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

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. Lett.95B,461(1980)

Scalars in the Zee model A. Zee Phys. Lett.95B,461(1980)

Scalars in the Zee model A. Zee Phys. Lett.95B,461(1980)

Scalars in the Zee model A. Zee Phys. Lett.95B,461(1980) +

Scalars in the Zee model A. Zee Phys. Lett.95B,461(1980) +

Scalars in the Zee model A. Zee Phys. Lett.95B,461(1980) + Due to the structure of scalar potential, will mix with

Scalars in the Zee model A. Zee Phys. Lett.95B,461(1980) + Due to the structure of scalar potential, will mix with As for the Yukawa sector, we have:

Neutrino Mass A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Charged Lepton Mass Matrix Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Charged Lepton Mass Matrix Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Super small 10^(-8) Charged Lepton Mass Matrix Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Super small O(1) 10^(-8) Charged Lepton Mass Matrix Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Neutrino Mass Herrero-Garcia, Ohlsson, Riad, Wiren, 2017’ Super small O(1) 10^(-8) Charged Lepton Mass Matrix Mass insertion from SM VEV A. Zee Phys. Lett.95B,461(1980)

Glashow-Like Signatures

Glashow-Like Signatures g S. L. Glashow 1960

Glashow-Like Signatures g S. L. Glashow 1960

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Chien-Yi Chen, P. S. Bhupal Dev, Amarjit Soni 2013’

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst m=80.4 GeV

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst m=100 GeV m=80.4 GeV

Glashow-Like Signatures g @ resonance, becomes dominant S. L. Glashow 1960 Y Zee burst Where to find these High Energy neutrinos? m=100 GeV m=80.4 GeV

Astrophysical Neutrino Sources

Astrophysical Neutrino Sources hadro-nuclear production p p p p p p p p

Astrophysical Neutrino Sources hadro-nuclear production p p p p p p p p

Astrophysical Neutrino Sources hadro-nuclear production p p p p p p p p

Astrophysical Neutrino Sources hadro-nuclear production p p p p X p p p p

Astrophysical Neutrino Sources hadro-nuclear production p p p p X p p p p

Astrophysical Neutrino Sources hadro-nuclear production p p p p X p p p p γ γ

Astrophysical Neutrino Sources hadro-nuclear production p p p p X p p p p μ ν γ γ

Astrophysical Neutrino Sources hadro-nuclear production p p p p X p p p p μ ν e γ γ ν ν

Astrophysical Neutrino Sources hadro-nuclear production p p p p X p p p p Starburst Galaxies, Galaxy Clusters/Groups μ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p γ X p p p p p γ p p Starburst Galaxies, p Galaxy Clusters/Groups p μ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p γ X p p p p p γ p p Starburst Galaxies, p Galaxy Clusters/Groups p μ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p γ X p p p p p γ p p Starburst Galaxies, p Galaxy Clusters/Groups p μ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ μ ν ν e γ γ ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ μ ν ν e e γ γ ν ν ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ μ ν GRB, AGN, Radio ν Galaxies, Blazars, e supernovae ... e γ γ ν ν ν ν

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ μ ν GRB, AGN, Radio ν Galaxies, Blazars, e supernovae ... e γ γ ν ν ν ν Charged Pions Decay

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ μ ν GRB, AGN, Radio ν Galaxies, Blazars, e supernovae ... e γ γ ν ν ν ν Charged Pions Decay Neutrinos typically have 1-5% of proton energy Maximally:

Astrophysical Neutrino Sources photo-hadronic hadro-nuclear production production p p p p p p p p p p γ X p p p p p γ p n p Starburst Galaxies, p Galaxy Clusters/Groups p μ γ γ μ ν GRB, AGN, Radio ν Galaxies, Blazars, e supernovae ... e γ γ ν ν ν ν Charged Pions Decay How do we detect Neutrinos typically have 1-5% of proton energy them? Maximally:

IceCube Detector

IceCube Detector track

IceCube Detector track cascade

IceCube Detector track cascade Mechanism: Cherenkov radiation from interaction products: leptons and hadrons

IceCube Detector track cascade Mechanism: Cherenkov radiation from interaction products: leptons and hadrons nu e interactions dominates in special case

IC signal simulation The IceCube Collaboration, 2017, 2019

IC signal simulation The IceCube Collaboration, 2017, 2019

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

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

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

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

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 muon neutrino effective area HESE e neutrino effective area The IceCube Collaboration, 2017, 2019