High energy neutrino yields from astrophysical sources II: Magnetized sources

Abstract

We calculate the yield of high energy neutrinos produced in astrophysical sources for arbitrary interaction depths ${\tau }_0$ and magnetic field strengths $B$. We take into account energy loss processes like synchrotron radiation and diffusion of charged particles in turbulent magnetic fields as well as the scattering of secondaries on background photons and the direct production of charm neutrinos. Meson-photon interactions are simulated with an extended version of the SOPHIA model. Diffusion leads to an increased path-length before protons leave the source of size R_s and therefore magnetized sources lose their transparency below the energy $E\sim 10^{18}\mathrm{eV}(R_s/\mathrm{pc})(B/\mathrm{mG}){\tau }_0^{1/\alpha }$, with $\alpha =1/3$ and 1 for Kolmogorov and Bohm diffusion, respectively. Moreover, the neutrino flux is suppressed above the energy where synchrotron energy losses become important for charged particles. As a consequence, the energy spectrum and the flavor composition of neutrinos are strongly modified both at low and high energies even for sources with $τ_0\lsim 1$.

15 pages, 16 figures

References in corpus (3)

• Revealing the Supernova--Gamma-Ray Burst Connection with TeV Neutrinos
• Neutrino flux ratios at neutrino telescopes: The role of uncertainties of neutrino mixing parameters and applications to neutrino decay
• Oscillation effects on high-energy neutrino fluxes from astrophysical hidden sources

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