Zee-Burst: Non-Standard Interactions in IceCube Yicong Sui - - PowerPoint PPT Presentation

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Zee-Burst: Non-Standard Interactions in IceCube Yicong Sui - - PowerPoint PPT Presentation

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Zee-Burst: Non-Standard Interactions in IceCube Yicong Sui Washington University in St. Louis In collaboration with K. S. Babu (OSU), P. S. Bhupal Dev (WashU), Sudip Jana (MPI) arXiv:1908.02779 Scalars in the Zee model A. Zee Phys.

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SLIDE 1

Zee-Burst: Non-Standard Interactions in IceCube

Yicong Sui Washington University in St. Louis

In collaboration with

  • K. S. Babu (OSU), P. S. Bhupal Dev (WashU),

Sudip Jana (MPI) arXiv:1908.02779

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SLIDE 2

Scalars in the Zee model

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 3

Scalars in the Zee model

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 4

Scalars in the Zee model

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 5

Scalars in the Zee model

  • A. Zee Phys. Lett.95B,461(1980)

+

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SLIDE 6

Scalars in the Zee model

  • A. Zee Phys. Lett.95B,461(1980)

+

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SLIDE 7

Scalars in the Zee model

  • A. Zee Phys. Lett.95B,461(1980)

+

Due to the structure of scalar potential, will mix with

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SLIDE 8

Scalars in the Zee model

As for the Yukawa sector, we have:

  • A. Zee Phys. Lett.95B,461(1980)

+

Due to the structure of scalar potential, will mix with

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SLIDE 9

Neutrino Mass

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 10

Neutrino Mass

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 11

Neutrino Mass

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 12

Neutrino Mass

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 13

Neutrino Mass

Mass insertion from SM VEV

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 14

Neutrino Mass

Mass insertion from SM VEV

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 15

Neutrino Mass

Mass insertion from SM VEV Charged Lepton Mass Matrix

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 16

Neutrino Mass

Mass insertion from SM VEV Charged Lepton Mass Matrix

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 17

Neutrino Mass

Super small 10^(-8) Mass insertion from SM VEV Charged Lepton Mass Matrix

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 18

Neutrino Mass

Super small 10^(-8) O(1) Mass insertion from SM VEV Charged Lepton Mass Matrix

  • A. Zee Phys. Lett.95B,461(1980)
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SLIDE 19

Neutrino Mass

Super small 10^(-8) O(1) Mass insertion from SM VEV Charged Lepton Mass Matrix

  • A. Zee Phys. Lett.95B,461(1980)

Herrero-Garcia, Ohlsson, Riad, Wiren, 2017’

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SLIDE 20

Glashow-Like Signatures

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SLIDE 21

Glashow-Like Signatures

  • S. L. Glashow 1960

g

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SLIDE 22

Glashow-Like Signatures

  • S. L. Glashow 1960

g

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SLIDE 23

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g

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SLIDE 24

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g

Chien-Yi Chen, P. S. Bhupal Dev, Amarjit Soni 2013’

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SLIDE 25

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g

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SLIDE 26

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g

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SLIDE 27

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g Y

Zee burst

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SLIDE 28

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g Y

Zee burst

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SLIDE 29

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g Y

Zee burst

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SLIDE 30

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g Y

Zee burst

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SLIDE 31

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g Y m=80.4 GeV

Zee burst

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SLIDE 32

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

g Y m=80.4 GeV m=100 GeV

Zee burst

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SLIDE 33

Glashow-Like Signatures

@ resonance, becomes dominant

  • S. L. Glashow 1960

Where to find these High Energy neutrinos? g Y m=80.4 GeV m=100 GeV

Zee burst

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SLIDE 34

Astrophysical Neutrino Sources

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SLIDE 35

Astrophysical Neutrino Sources

p p p p p p p p

hadro-nuclear production

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SLIDE 36

Astrophysical Neutrino Sources

p p p p p p p p

hadro-nuclear production

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SLIDE 37

Astrophysical Neutrino Sources

p p p p p p p p

hadro-nuclear production

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SLIDE 38

Astrophysical Neutrino Sources

p p p p p p p p

X hadro-nuclear production

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SLIDE 39

Astrophysical Neutrino Sources

p p p p p p p p

X hadro-nuclear production

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SLIDE 40

Astrophysical Neutrino Sources

p p p p p p p p

X hadro-nuclear production

γ γ

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SLIDE 41

Astrophysical Neutrino Sources

p p p p p p p p

X hadro-nuclear production ν

γ γ

μ

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SLIDE 42

Astrophysical Neutrino Sources

p p p p p p p p

X hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 43

Astrophysical Neutrino Sources

p p p p p p p p

X Starburst Galaxies, Galaxy Clusters/Groups hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 44

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p γ

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 45

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p γ

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 46

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p γ

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 47

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 48

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

ν ν μ

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SLIDE 49

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν μ

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SLIDE 50

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν μ ν μ

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SLIDE 51

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν μ ν

e

ν ν μ

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SLIDE 52

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production GRB, AGN, Radio Galaxies, Blazars, supernovae ...

