Astrophysical neutrino source searches with IceCube starting track events

Cosmic rays and neutrinos are intimately related. And though TeVPeV astrophysical neutrinos have been observed, their sources and their relation to potential sources of cosmic rays remain unknown. Recently, the blazar TXS 0506+056 has been identified as a candidate neutrino source. In parallel, IceCube has conducted numerous searches for other potential neutrino neutrino sources. These proceedings are limited in scope, given the large breath of science results by IceCube: A description of the astrophysical neutrino flux; a review of the real-time program that enables multi-messenger follow-up of neutrinos; a summary of the observations of TXS 0506+056; a recap of the search for neutrino point sources with 7 years of IceCube data; an account of the tantalizing capabilities of IceCube and ANTARES to detect Milky Way neutrinos and a description of a method to identify Glashow resonance events.

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Bayesian constraints on the astrophysical neutrino source population from IceCube data

Physical Review D ◽

10.1103/physrevd.101.123017 ◽

2020 ◽

Vol 101 (12) ◽

Cited By ~ 1

Author(s):

F. Capel ◽

D. J. Mortlock ◽

C. Finley

Keyword(s):

Source Population ◽

Neutrino Source ◽

Astrophysical Neutrino

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INTRINSIC AND OSCILLATED ASTROPHYSICAL NEUTRINO FLAVOR RATIOS REVISITED

Modern Physics Letters A ◽

10.1142/s021773230602038x ◽

2006 ◽

Vol 21 (13) ◽

pp. 1049-1065 ◽

Cited By ~ 30

Author(s):

H. ATHAR ◽

C. S. KIM ◽

JAKE LEE

Keyword(s):

Neutrino Oscillations ◽

Muon Neutrinos ◽

Neutrino Source ◽

Tau Neutrinos ◽

Neutrino Flavor ◽

Astrophysical Neutrinos ◽

Astrophysical Neutrino

The pp interactions taking place in the cosmos around us are a source of the astrophysical neutrinos of all the three flavors. In these interactions, the electron and the muon neutrinos mainly come from the production and the decay of the π± mesons, whereas the tau neutrinos mainly come from the production and the decay of the [Formula: see text] mesons. We estimate the three intrinsic neutrino flavor ratios for 1 GeV ≤E≤1012 GeV in the pp interactions and found them to be 1:2:3×10-5. We study the effects of neutrino oscillations on these intrinsic ratios. We point out that the three ratios become 1:1:1 if L (pc)/E(GeV) ≥10-10 in the presence of neutrino oscillations, where L is the distance to the astrophysical neutrino source in units of parsecs.

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