµ ⇒ mν
• The present experimental result bound:
meffνµ
≡√
∑
m2j |Uµj |2 < 190 KeV
Tau neutrino mass• The τ is much heavier mτ = 1.776 GeV⇒ Large phase space ⇒ difficult precisionfor mν
• The best precision is obtained fromhadronic final states
τ → nπ + ντ with n ≥ 3
• Lep I experiments obtain:
meffντ
≡√
∑
m2j |Uτj|2 < 18.2 MeV
⇒ If mixing angles Uej are not negligibleBest kinematic limit on Neutrino Mass Scale comes from Tritium Beta Decay
![Page 34: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/34.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: ν-less Double-β Decay
(A, Z) → (A, Z + 2) + e− + e−
n
p
W
n
p
W
ν
e−
e−
only for Majorana ν’s
Sensitive to Majorana CP phases
• Amplitude involves the product of two leptonic currents:[
eγµLν][
eγµLν]
– If ν Dirac ⇒ ν annihilates a neutrino and creates an antineutrino⇒ no same state ⇒ Amplitude = 0
– If ν Majorana ⇒ ν = νc annihilates and creates a neutrino=antineutrino⇒ same state ⇒ Amplitude ∝ ν (νc)T
]
6= 0
• Amplitude of ν-less-ββ decay is proportional to |〈mee〉| = |∑
U2ejmj |
– Present bound: |〈mee〉| < 0.35 eV +theor. uncert. < 1.05 eV (90% CL)
– Several proposed experiments to reach |〈mee〉| ∼ 10−2 eV
![Page 35: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/35.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: ν-less Double-β Decay
(A, Z) → (A, Z + 2) + e− + e−
n
p
W
n
p
W
ν
e−
e−
only for Majorana ν’s
Sensitive to Majorana CP phases
• Amplitude involves the product of two leptonic currents:[
eγµLν][
eγµLν]
– If ν Dirac ⇒ ν annihilates a neutrino and creates an antineutrino⇒ no same state ⇒ Amplitude = 0
– If ν Majorana ⇒ ν = νc annihilates and creates a neutrino=antineutrino⇒ same state ⇒ Amplitude ∝ ν (νc)T
]
6= 0
• Amplitude of ν-less-ββ decay is proportional to |〈mee〉| = |∑
U2ejmj |
– Present bound: |〈mee〉| < 0.35 eV +theor. uncert. < 1.05 eV (90% CL)
– Several proposed experiments to reach |〈mee〉| ∼ 10−2 eV
![Page 36: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/36.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: ν-less Double-β Decay
(A, Z) → (A, Z + 2) + e− + e−
n
p
W
n
p
W
ν
e−
e−
only for Majorana ν’s
Sensitive to Majorana CP phases
• Amplitude involves the product of two leptonic currents:[
eγµLν][
eγµLν]
– If ν Dirac ⇒ ν annihilates a neutrino and creates an antineutrino⇒ no same state ⇒ Amplitude = 0
– If ν Majorana ⇒ ν = νc annihilates and creates a neutrino=antineutrino⇒ same state ⇒ Amplitude ∝ ν (νc)T
]
6= 0
• Amplitude of ν-less-ββ decay is proportional to |〈mee〉| = |∑
U2ejmj |
– Present bound: |〈mee〉| < 0.35 eV +theor. uncert. < 1.05 eV (90% CL)
– Several proposed experiments to reach |〈mee〉| ∼ 10−2 eV
![Page 37: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/37.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale: ν-less Double-β Decay
(A, Z) → (A, Z + 2) + e− + e−
n
p
W
n
p
W
ν
e−
e−
only for Majorana ν’s
Sensitive to Majorana CP phases
• Amplitude involves the product of two leptonic currents:[
eγµLν][
eγµLν]
– If ν Dirac ⇒ ν annihilates a neutrino and creates an antineutrino⇒ no same state ⇒ Amplitude = 0
– If ν Majorana ⇒ ν = νc annihilates and creates a neutrino=antineutrino⇒ same state ⇒ Amplitude ∝ ν (νc)T
]
6= 0
• Amplitude of ν-less-ββ decay is proportional to |〈mee〉| = |∑
U2ejmj |
– Present bound: |〈mee〉| < 0.35 eV +theor. uncert. < 1.05 eV (90% CL)
– Several proposed experiments to reach |〈mee〉| ∼ 10−2 eV
![Page 38: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/38.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale in Cosmology∑
mνihas effects on:
Cosmic MicrowaveBackground TemperatureFluctuations
Most recent from WMAP
Large scale structure:– 2◦ Field GalaxyRedshift Survey(2dFGRS)–Sloan DigitalSky Survey (SDSS)
Tegmark et. al astro-ph/0310723
Prob
lem
:13
para
met
erst
obe
dete
rmin
ed!!
⇒ limit on∑
mνidepends on
prior and data used to constraintother 12 parameters
∑
mνi≤ 0.7 − 2.1 eV at 95 % CL
![Page 39: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/39.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale in Cosmology∑
mνihas effects on:
Cosmic MicrowaveBackground TemperatureFluctuations
Most recent from WMAP
Large scale structure:– 2◦ Field GalaxyRedshift Survey(2dFGRS)–Sloan DigitalSky Survey (SDSS)
Tegmark et. al astro-ph/0310723 Prob
lem
:13
para
met
erst
obe
dete
rmin
ed!!
⇒ limit on∑
mνidepends on
prior and data used to constraintother 12 parameters
∑
mνi≤ 0.7 − 2.1 eV at 95 % CL
![Page 40: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/40.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Neutrino Mass Scale in Cosmology∑
mνihas effects on:
Cosmic MicrowaveBackground TemperatureFluctuations
Most recent from WMAP
Large scale structure:– 2◦ Field GalaxyRedshift Survey(2dFGRS)–Sloan DigitalSky Survey (SDSS)
Tegmark et. al astro-ph/0310723 Prob
lem
:13
para
met
erst
obe
dete
rmin
ed!!
⇒ limit on∑
mνidepends on
prior and data used to constraintother 12 parameters
∑
mνi≤ 0.7 − 2.1 eV at 95 % CL
![Page 41: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/41.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 42: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/42.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 43: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/43.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 44: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/44.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 45: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/45.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation
⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 46: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/46.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 47: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/47.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 48: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/48.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )
– Difference between propagation eigenvalues– Propagation distance
![Page 49: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/49.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues
– Propagation distance
![Page 50: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/50.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Effects of ν Mass: Flavour Transitions
• Flavour (≡ Interaction) basis (production and detection): νe, νµ and ντ
• Mass basis (free propagation in space-time): ν1, ν2 and ν3 . . .
• In general interaction eigenstates 6= propagation eigenstates
U(ν1, ν2, ν3, . . .) = (νe, νµ, ντ )
⇒ Flavour is not conserved during propagation⇒ ν can be detected with different (or same) flavour than produced
• The probability Pαβ of producing neutrino with flavour α and detecting withflavour β has to depend on:
– Misalignment between interaction and propagation states (≡ U )– Difference between propagation eigenvalues– Propagation distance
![Page 51: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/51.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• If neutrinos have mass, a weak eigenstate |να〉 produced in lα + N →να + N ′
is a linear combination of the mass eigenstates (|νi〉)
|να〉=n
∑
i=1
Uαi |νi〉
U is the unitary mixing matrix.
• After a distance L (or time t) it evolves
|ν(t)〉=n
∑
i=1
Uαi|νi(t)〉
• it can be detected with flavour β with probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
![Page 52: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/52.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• If neutrinos have mass, a weak eigenstate |να〉 produced in lα + N →να + N ′
is a linear combination of the mass eigenstates (|νi〉)
|να〉=n
∑
i=1
Uαi |νi〉
U is the unitary mixing matrix.
