Production of high-energy cosmic neutrinos in pγ and nγ scattering. I. Neutrino yields for power-law spectra of protons and neutrons

Details Production of high-energy cosmic neutrinos in pγ and nγ scattering. I. Neutrino yields for power-law spectra of protons and neutrons Production of high-energy cosmic neutrinos in pγ and nγ scattering. I. Neutrino yields for power-law spectra of protons and neutrons

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phrvd..47.4206b&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 47, Issue 10, 15 May 1993, pp.4206-4216

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15

Neutrino, Muon, Pion, And Other Elementary Particles, Cosmic Rays, Elementary Particle Processes, Cosmic Rays

Scientific paper

For the purpose of high-energy neutrino astronomy, the rates of neutrino production through decay of pions and kaons born in pγ and nγ scattering in cosmic sources are calculated. A source is assumed to be filled with low-energy photons and high-energy protons (neutrons). The photons are assumed to be isotropically distributed, while the distribution of protons might be anisotropic. The production rate of neutrinos per unit volume of the source is given by Qνi(Eν,θ)=Yνi(ɛν)σ0n0cnp (Eν,θ), where Yνi are neutrino yields, σ0=100 μb is a normalizing value of the pγ cross section, n0 (in cm-3) is a spatial density of photons, and np(Eν,θ) (in cm-3sr-1 GeV-1) is the density of protons (neutrons) with momenta in some direction θ. The neutrino yield is shown to be a function of the product ɛν=Eνω0/m2p, with ω0 being a photon energy where the spectrum nγ(ω) has a maximum. Neutrino yields are calculated for the power-law spectra of protons, np(E)~E-(γ+1), and for several spectra of photons (namely, for the diluted Planckian spectrum with temperature T and for the power-law spectra both with and without a high-energy cutoff).

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