The feasibility for detection and distinguishing HNLs signals with neutrino signals in IceCube/KM3NeT neutrino telescopes were discussed andWe proposed a distinguishable double tracks events...Show moreThe feasibility for detection and distinguishing HNLs signals with neutrino signals in IceCube/KM3NeT neutrino telescopes were discussed andWe proposed a distinguishable double tracks events geometry and calculated the sensitivity curves by Mathematica. Comparison of the number of events at the lower boundary in KM3NET and CHARM experiments implied IceCube/KM3NeT has no potential for probing this kind of event. We also studied the full decay channels of HNLs and calculated the corresponding sensitivity curves in IceCube and CHARM experiments, excellent agreements were obtained by comparing the numeric sensitivity bounds with the analytic formulas. Further comparison of sensitivity curves of HNLs in both experiments indicates that IceCube has no superiority in HNLs detection. The methods to improve HNLs detection sensitivity in IceCube were also considered, where extension of working time is the most reliable way. Besides, IceCube sensitivity may exceed CHARM by increasing the detector area and/or decay volume length, thus, IceCube gen2 is prospective to contribute to HNLs detection.Show less
We look for cosmic neutrinos originating in Gamma Ray bursts using public data from the IceCube collaboration. We allow for a time difference between a neutrino and GRB photon of up to 40 days to...Show moreWe look for cosmic neutrinos originating in Gamma Ray bursts using public data from the IceCube collaboration. We allow for a time difference between a neutrino and GRB photon of up to 40 days to probe possible Lorentz invariance violations. These violations might become visible if a neutrino has high enough energy and traveled a long enough distance before we observe it. We make use of pseudo experiments to simulate different possible neutrino realizations and see how well a signal can be discerned from background. We find slightly less neutrinos than expected from background in the IceCube data. A signal associated with more than 3% of the GRBs can be excluded at 98% confidence in the northern hemisphere, and at 70% confidence in the southern hemisphere. Under the assumption that the highest energy neutrinos that can be associated to a GRB are experiencing LIV induced time shifts we have derived an intrinsic time difference at emission between GRB neutrinos and photons of ∆tin = (4.49 ± 23.0) 10^4s, and a LIV scale of ELIV = (1.05 ± 0.85) 10^15GeV, while the probability of finding similar results from purely uncorrelated events is P = 54%.Show less