• After a distance L (or time t) it evolves
|ν(t)〉=n
∑
i=1
Uαi|νi(t)〉
• it can be detected with flavour β with probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
![Page 53: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/53.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• If neutrinos have mass, a weak eigenstate |να〉 produced in lα + N →να + N ′
is a linear combination of the mass eigenstates (|νi〉)
|να〉=n
∑
i=1
Uαi |νi〉
U is the unitary mixing matrix.
• After a distance L (or time t) it evolves
|ν(t)〉=n
∑
i=1
Uαi|νi(t)〉
• it can be detected with flavour β with probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
![Page 54: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/54.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• If neutrinos have mass, a weak eigenstate |να〉 produced in lα + N →να + N ′
is a linear combination of the mass eigenstates (|νi〉)
|να〉=n
∑
i=1
Uαi |νi〉
U is the unitary mixing matrix.
• After a distance L (or time t) it evolves
|ν(t)〉=n
∑
i=1
Uαi|νi(t)〉
• it can be detected with flavour β with probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
![Page 55: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/55.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• The probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
• We call Ei the neutrino energy and mi the neutrino mass
• Under the approximations:
(1) |ν〉 is a plane wave ⇒ |νi(t)〉 = e −i Eit|νi(0)〉
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
with ∆ij = (Ei − Ej)t
(2) relativistic ν
Ei =√
p2i + m2
i ' pi +m2
i
2Ei
(3) Assuming pi ' pj = p ' E
∆ij
2= 1.27
m2i − m2
j
eV2
L/E
Km/GeV
![Page 56: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/56.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• The probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
• We call Ei the neutrino energy and mi the neutrino mass
• Under the approximations:
(1) |ν〉 is a plane wave ⇒ |νi(t)〉 = e −i Eit|νi(0)〉
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
with ∆ij = (Ei − Ej)t
(2) relativistic ν
Ei =√
p2i + m2
i ' pi +m2
i
2Ei
(3) Assuming pi ' pj = p ' E
∆ij
2= 1.27
m2i − m2
j
eV2
L/E
Km/GeV
![Page 57: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/57.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• The probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
• We call Ei the neutrino energy and mi the neutrino mass
• Under the approximations:
(1) |ν〉 is a plane wave ⇒ |νi(t)〉 = e −i Eit|νi(0)〉
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
with ∆ij = (Ei − Ej)t
(2) relativistic ν
Ei =√
p2i + m2
i ' pi +m2
i
2Ei
(3) Assuming pi ' pj = p ' E
∆ij
2= 1.27
m2i − m2
j
eV2
L/E
Km/GeV
![Page 58: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/58.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• The probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
• We call Ei the neutrino energy and mi the neutrino mass
• Under the approximations:
(1) |ν〉 is a plane wave ⇒ |νi(t)〉 = e −i Eit|νi(0)〉
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
with ∆ij = (Ei − Ej)t
(2) relativistic ν
Ei =√
p2i + m2
i ' pi +m2
i
2Ei
(3) Assuming pi ' pj = p ' E
∆ij
2= 1.27
m2i − m2
j
eV2
L/E
Km/GeV
![Page 59: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/59.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations
• The probability
Pαβ = |〈νβ(t)|να(0)〉|2 = |n
∑
i=1
UαiU∗βi〈νi(t)|νi(0)〉|2
• We call Ei the neutrino energy and mi the neutrino mass
• Under the approximations:
(1) |ν〉 is a plane wave ⇒ |νi(t)〉 = e −i Eit|νi(0)〉
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
with ∆ij = (Ei − Ej)t
(2) relativistic ν
Ei =√
p2i + m2
i ' pi +m2
i
2Ei
(3) Assuming pi ' pj = p ' E
∆ij
2= 1.27
m2i − m2
j
eV2
L/E
Km/GeV
![Page 60: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/60.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations• The oscillation probability:
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
∆ij
2 =(Ei−Ej)L
2 = 1.27(m2
i−m2
j)
eV2
L/E
Km/GeV
– The first term δαβ − 4n
∑
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
(
∆ij
2
)
equal for ν (U → U∗)
→ conserves CP
– The last piece 2∑
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij) opposite sign for ν
→ violates CP
• Pαβ depends on Theoretical Parameters and on Two Experimental Parameters:• ∆m2
ij = m2i − m2
j The mass differences • E The neutrino energy• Uαj The mixing angles • L Distance ν source to detector
(and Dirac phases)
• No information on mass scale nor Majorana phases
![Page 61: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/61.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations• The oscillation probability:
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
∆ij
2 =(Ei−Ej)L
2 = 1.27(m2
i−m2
j)
eV2
L/E
Km/GeV
– The first term δαβ − 4n
∑
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
(
∆ij
2
)
equal for ν (U → U∗)
→ conserves CP
– The last piece 2∑
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij) opposite sign for ν
→ violates CP
• Pαβ depends on Theoretical Parameters and on Two Experimental Parameters:• ∆m2
ij = m2i − m2
j The mass differences • E The neutrino energy• Uαj The mixing angles • L Distance ν source to detector
(and Dirac phases)
• No information on mass scale nor Majorana phases
![Page 62: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/62.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations• The oscillation probability:
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
∆ij
2 =(Ei−Ej)L
2 = 1.27(m2
i−m2
j)
eV2
L/E
Km/GeV
– The first term δαβ − 4n
∑
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
(
∆ij
2
)
equal for ν (U → U∗)
→ conserves CP
– The last piece 2∑
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij) opposite sign for ν
→ violates CP
• Pαβ depends on Theoretical Parameters and on Two Experimental Parameters:• ∆m2
ij = m2i − m2
j The mass differences • E The neutrino energy• Uαj The mixing angles • L Distance ν source to detector
(and Dirac phases)
• No information on mass scale nor Majorana phases
![Page 63: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/63.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations• The oscillation probability:
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
∆ij
2 =(Ei−Ej)L
2 = 1.27(m2
i−m2
j)
eV2
L/E
Km/GeV
– The first term δαβ − 4n
∑
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
(
∆ij
2
)
equal for ν (U → U∗)
→ conserves CP
– The last piece 2∑
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij) opposite sign for ν
→ violates CP
• Pαβ depends on Theoretical Parameters and on Two Experimental Parameters:• ∆m2
ij = m2i − m2
j The mass differences • E The neutrino energy• Uαj The mixing angles • L Distance ν source to detector
(and Dirac phases)
• No information on mass scale nor Majorana phases
![Page 64: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/64.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Vacuum Oscillations• The oscillation probability:
Pαβ = δαβ − 4
nX
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
„
∆ij
2
«
+ 2X
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij)
∆ij
2 =(Ei−Ej)L
2 = 1.27(m2
i−m2
j)
eV2
L/E
Km/GeV
– The first term δαβ − 4n
∑
j 6=i
Re[U?αiUβiUαjU
?βj ]sin
2
(
∆ij
2
)
equal for ν (U → U∗)
→ conserves CP
– The last piece 2∑
j 6=i
Im[U?αiUβiUαjU
?βj ]sin (∆ij) opposite sign for ν
→ violates CP
• Pαβ depends on Theoretical Parameters and on Two Experimental Parameters:• ∆m2
ij = m2i − m2
j The mass differences • E The neutrino energy• Uαj The mixing angles • L Distance ν source to detector
(and Dirac phases)
• No information on mass scale nor Majorana phases
![Page 65: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/65.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
• For 2-ν: U =
0
@
cos θ sin θ
− sin θ cos θ
1
A
Posc = sin2(2θ) sin2(
∆m2L4E
)
Appear
Pαα = 1 − Posc Disappear
• ∆m2 → −∆m2 and θ → −θ + π2 is only a redefinition ν1 ↔ ν2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π2
• Moreover Posc is symmetric under ∆m2 → −∆m2 or θ → −θ + π2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π4
This only happens for 2ν vacuum oscillations
