2015/04/07 by D. Xiao, Z. G. Dai
Physics and Astronomy · #Adiabatic process #Astrophysics and Cosmic Phenomena #Energy (signal processing) #Gamma-ray burst #Gamma-ray bursts and supernovae #Jet (fluid) #Mixing (physics) #Neutrino #Neutrino Physics Research #Neutrino oscillation #Oscillation (cell signaling) #Sterile neutrino #astro-ph.HE
paper · pdf · doi:10.1088/0004-637x/805/2/137
18 pages, 7 figures, accepted for publication in ApJ
arxiv created 2015/04/07 · openalex publication_date 2015/05/28 · arxiv updated 2015/06/03 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
There is evidence that long-duration gamma-ray bursts (GRBs) originate from the core collapse of massive stars. When a jet punctures through the progenitor envelope, high-energy neutrinos can be produced by the reverse shock formed at the jet head. It is suggested that low-luminosity GRBs are possible candidates of this high-energy neutrino precursor up to scales. Before leaving the progenitor, these high-energy neutrinos must oscillate from one flavor to another with the matter effect in the envelope. Under the assumption of a power-law stellar envelope density profile with an index α , we study the properties of TeV–PeV neutrino oscillation. We find that adiabatic conversion is violated for these neutrinos so we calibrate the level crossing effect. The resonance condition is reached for different energies at different radii. We note that the effective mixing angles in matter for neutrinos are close to zero, so the transition probabilities from one flavor to another are almost invariant for neutrinos. We plot all the transition probabilities versus the energy of TeV–PeV neutrinos from the birth place to the surface of the progenitor. With an initial flavor ratio , we plot how the flavor ratio evolves with energy and distance when neutrinos are still in the envelope, and we find the ratio when they reach the Earth. For neutrinos, the ratio is always on Earth. In addition, we discuss the dependence of the flavor ratio on energy and α and find a good result. This dependence may provide a promising probe of the progenitor structure.