2005/07/31 by Tamar Kashti, Eli Waxman · 3 citations
Physics and Astronomy · #Adiabatic process #Astronomy #Astrophysics and Cosmic Phenomena #Atomic physics #Electron #Energy (signal processing) #Energy flux #Flux (metallurgy) #Gamma-ray bursts and supernovae #Lepton #Neutrino #Neutrino Physics Research #Nuclear physics #Particle physics #Physics #Thermodynamics #astro-ph #hep-ph
paper · pdf · doi:10.1103/physrevlett.95.181101
published as Phys.Rev.Lett.95:181101,2005 · v1: 4 pages, 1 figure; v2: added reference; v3: improved introduction, accepted to PRL; v4: added note about matter oscillations
arxiv created 2005/10/19 · openalex publication_date 2005/10/26 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Electromagnetic (and adiabatic) energy losses of \ensuremathπ's and \ensuremathμ's modify the flavor ratio (measured at Earth) of neutrinos produced by \ensuremathπ decay in astrophysical sources, \ensuremathΦ_\ensuremathνe\ensuremath\mathbin:\ensuremathΦ_\ensuremathν_\ensuremathμ\ensuremath\mathbin:\ensuremathΦ_\ensuremathν_\ensuremathτ, from 1\ensuremath\mathbin:1\ensuremath\mathbin:1 at low energy to 1\ensuremath\mathbin:1.8\ensuremath\mathbin:1.8 at high energy. The transition occurs over 1--2 decades of \ensuremathν energy, and is correlated with a modification of the neutrino spectrum. For \ensuremathγ-ray bursts, e.g., the transition is expected at \ensuremath∼100 TeV and may be detected by km-scale \ensuremathν telescopes. Measurements of the transition energy and energy width will provide unique probes of the physics of the sources. \ensuremathπ and \ensuremathμ energy losses also affect the ratio of \ensuremathνe flux to total \ensuremathν flux, which may be measured at the W resonance (6.3 PeV): It is modified from 1/6 (1/15) at low energy to 1/9 (practically 0) at high energy for neutrinos produced in pp (p\ensuremathγ) interactions.