![Page 66: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/66.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
• For 2-ν: U =
0
@
cos θ sin θ
− sin θ cos θ
1
A
Posc = sin2(2θ) sin2(
∆m2L4E
)
Appear
Pαα = 1 − Posc Disappear
• ∆m2 → −∆m2 and θ → −θ + π2 is only a redefinition ν1 ↔ ν2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π2
• Moreover Posc is symmetric under ∆m2 → −∆m2 or θ → −θ + π2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π4
This only happens for 2ν vacuum oscillations
![Page 67: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/67.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
• For 2-ν: U =
0
@
cos θ sin θ
− sin θ cos θ
1
A
Posc = sin2(2θ) sin2(
∆m2L4E
)
Appear
Pαα = 1 − Posc Disappear
• ∆m2 → −∆m2 and θ → −θ + π2 is only a redefinition ν1 ↔ ν2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π2
• Moreover Posc is symmetric under ∆m2 → −∆m2 or θ → −θ + π2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π4
This only happens for 2ν vacuum oscillations
![Page 68: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/68.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
• For 2-ν: U =
0
@
cos θ sin θ
− sin θ cos θ
1
A
Posc = sin2(2θ) sin2(
∆m2L4E
)
Appear
Pαα = 1 − Posc Disappear
• ∆m2 → −∆m2 and θ → −θ + π2 is only a redefinition ν1 ↔ ν2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π2
• Moreover Posc is symmetric under ∆m2 → −∆m2 or θ → −θ + π2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π4
This only happens for 2ν vacuum oscillations
![Page 69: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/69.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
• For 2-ν: U =
0
@
cos θ sin θ
− sin θ cos θ
1
A
Posc = sin2(2θ) sin2(
∆m2L4E
)
Appear
Pαα = 1 − Posc Disappear
• ∆m2 → −∆m2 and θ → −θ + π2 is only a redefinition ν1 ↔ ν2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π2
• Moreover Posc is symmetric under ∆m2 → −∆m2 or θ → −θ + π2
⇒ We can chose the convention ∆m2 > 0 and 0 ≤ θ ≤ π4
This only happens for 2ν vacuum oscillations
![Page 70: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/70.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
Posc = sin2(2θ) sin2(
∆m2LE
)
Appear
Pαα = 1 − Posc Disappear
• In real experimentsneutrinos are not monochromatic
⇒ 〈Pαβ〉=∫
dEνdΦdEν
σCC(Eν)Pαβ(Eν)
• Maximal sensitivity for ∆m2 ∼ E/L
– ∆m2 � E/L ⇒ No time to oscillate⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 0 → 〈Posc〉 ' 0
– ∆m2 � E/L ⇒ Averaged oscillations⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 12 → 〈Posc〉 ' 1
2sin2(2θ)
![Page 71: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/71.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
Posc = sin2(2θ) sin2(
∆m2LE
)
Appear
Pαα = 1 − Posc Disappear
• In real experimentsneutrinos are not monochromatic
⇒ 〈Pαβ〉=∫
dEνdΦdEν
σCC(Eν)Pαβ(Eν)
• Maximal sensitivity for ∆m2 ∼ E/L
– ∆m2 � E/L ⇒ No time to oscillate⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 0 → 〈Posc〉 ' 0
– ∆m2 � E/L ⇒ Averaged oscillations⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 12 → 〈Posc〉 ' 1
2sin2(2θ)
![Page 72: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/72.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
Posc = sin2(2θ) sin2(
∆m2LE
)
Appear
Pαα = 1 − Posc Disappear
• In real experimentsneutrinos are not monochromatic
⇒ 〈Pαβ〉=∫
dEνdΦdEν
σCC(Eν)Pαβ(Eν)
• Maximal sensitivity for ∆m2 ∼ E/L
– ∆m2 � E/L ⇒ No time to oscillate⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 0 → 〈Posc〉 ' 0
– ∆m2 � E/L ⇒ Averaged oscillations⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 12 → 〈Posc〉 ' 1
2sin2(2θ)
![Page 73: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/73.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
Posc = sin2(2θ) sin2(
∆m2LE
)
Appear
Pαα = 1 − Posc Disappear
• In real experimentsneutrinos are not monochromatic
⇒ 〈Pαβ〉=∫
dEνdΦdEν
σCC(Eν)Pαβ(Eν)
• Maximal sensitivity for ∆m2 ∼ E/L
– ∆m2 � E/L ⇒ No time to oscillate⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 0 → 〈Posc〉 ' 0
– ∆m2 � E/L ⇒ Averaged oscillations⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 12 → 〈Posc〉 ' 1
2sin2(2θ)
![Page 74: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/74.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
2-ν Oscillations
Posc = sin2(2θ) sin2(
∆m2LE
)
Appear
Pαα = 1 − Posc Disappear
• In real experimentsneutrinos are not monochromatic
⇒ 〈Pαβ〉=∫
dEνdΦdEν
σCC(Eν)Pαβ(Eν)
• Maximal sensitivity for ∆m2 ∼ E/L
– ∆m2 � E/L ⇒ No time to oscillate⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 0 → 〈Posc〉 ' 0
– ∆m2 � E/L ⇒ Averaged oscillations⇒ 〈sin2
(
1.27∆m2L/E)
〉 ' 12 → 〈Posc〉 ' 1
2sin2(2θ)
![Page 75: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/75.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
p
Sources of ν’s
Concha Gonzalez-Garcia
The Big Bangρν = 330/cm3
Eν =0.0004 eVSN1987Eν ∼ MeV
The Sunνe
ΦEarthν = 6 × 1010ν/cm2s
Eν ∼ 0.1–20 MeVAtmospheric ν′s
νe, νµ, νe, νµ
Φν ∼ 1ν/cm2sHuman BodyΦν = 340 × 106ν/day
Nuclear Reactors
νe
Eν ∼ few MeV
AcceleratorsEν ' 0.3–30 GeV
Earth’s radioactivityΦν ∼ 6 × 106ν/cm2s
![Page 76: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/76.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
To allow observation of neutrino oscillations:
– Nature has to be good: θ �/ 0
– Need the right set up (≡right 〈L
E〉) for ∆m2
Source E (GeV) L (Km) ∆m2 (eV2)
Solar 10−3 107 10−10
Atmospheric 0.1–102 10–103 10−1–10−4
Reactor 10−3 SBL: 0.1–1 10−2–10−3
LBL: 10–102 10−4–10−5
Accelerator 10 SBL: 0.1 & 0.01
LBL: 102– 103 10−2–10−3
![Page 77: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/77.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
To allow observation of neutrino oscillations:
– Nature has to be good: θ �/ 0
– Need the right set up (≡right 〈L
E〉) for ∆m2
Source E (GeV) L (Km) ∆m2 (eV2)
Solar 10−3 107 10−10
Atmospheric 0.1–102 10–103 10−1–10−4
Reactor 10−3 SBL: 0.1–1 10−2–10−3
LBL: 10–102 10−4–10−5
Accelerator 10 SBL: 0.1 & 0.01
LBL: 102– 103 10−2–10−3
![Page 78: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/78.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
To allow observation of neutrino oscillations:
– Nature has to be good: θ �/ 0
– Need the right set up (≡right 〈L
E〉) for ∆m2
Source E (GeV) L (Km) ∆m2 (eV2)
Solar 10−3 107 10−10
Atmospheric 0.1–102 10–103 10−1–10−4
Reactor 10−3 SBL: 0.1–1 10−2–10−3
LBL: 10–102 10−4–10−5
Accelerator 10 SBL: 0.1 & 0.01
LBL: 102– 103 10−2–10−3
![Page 79: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/79.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
To allow observation of neutrino oscillations:
– Nature has to be good: θ �/ 0
– Need the right set up (≡right 〈L
E〉) for ∆m2
Source E (GeV) L (Km) ∆m2 (eV2)
Solar 10−3 107 10−10
Atmospheric 0.1–102 10–103 10−1–10−4
Reactor 10−3 SBL: 0.1–1 10−2–10−3
LBL: 10–102 10−4–10−5
Accelerator 10 SBL: 0.1 & 0.01
LBL: 102– 103 10−2–10−3
![Page 80: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/80.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
To allow observation of neutrino oscillations:
– Nature has to be good: θ �/ 0
– Need the right set up (≡right 〈L
E〉) for ∆m2
Source E (GeV) L (Km) ∆m2 (eV2)
Solar 10−3 107 10−10
Atmospheric 0.1–102 10–103 10−1–10−4
Reactor 10−3 SBL: 0.1–1 10−2–10−3
LBL: 10–102 10−4–10−5
Accelerator 10 SBL: 0.1 & 0.01
LBL: 102– 103 10−2–10−3
![Page 81: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/81.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
To allow observation of neutrino oscillations:
– Nature has to be good: θ �/ 0
– Need the right set up (≡right 〈L
E〉) for ∆m2
Source E (GeV) L (Km) ∆m2 (eV2)
Solar 10−3 107 10−10
Atmospheric 0.1–102 10–103 10−1–10−4
Reactor 10−3 SBL: 0.1–1 10−2–10−3
LBL: 10–102 10−4–10−5
Accelerator 10 SBL: 0.1 & 0.01
LBL: 102– 103 10−2–10−3
![Page 82: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/82.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 83: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/83.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 84: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/84.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact?