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν μ ν

e

ν ν μ

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SLIDE 53

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production GRB, AGN, Radio Galaxies, Blazars, supernovae ...

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν Charged Pions Decay μ ν

e

ν ν μ

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SLIDE 54

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production GRB, AGN, Radio Galaxies, Blazars, supernovae ...

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν Charged Pions Decay μ ν

e

ν ν μ Neutrinos typically have 1-5% of proton energy Maximally:

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SLIDE 55

Astrophysical Neutrino Sources

p p p p p p p p

X

p p p p p γ p p γ n

Starburst Galaxies, Galaxy Clusters/Groups photo-hadronic production GRB, AGN, Radio Galaxies, Blazars, supernovae ...

p p p p

hadro-nuclear production ν

γ γ

e

γ γ

ν ν Charged Pions Decay μ ν

e

ν ν μ Neutrinos typically have 1-5% of proton energy

How do we detect them?

Maximally:

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SLIDE 56

IceCube Detector

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SLIDE 57

track

IceCube Detector

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SLIDE 58

track cascade

IceCube Detector

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SLIDE 59

Mechanism:

Cherenkov radiation from interaction products: leptons and hadrons

track cascade

IceCube Detector

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SLIDE 60

Mechanism:

Cherenkov radiation from interaction products: leptons and hadrons

track cascade

IceCube Detector

nu e interactions dominates in special case

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SLIDE 61

IC signal simulation

The IceCube Collaboration, 2017, 2019

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SLIDE 62

IC signal simulation

The IceCube Collaboration, 2017, 2019

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SLIDE 63

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

The IceCube Collaboration, 2017, 2019

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SLIDE 64

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

T : Exposure time is 2635 days

The IceCube Collaboration, 2017, 2019

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SLIDE 65

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

T : Exposure time is 2635 days

The IceCube Collaboration, 2017, 2019

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SLIDE 66

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

T : Exposure time is 2635 days

The IceCube Collaboration, 2017, 2019

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SLIDE 67

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

T : Exposure time is 2635 days

HESE e neutrino effective area HESE muon neutrino effective area

The IceCube Collaboration, 2017, 2019

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SLIDE 68

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

T : Exposure time is 2635 days

HESE e neutrino effective area HESE muon neutrino effective area 6.3 PeV

The IceCube Collaboration, 2017, 2019

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SLIDE 69

IC signal simulation

HESE effective area, sum of cross sections for all the particles in the detector, an effective total cross section

T : Exposure time is 2635 days

HESE e neutrino effective area HESE muon neutrino effective area Glashow Peak 6.3 PeV

The IceCube Collaboration, 2017, 2019

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SLIDE 70

Spectrum plot

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SLIDE 71

Spectrum plot

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SLIDE 72

Spectrum plot

Glashow Peak

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SLIDE 73

Spectrum plot

Glashow Peak

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SLIDE 74

Spectrum plot

Glashow Peak Zee Burst

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SLIDE 75

NSI from Zee Model

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SLIDE 76

NSI from Zee Model

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SLIDE 77

NSI from Zee Model

Effectively, we have:

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SLIDE 78

NSI from Zee Model

Effectively, we have:

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SLIDE 79

NSI from Zee Model

Effectively, we have:

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SLIDE 80

NSI from Zee Model

Effectively, we have: Condition for Maximum contribution to NSI and to Zee burst:

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SLIDE 81

Sensitivity of IceCube and DUNE

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SLIDE 82

Sensitivity of IceCube and DUNE

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SLIDE 83

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity

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SLIDE 84

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity

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SLIDE 85

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter

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SLIDE 86

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter

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SLIDE 87

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI

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SLIDE 88

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search

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SLIDE 89

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search

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SLIDE 90

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search LEP monophoton

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SLIDE 91

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search LEP monophoton nu e scattering: BOREXINO

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SLIDE 92

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search LEP monophoton nu e scattering: BOREXINO IceCube Atm.

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SLIDE 93

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search LEP monophoton nu e scattering: BOREXINO IceCube Atm. Oscillation + COHERENT

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SLIDE 94

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search LEP monophoton nu e scattering: BOREXINO IceCube Atm. Oscillation + COHERENT

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SLIDE 95

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI LEP direct search LEP di-lepton search LEP monophoton nu e scattering: BOREXINO IceCube Atm. Oscillation + COHERENT

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SLIDE 96

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI

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SLIDE 97

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI Double-dip feature is due to the double peak cross section feature:

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SLIDE 98

Sensitivity of IceCube and DUNE

IceCube Zee Burst Sensitivity Magnitude of parameter DUNE sensitivity for NSI Double-dip feature is due to the double peak cross section feature: mH – mh = 30 GeV

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SLIDE 99

Conclusion

  • We proposed a new way to probe light charged

scalars using a Glashow-like resonance in the UHE neutrino data (IceCube).

  • The same interactions for Glashow-like resonance

also give rise to observable NSI effect.

  • UHE neutrinos provide a complementary probe of

NSI.

  • We have used the popular Zee model of radiative

neutrino mass as a demonstration.

  • Further extensions to other models are possible

and promising.

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SLIDE 100

Thank you!