In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 85: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/85.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 86: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/86.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 87: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/87.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 88: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/88.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 89: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/89.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Interactions
• Due to SM Weak Interactions
σνp ∼ 10−38cm2 Eν
GeV
• Let’s consider for example atmospheric ν ′s?
ΦATMν = 1 ν per cm2 per second and 〈Eν〉 = 1 GeV
• How many interact? In a human body:
Nint = Φν × σνp × Nhumanprot × T human
life (M × T ≡ Exposure)
Nhumanprotons = Mhuman
gr× NA = 80kg × NA ∼ 5 × 1028protons
T human = 80years = 2 × 109 sec
9
=
;
Exposurehuman
∼ Ton × year
Nint = (5 × 1028) (2 × 109) × 10−38 ∼ 1 interaction per lifetime
⇒ Need huge detectors with Exposure ∼ KTon × year
![Page 90: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/90.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Experimental Probes
• Generically there are two types of experiments to search for ν oscillations :
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
![Page 91: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/91.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Experimental Probes
• Generically there are two types of experiments to search for ν oscillations :
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
![Page 92: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/92.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Experimental Probes
• Generically there are two types of experiments to search for ν oscillations :
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
![Page 93: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/93.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos
Atmospheric νe,µ are produced by the interaction of cosmic rays (p, He . . . ) with theatmosphere
-
_
+
( )
( )
( ) ( )
Rµ/e=
Nµν
νe
N
πp , He
νµ
µ+_
e
ννµ e
+_
Nπ+_π+
2N
N
νν µ+
+~
eν
![Page 94: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/94.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos: Data
EVENT CLASSIFICATION
UPGOING MUONS
e,µ
µ
µ
ν νµµ
CONTAINED
νe,µ
Eν
µ
µνFullyContained
Partially Contained Thru-going
MuonStopping
Muon0.1 - few GeV few GeV few 10 GeV few 100 GeV
• Total Rates for Contained Events
• Angular Distribution at SKp, He
π , Kµ
e
νeνµ
detector
atmosphere
EARTH
νµ
down-going
up-going
zenithangle
L ≈1.2×104 km
L −~ 10-30 km
L ≈104 km
L ≈500 km
[not to scale]
+−
+− +−
+−
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV e-like
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV µ-like
0
20
40
60
80
100
120
140
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV e-like
0
50
100
150
200
250
300
350
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV µ-like + PC
0
0.5
1
1.5
2
2.5
3
3.5
4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Flu
x(10
-13 cm
-2s-1
sr-1
) Upward Through Going µ
0
0.2
0.4
0.6
0.8
1
1.2
1.4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Upward Stopping µ
νe
inag
reem
entw
ithSM
→ Deficitgrows with L
→ Decreaseswith E
![Page 95: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/95.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos: Data
EVENT CLASSIFICATION
UPGOING MUONS
e,µ
µ
µ
ν νµµ
CONTAINED
νe,µ
Eν
µ
µνFullyContained
Partially Contained Thru-going
MuonStopping
Muon0.1 - few GeV few GeV few 10 GeV few 100 GeV
• Total Rates for Contained Events
• Angular Distribution at SKp, He
π , Kµ
e
νeνµ
detector
atmosphere
EARTH
νµ
down-going
up-going
zenithangle
L ≈1.2×104 km
L −~ 10-30 km
L ≈104 km
L ≈500 km
[not to scale]
+−
+− +−
+−
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV e-like
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV µ-like
0
20
40
60
80
100
120
140
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV e-like
0
50
100
150
200
250
300
350
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV µ-like + PC
0
0.5
1
1.5
2
2.5
3
3.5
4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Flu
x(10
-13 cm
-2s-1
sr-1
) Upward Through Going µ
0
0.2
0.4
0.6
0.8
1
1.2
1.4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Upward Stopping µ
νe
inag
reem
entw
ithSM
→ Deficitgrows with L
→ Decreaseswith E
![Page 96: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/96.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos: Data
EVENT CLASSIFICATION
UPGOING MUONS
e,µ
µ
µ
ν νµµ
CONTAINED
νe,µ
Eν
µ
µνFullyContained
Partially Contained Thru-going
MuonStopping
Muon0.1 - few GeV few GeV few 10 GeV few 100 GeV
• Total Rates for Contained Events
• Angular Distribution at SKp, He
π , Kµ
e
νeνµ
detector
atmosphere
EARTH
νµ
down-going
up-going
zenithangle
L ≈1.2×104 km
L −~ 10-30 km
L ≈104 km
L ≈500 km
[not to scale]
+−
+− +−
+−
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV e-like
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV µ-like
0
20
40
60
80
100
120
140
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV e-like
0
50
100
150
200
250
300
350
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV µ-like + PC
0
0.5
1
1.5
2
2.5
3
3.5
4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Flu
x(10
-13 cm
-2s-1
sr-1
) Upward Through Going µ
0
0.2
0.4
0.6
0.8
1
1.2
1.4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Upward Stopping µ
νe
inag
reem
entw
ithSM
→ Deficitgrows with L
→ Decreaseswith E
![Page 97: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/97.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos: Data
EVENT CLASSIFICATION
UPGOING MUONS
e,µ
µ
µ
ν νµµ
CONTAINED
νe,µ
Eν
µ
µνFullyContained
Partially Contained Thru-going
MuonStopping
Muon0.1 - few GeV few GeV few 10 GeV few 100 GeV
• Total Rates for Contained Events
• Angular Distribution at SKp, He
π , Kµ
e
νeνµ
detector
atmosphere
EARTH
νµ
down-going
up-going
zenithangle
L ≈1.2×104 km
L −~ 10-30 km
L ≈104 km
L ≈500 km
[not to scale]
+−
+− +−
+−
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV e-like
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV µ-like
0
20
40
60
80
100
120
140
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV e-like
0
50
100
150
200
250
300
350
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV µ-like + PC
0
0.5
1
1.5
2
2.5
3
3.5
4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Flu
x(10
-13 cm
-2s-1
sr-1
) Upward Through Going µ
0
0.2
0.4
0.6
0.8
1
1.2
1.4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Upward Stopping µ
νe
inag
reem
entw
ithSM
→ Deficitgrows with L
→ Decreaseswith E
![Page 98: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/98.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos: Data
EVENT CLASSIFICATION
UPGOING MUONS
e,µ
µ
µ
ν νµµ
CONTAINED
νe,µ
Eν
µ
µνFullyContained
Partially Contained Thru-going
MuonStopping
Muon0.1 - few GeV few GeV few 10 GeV few 100 GeV
• Total Rates for Contained Events
• Angular Distribution at SKp, He
π , Kµ
e
νeνµ
detector
atmosphere
EARTH
νµ
down-going
up-going
zenithangle
L ≈1.2×104 km
L −~ 10-30 km
L ≈104 km
L ≈500 km
[not to scale]
+−
+− +−
+−
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV e-like
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV µ-like
0
20
40
60
80
100
120
140
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV e-like
0
50
100
150
200
250
300
350
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV µ-like + PC
0
0.5
1
1.5
2
2.5
3
3.5
4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Flu
x(10
-13 cm
-2s-1
sr-1
) Upward Through Going µ
0
0.2
0.4
0.6
0.8
1
1.2
1.4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Upward Stopping µ
νe
inag
reem
entw
ithSM
→ Deficitgrows with L
→ Decreaseswith E
![Page 99: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/99.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric Neutrinos: Data
EVENT CLASSIFICATION
UPGOING MUONS
e,µ
µ
µ
ν νµµ
CONTAINED
νe,µ
Eν
µ
µνFullyContained
Partially Contained Thru-going
MuonStopping
Muon0.1 - few GeV few GeV few 10 GeV few 100 GeV
• Total Rates for Contained Events
• Angular Distribution at SKp, He
π , Kµ
e
νeνµ
detector
atmosphere
EARTH
νµ
down-going
up-going
zenithangle
L ≈1.2×104 km
L −~ 10-30 km
L ≈104 km
L ≈500 km
[not to scale]
+−
+− +−
+−
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV e-like
050
100150200250300350400450
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Sub-GeV µ-like
0
20
40
60
80
100
120
140
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV e-like
0
50
100
150
200
250
300
350
-1 -0.5 0 0.5 1cosθ
Num
ber
of E
vent
s Multi-GeV µ-like + PC
0
0.5
1
1.5
2
2.5
3
3.5
4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Flu
x(10
-13 cm
-2s-1
sr-1
) Upward Through Going µ
0
0.2
0.4
0.6
0.8
1
1.2
1.4
-1 -0.8 -0.6 -0.4 -0.2 0cosθ
Upward Stopping µ
νe
inag
reem
entw
ithSM
→ Deficitgrows with L
→ Decreaseswith E
![Page 100: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/100.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric ν Oscillations: Parameter Estimate
• From Total Contained Event Rates:
〈Pµµ〉 = 1 − sin2 2θ sin2 ∆m2L
2E∼ 0.5 − 0.7
⇒ sin2 2θ & 0.6
• From Angular Distribution:
SK sub-GeV e-like
No oscillation
N e
vent
s
0
200
400
L~ 13000Km ~ 500Km ~ 15Km
SK sub-GeV µ-like
SK multi-GeV e-like
N e
vent
sUP HORIZ DOWN
0
100
200
-1 -0.5 0 0.5 1
SK multi-GeV µ-like
cosθ-1 -0.5 0 0.5 1
For E ∼ 1 GeV deficit at L ∼ 102– 104 Km
∆m2(eV2)L(km)
2E(GeV)∼ 1
⇒ ∆m2 ∼ 10−4 − 10−2eV2
![Page 101: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/101.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric ν Oscillations: Parameter Estimate
• From Total Contained Event Rates:
〈Pµµ〉 = 1 − sin2 2θ sin2 ∆m2L
2E∼ 0.5 − 0.7
⇒ sin2 2θ & 0.6
• From Angular Distribution:
SK sub-GeV e-like
No oscillation
N e
vent
s
0
200
400
L~ 13000Km ~ 500Km ~ 15Km
SK sub-GeV µ-like
SK multi-GeV e-like
N e
vent
sUP HORIZ DOWN
0
100
200
-1 -0.5 0 0.5 1
SK multi-GeV µ-like
cosθ-1 -0.5 0 0.5 1
For E ∼ 1 GeV deficit at L ∼ 102– 104 Km
∆m2(eV2)L(km)
2E(GeV)∼ 1
⇒ ∆m2 ∼ 10−4 − 10−2eV2
![Page 102: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/102.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Atmospheric ν Oscillation Solution: νµ → ντ
★
0.3 0.5 1 2 3
tan2 θ
0
1
2
3
4
5
∆m2 [1
0-3 e
V2 ]
Best fit:∆m2 = 2.2 × 10−3 eV2
tan2 θ = 1
![Page 103: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/103.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Lab Searches at Short Distance
• In laboratory experiments ν source: Accelerator or Nuclear Reactor
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
Experiment 〈E/MeV
L/m〉 α β
CCFR 100 FNAL νµ, νe ντ
E531 25 FNAL νµ, νe ντ
Nomad 13 CERN νµ, νe ντ
Chorus 13 CERN νµ, νe ντ
E776 2.5 BNL νµ νe
Karmen2 2.5 Rutherford ν̄µ ν̄e
LSND 3 Los Alamos ν̄µ ν̄e
Miniboone 3 Fermilab νµ νe
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Experiment 〈E/MeV
L/m〉 α
CDHSW 1.4 CERN νµ
BugeyIII 0.05 Reactor ν̄e
Chooz 0.005 Reactor ν̄e
![Page 104: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/104.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Lab Searches at Short Distance
• In laboratory experiments ν source: Accelerator or Nuclear Reactor
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
Experiment 〈E/MeV
L/m〉 α β
CCFR 100 FNAL νµ, νe ντ
E531 25 FNAL νµ, νe ντ
Nomad 13 CERN νµ, νe ντ
Chorus 13 CERN νµ, νe ντ
E776 2.5 BNL νµ νe
Karmen2 2.5 Rutherford ν̄µ ν̄e
LSND 3 Los Alamos ν̄µ ν̄e
Miniboone 3 Fermilab νµ νe
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Experiment 〈E/MeV
L/m〉 α
CDHSW 1.4 CERN νµ
BugeyIII 0.05 Reactor ν̄e
Chooz 0.005 Reactor ν̄e
![Page 105: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/105.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Lab Searches at Short Distance
• In laboratory experiments ν source: Accelerator or Nuclear Reactor
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
Experiment 〈E/MeV
L/m〉 α β
CCFR 100 FNAL νµ, νe ντ
E531 25 FNAL νµ, νe ντ
Nomad 13 CERN νµ, νe ντ
Chorus 13 CERN νµ, νe ντ
E776 2.5 BNL νµ νe
Karmen2 2.5 Rutherford ν̄µ ν̄e
LSND 3 Los Alamos ν̄µ ν̄e
Miniboone 3 Fermilab νµ νe
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Experiment 〈E/MeV
L/m〉 α
CDHSW 1.4 CERN νµ
BugeyIII 0.05 Reactor ν̄e
Chooz 0.005 Reactor ν̄e
![Page 106: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/106.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Lab Searches at Short Distance
• In laboratory experiments ν source: Accelerator or Nuclear Reactor
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
Experiment 〈E/MeV
L/m〉 α β
CCFR 100 FNAL νµ, νe ντ
E531 25 FNAL νµ, νe ντ
Nomad 13 CERN νµ, νe ντ
Chorus 13 CERN νµ, νe ντ
E776 2.5 BNL νµ νe
Karmen2 2.5 Rutherford ν̄µ ν̄e
LSND 3 Los Alamos ν̄µ ν̄e
Miniboone 3 Fermilab νµ νe
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Experiment 〈E/MeV
L/m〉 α
CDHSW 1.4 CERN νµ
BugeyIII 0.05 Reactor ν̄e
Chooz 0.005 Reactor ν̄e
![Page 107: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/107.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Lab Searches at Short Distance
• In laboratory experiments ν source: Accelerator or Nuclear Reactor
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
Experiment 〈E/MeV
L/m〉 α β
CCFR 100 FNAL νµ, νe ντ
E531 25 FNAL νµ, νe ντ
Nomad 13 CERN νµ, νe ντ
Chorus 13 CERN νµ, νe ντ
E776 2.5 BNL νµ νe
Karmen2 2.5 Rutherford ν̄µ ν̄e
LSND 3 Los Alamos ν̄µ ν̄e
Miniboone 3 Fermilab νµ νe
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Experiment 〈E/MeV
L/m〉 α
CDHSW 1.4 CERN νµ
BugeyIII 0.05 Reactor ν̄e
Chooz 0.005 Reactor ν̄e
![Page 108: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/108.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ν Oscillations: Lab Searches at Short Distance
• In laboratory experiments ν source: Accelerator or Nuclear Reactor
Appearance Experiment
L
αν sourceν ν detectorSearches for β
β
αdiff
Experiment 〈E/MeV
L/m〉 α β
CCFR 100 FNAL νµ, νe ντ
E531 25 FNAL νµ, νe ντ
Nomad 13 CERN νµ, νe ντ
Chorus 13 CERN νµ, νe ντ
E776 2.5 BNL νµ νe
Karmen2 2.5 Rutherford ν̄µ ν̄e
LSND 3 Los Alamos ν̄µ ν̄e
Miniboone 3 Fermilab νµ νe
Disappearance Experiment
αν sourceν να
detector ναdetectorI II
Φα Ι Φα ΙΙLL
I
II
α Ι α ΙΙandCompares ΦΦ to look for loss
Experiment 〈E/MeV
L/m〉 α
CDHSW 1.4 CERN νµ
BugeyIII 0.05 Reactor ν̄e
Chooz 0.005 Reactor ν̄e
![Page 109: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/109.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
LSND
• The only short distance signal for oscillation: L = 30 m with 〈Eν〉 ∼ 30 MeV• Used the proton beam of Los Alamos p + Target → π+ + X
π+ → νµ µ+
µ+ → e+ νe νµ
• observed νµ → νe with probability 〈Peµ〉= (0.26 ± 0.07 ± 0.05)%
• Karmen which searched for the same signal and did not observe oscillations.• MiniBoone in Fermilab is/has been running to solve this.
![Page 110: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/110.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
LSND
• The only short distance signal for oscillation: L = 30 m with 〈Eν〉 ∼ 30 MeV• Used the proton beam of Los Alamos p + Target → π+ + X
π+ → νµ µ+
µ+ → e+ νe νµ
• observed νµ → νe with probability 〈Peµ〉= (0.26 ± 0.07 ± 0.05)%
• Karmen which searched for the same signal and did not observe oscillations.• MiniBoone in Fermilab is/has been running to solve this.
![Page 111: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/111.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
LSND
• The only short distance signal for oscillation: L = 30 m with 〈Eν〉 ∼ 30 MeV• Used the proton beam of Los Alamos p + Target → π+ + X
π+ → νµ µ+
µ+ → e+ νe νµ
• observed νµ → νe with probability 〈Peµ〉= (0.26 ± 0.07 ± 0.05)%
• Karmen which searched for the same signal and did not observe oscillations.• MiniBoone in Fermilab is/has been running to solve this.
![Page 112: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/112.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
LSND
• The only short distance signal for oscillation: L = 30 m with 〈Eν〉 ∼ 30 MeV• Used the proton beam of Los Alamos p + Target → π+ + X
π+ → νµ µ+
µ+ → e+ νe νµ
• observed νµ → νe with probability 〈Peµ〉= (0.26 ± 0.07 ± 0.05)%
• Karmen which searched for the same signal and did not observe oscillations.
• MiniBoone in Fermilab is/has been running to solve this.
![Page 113: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/113.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
LSND
• The only short distance signal for oscillation: L = 30 m with 〈Eν〉 ∼ 30 MeV• Used the proton beam of Los Alamos p + Target → π+ + X
π+ → νµ µ+
µ+ → e+ νe νµ
• observed νµ → νe with probability 〈Peµ〉= (0.26 ± 0.07 ± 0.05)%
• Karmen which searched for the same signal and did not observe oscillations.• MiniBoone in Fermilab is/has been running to solve this.
![Page 114: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/114.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
MiniBooNE
• Search for νµ → νe with Eν = 0.3 − 2 GeV and L = 540 m
Observed spectrum of νe
even
ts / M
eV
0 .5
1 .0
1 .5
2 .0
2 .5analysis threshold
osc illationν2
y M iniB ooN E data
µνg ex p ec ted b ac k grou nd
µνeν→µν B G + b est-fit
b ac k grou ndµν
b ac k grou ndeν
3 0 0 6 0 0 9 0 0 1 2 0 0 1 5 0 0
excess e
ven
ts / M
eV
0 .0
0 .2
0 .4
0 .6
0 .8
(MeV)νrec o nstr u c ted E
3 0 0 0
data - ex p ec ted b ac k grou nd
eν→µν b est-fit
µν2= 1 .0 eV2m∆)= 0 .0 0 4 ,θ(22 sin
µν2= 0 .1 eV2m∆)= 0 .2,θ(22 sin
Excluded region
ts
sta -
k g ro u n d
d a sh e d
o sc illa -
e rs
fro m
e x -
re p re se n t
o n d
with
re c o n -
n o r-
sim p le r
)θ(22
s in
-310
-210
-110 1
)4
/c2
| (
eV
2m∆|
-210
-110
1
10
210
LSND 90% C.L.
LSND 99% C.L.
) u p p e r limitθ(22s in
yM in iB o o NE 90% C.L.
M in iB o o NE 90% C.L. s e n s itiv ity
B DT a n a lys is 90% C.L.
Based on this analysis LSND Excluded at 90-98% CL by MiniBooNE.
![Page 115: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/115.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary of Searches at Short Baseline
1
10
10 2
10 3
10 -4 10 -3 10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
E531CCFR
NOMAD
CHORUS
CDHS
νµ → ντ90% C.L. 10
10 2
10 3
10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
NOMAD
CHORUS
CHOOZνe → ντ
90% C.L.
• Reactor disappearance experiments⇒ Lower E and longer L⇒ are more sensitive to lower ∆m2
• Accelerator appearance experiments⇒ higher E shorter L more precision⇒ better limits on mixing
• To reach small ∆m2 & 10−4 eV2
⇒ very large L and intermediate E⇒ Long Baseline Exp at Accelerators
• To reach smaller ∆m2 & 10−5 eV2
⇒ Long Baseline Exp at Reactors
![Page 116: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/116.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary of Searches at Short Baseline
1
10
10 2
10 3
10 -4 10 -3 10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
E531CCFR
NOMAD
CHORUS
CDHS
νµ → ντ90% C.L. 10
10 2
10 3
10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
NOMAD
CHORUS
CHOOZνe → ντ
90% C.L.
• Reactor disappearance experiments⇒ Lower E and longer L⇒ are more sensitive to lower ∆m2
• Accelerator appearance experiments⇒ higher E shorter L more precision⇒ better limits on mixing
• To reach small ∆m2 & 10−4 eV2
⇒ very large L and intermediate E⇒ Long Baseline Exp at Accelerators
• To reach smaller ∆m2 & 10−5 eV2
⇒ Long Baseline Exp at Reactors
![Page 117: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/117.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary of Searches at Short Baseline
1
10
10 2
10 3
10 -4 10 -3 10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
E531CCFR
NOMAD
CHORUS
CDHS
νµ → ντ90% C.L. 10
10 2
10 3
10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
NOMAD
CHORUS
CHOOZνe → ντ
90% C.L.
• Reactor disappearance experiments⇒ Lower E and longer L⇒ are more sensitive to lower ∆m2
• Accelerator appearance experiments⇒ higher E shorter L more precision⇒ better limits on mixing
• To reach small ∆m2 & 10−4 eV2
⇒ very large L and intermediate E⇒ Long Baseline Exp at Accelerators
• To reach smaller ∆m2 & 10−5 eV2
⇒ Long Baseline Exp at Reactors
![Page 118: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/118.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary of Searches at Short Baseline
1
10
10 2
10 3
10 -4 10 -3 10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
E531CCFR
NOMAD
CHORUS
CDHS
νµ → ντ90% C.L. 10
10 2
10 3
10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
NOMAD
CHORUS
CHOOZνe → ντ
90% C.L.
• Reactor disappearance experiments⇒ Lower E and longer L⇒ are more sensitive to lower ∆m2
• Accelerator appearance experiments⇒ higher E shorter L more precision⇒ better limits on mixing
• To reach small ∆m2 & 10−4 eV2
⇒ very large L and intermediate E⇒ Long Baseline Exp at Accelerators
• To reach smaller ∆m2 & 10−5 eV2
⇒ Long Baseline Exp at Reactors
![Page 119: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/119.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary of Searches at Short Baseline
1
10
10 2
10 3
10 -4 10 -3 10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
E531CCFR
NOMAD
CHORUS
CDHS
νµ → ντ90% C.L. 10
10 2
10 3
10 -2 10 -1 1sin2 2θ
∆m2 (e
V2 /c
4 )
NOMAD
CHORUS
CHOOZνe → ντ
90% C.L.
• Reactor disappearance experiments⇒ Lower E and longer L⇒ are more sensitive to lower ∆m2
• Accelerator appearance experiments⇒ higher E shorter L more precision⇒ better limits on mixing
• To reach small ∆m2 & 10−4 eV2
⇒ very large L and intermediate E⇒ Long Baseline Exp at Accelerators
• To reach smaller ∆m2 & 10−5 eV2
⇒ Long Baseline Exp at Reactors
![Page 120: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/120.jpg)
Physics of Massive Neutrinos Concha Gonzalez-GarciaATM Test at Long Baseline Experiments
K2K νµ at KEK SK L=250 kmMINOS νµ at Fermilab Soundan L=735 km
Opera νµ at CERN Gran Sasso L=740 km
K2K 2004: spectral distortion
0
4
8
12
Even
ts / 0
.2 (G
eV)
0 1 5432Eν
rec (GeV)
16
Confirmation of ATM oscillations
★
0.1 1 10
tan2 θ
0
1
2
3
4
5
6
∆m2 [1
0-3 e
V2 ]
K2K
MINOS 2006: spectral distortion
Impact on ∆m2 Determination
0.1 1 10
tan2 θ
0
1
2
3
4
5
6
∆m2 [1
0-3 e
V2 ]
MINOS
![Page 121: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/121.jpg)
Physics of Massive Neutrinos Concha Gonzalez-GarciaATM Test at Long Baseline Experiments
K2K νµ at KEK SK L=250 kmMINOS νµ at Fermilab Soundan L=735 km
Opera νµ at CERN Gran Sasso L=740 km
K2K 2004: spectral distortion
0
4
8
12
Even
ts / 0
.2 (G
eV)
0 1 5432Eν
rec (GeV)
16
Confirmation of ATM oscillations
★
0.1 1 10
tan2 θ
0
1
2
3
4
5
6
∆m2 [1
0-3 e
V2 ]
K2K
MINOS 2006: spectral distortion
Impact on ∆m2 Determination
0.1 1 10
tan2 θ
0
1
2
3
4
5
6
∆m2 [1
0-3 e
V2 ]
MINOS
![Page 122: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/122.jpg)
Physics of Massive Neutrinos Concha Gonzalez-GarciaATM Test at Long Baseline Experiments
K2K νµ at KEK SK L=250 kmMINOS νµ at Fermilab Soundan L=735 km
Opera νµ at CERN Gran Sasso L=740 km
K2K 2004: spectral distortion
0
4
8
12
Even
ts / 0
.2 (G
eV)
0 1 5432Eν
rec (GeV)
16
Confirmation of ATM oscillations
★
0.1 1 10
tan2 θ
0
1
2
3
4
5
6
∆m2 [1
0-3 e
V2 ]
K2K
MINOS 2006: spectral distortion
Impact on ∆m2 Determination
0.1 1 10
tan2 θ
0
1
2
3
4
5
6
∆m2 [1
0-3 e
V2 ]
MINOS
![Page 123: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/123.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Altenative Oscillation Mechanisms• Oscillations are due to:
– Misalignment between CC-int and propagation states: Mixing ⇒ Amplitude
– Difference phases of propagation states ⇒ Wavelength. For ∆m2-OSC λ =4πE
∆m2
• ν masses are not the only mechanism for oscillations
Violation of Equivalence Principle (VEP): Gasperini 88, Halprin,Leung 01
Non universal coupling of neutrinos γ1 6= γ2 to graviational potential φ
λ =π
E|φ|δγ
Violation of Lorentz Invariance (VLI): Coleman, Glashow 97
Non universal asymptotic velocity of neutrinos c1 6= c2 ⇒ Ei =m2
i
2p+ cip
λ =2π
E∆c
Interactions with space-time torsion: Sabbata, Gasperini 81
Non universal couplings of neutrinos k1 6= k2 to torsion strength Q
λ =2π
Q∆k
Violation of Lorentz Invariance (VLI) Colladay, Kostelecky 97; Coleman, Glashow 99
due to CPT violating terms: ν̄αLbαβ
µ γµνβL ⇒ Ei =
m2
i
2p ± bi λ = ± 2π
∆b
![Page 124: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/124.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Altenative Oscillation Mechanisms• Oscillations are due to:
– Misalignment between CC-int and propagation states: Mixing ⇒ Amplitude
– Difference phases of propagation states ⇒ Wavelength. For ∆m2-OSC λ =4πE
∆m2
• ν masses are not the only mechanism for oscillations
Violation of Equivalence Principle (VEP): Gasperini 88, Halprin,Leung 01
Non universal coupling of neutrinos γ1 6= γ2 to graviational potential φ
λ =π
E|φ|δγ
Violation of Lorentz Invariance (VLI): Coleman, Glashow 97
Non universal asymptotic velocity of neutrinos c1 6= c2 ⇒ Ei =m2
i
2p+ cip
λ =2π
E∆c
Interactions with space-time torsion: Sabbata, Gasperini 81
Non universal couplings of neutrinos k1 6= k2 to torsion strength Q
λ =2π
Q∆k
Violation of Lorentz Invariance (VLI) Colladay, Kostelecky 97; Coleman, Glashow 99
due to CPT violating terms: ν̄αLbαβ
µ γµνβL ⇒ Ei =
m2
i
2p ± bi λ = ± 2π
∆b
![Page 125: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/125.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ATM ν’s: Subdominant NP Effects
Pνµ→νµ= 1 − sin2 2Θ sin2
(
∆m2L
4ER
)
R cos 2Θ = cos 2θ +∑
n
Rn cos 2ξn
R sin 2Θ = sin 2θ +∑
n
Rn sin 2ξn eiηn
Rn = σ+n
∆δnEn
2
4E
∆m2
-1 -0.5 0 0.5 10.5
0.6
0.7
0.8
0.9
1
SK sub-GeV (µ)
OscillationsVLI CPT evenTORSION
-1 -0.5 0 0.5 10.4
0.5
0.6
0.7
0.8
0.9
1
SK multi-GeV (µ)
-1 -0.8 -0.6 -0.4 -0.2 0
cos θ
0.4
0.5
0.6
0.7
0.8
0.9
1
SK stop (µ)
-1 -0.8 -0.6 -0.4 -0.2 0
cos θ
0.6
0.8
1
1.2
1.4
SK thru (µ)
• Questions:
– Do these effects affect our determination of oscillation parameters?
– Can we limit these effects?
![Page 126: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/126.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
ATM ν’s: Subdominant NP EffectsMCG-G, M. Maltoni 04,07
★
1
2
3
4
5
∆m2 31
[10-3
eV
2 ]
n=1 CPT even
10-27
10-26
10-25
10-24
10-23
∆δ1
n=1 CPT even
★
1
2
3
4
5
∆m2 31
[10-3
eV
2 ]
n=0 CPT odd
10-24
10-23
10-22
10-21
∆δ0 [G
eV]
n=0 CPT odd
★
0 0.25 0.5 0.75 1
sin2 θ23
1
2
3
4
5
∆m2 31
[10-3
eV
2 ]
n=0 CPT even
-1 -0.5 0 0.5 1
sin 2ξn
10-24
10-23
10-22
10-21
∆δ0 [G
eV]
n=0 CPT even
At 90% CL:|∆c|
c≤ 1.2 × 10−24
|φ ∆γ| ≤ 5.9 × 10−25
|∆b| ≤ 3.0 × 10−23 GeV
|Q∆k| ≤ 4.8 × 10−23 GeV
|εdµµ − εd
ττ | ≤ 0.012
|εdµτ | ≤ 0.038
![Page 127: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/127.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Future Bounds on New Physics: ν Telescopes
At ν Telescopes (Amanda, Antares, IceCube)Eν,thres & 100 GeVLarge # ATM ν′s
(∼ 105νµ events/yr at ICECUBE)⇒ Standard oscillations suppressed⇒ Better sensitivity to Oscillations due to NP
102
103
104
105
Eµ [GeV]
0.6
0.8
1
1.2
1.4
1.6
1.8
2
p horiz
/ p ve
rt
10-2810
-2710-2610
-25
10-24
Solid=νµ+ντ Dashed=νµ only
δc/c = vary, ξ = 45
pi = Ni / Niosc
vert=[-1.0, -0.6] horiz=[-0.6, -0.2]
Expected Sensitivity at IceCube
0 0.25 0.5 0.75 1
sin2 2ξ
10-28
10-27
10-26
10-25
10-24
δc/c
2|φ
| ∆γ
SK excluded (3σ)
Solid = RQPM
Lines = TIG
MCG-G, Halzen,Maltoni, 05
![Page 128: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/128.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary II
• If mν 6= 0 → Lepton Mixing≡ breaking of Le × Lµ × Lτ
• From direct searches of ν-mass: mν ≤ O(eV )
• Neutrino masses and mixing ⇒ Flavour oscillations
• Experiments observing oscillations ⇒ measurement of ∆m2ij and θij
• Atmospheric, K2K and MINOS (+ negative SBL searches)⇒ νµ → ντ with ∆m2 ∼ 2 × 10−3 eV2 and tan2 θ ∼ 1
• Possible alternative oscillation scenarios due to non-universal VLI, VWEP, etc...But Strongly Constrained from Existing Oscillation Data
![Page 129: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/129.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary II
• If mν 6= 0 → Lepton Mixing≡ breaking of Le × Lµ × Lτ
• From direct searches of ν-mass: mν ≤ O(eV )
• Neutrino masses and mixing ⇒ Flavour oscillations
• Experiments observing oscillations ⇒ measurement of ∆m2ij and θij
• Atmospheric, K2K and MINOS (+ negative SBL searches)⇒ νµ → ντ with ∆m2 ∼ 2 × 10−3 eV2 and tan2 θ ∼ 1
• Possible alternative oscillation scenarios due to non-universal VLI, VWEP, etc...But Strongly Constrained from Existing Oscillation Data
![Page 130: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/130.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary II
• If mν 6= 0 → Lepton Mixing≡ breaking of Le × Lµ × Lτ
• From direct searches of ν-mass: mν ≤ O(eV )
• Neutrino masses and mixing ⇒ Flavour oscillations
• Experiments observing oscillations ⇒ measurement of ∆m2ij and θij
• Atmospheric, K2K and MINOS (+ negative SBL searches)⇒ νµ → ντ with ∆m2 ∼ 2 × 10−3 eV2 and tan2 θ ∼ 1
• Possible alternative oscillation scenarios due to non-universal VLI, VWEP, etc...But Strongly Constrained from Existing Oscillation Data
![Page 131: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/131.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary II
• If mν 6= 0 → Lepton Mixing≡ breaking of Le × Lµ × Lτ
• From direct searches of ν-mass: mν ≤ O(eV )
• Neutrino masses and mixing ⇒ Flavour oscillations
• Experiments observing oscillations ⇒ measurement of ∆m2ij and θij
• Atmospheric, K2K and MINOS (+ negative SBL searches)⇒ νµ → ντ with ∆m2 ∼ 2 × 10−3 eV2 and tan2 θ ∼ 1
• Possible alternative oscillation scenarios due to non-universal VLI, VWEP, etc...But Strongly Constrained from Existing Oscillation Data
![Page 132: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/132.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary II
• If mν 6= 0 → Lepton Mixing≡ breaking of Le × Lµ × Lτ
• From direct searches of ν-mass: mν ≤ O(eV )
• Neutrino masses and mixing ⇒ Flavour oscillations
• Experiments observing oscillations ⇒ measurement of ∆m2ij and θij
• Atmospheric, K2K and MINOS (+ negative SBL searches)⇒ νµ → ντ with ∆m2 ∼ 2 × 10−3 eV2 and tan2 θ ∼ 1
• Possible alternative oscillation scenarios due to non-universal VLI, VWEP, etc...But Strongly Constrained from Existing Oscillation Data
![Page 133: IceCube Neutrino Observatoryhalzen/notes/week14-2.pdf · IceCube Neutrino Observatory](https://reader033.vdocuments.site/reader033/viewer/2022060602/60562481da7c5b57314f8fdd/html5/thumbnails/133.jpg)
Physics of Massive Neutrinos Concha Gonzalez-Garcia
Summary II
• If mν 6= 0 → Lepton Mixing≡ breaking of Le × Lµ × Lτ
• From direct searches of ν-mass: mν ≤ O(eV )
• Neutrino masses and mixing ⇒ Flavour oscillations
• Experiments observing oscillations ⇒ measurement of ∆m2ij and θij
• Atmospheric, K2K and MINOS (+ negative SBL searches)⇒ νµ → ντ with ∆m2 ∼ 2 × 10−3 eV2 and tan2 θ ∼ 1
• Possible alternative oscillation scenarios due to non-universal VLI, VWEP, etc...But Strongly Constrained from Existing Oscillation Data