Origin of ultra-high-energy gamma-rays from Cygnus X-3 and related sources

Details Origin of ultra-high-energy gamma-rays from Cygnus X-3 and related sources Origin of ultra-high-energy gamma-rays from Cygnus X-3 and related sources

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986natur.319..380k&link_type=abstract

Nature (ISSN 0028-0836), vol. 319, Jan. 30, 1986, p. 380-382.

Astronomy and Astrophysics

Astronomy

68

Accretion Disks, Gamma Ray Astronomy, Neutron Flux Density, Particle Acceleration, Shock Waves, X Ray Binaries, Cosmic Rays, Helium Isotopes, Ions, Photodissociation, Proton-Proton Reactions

Scientific paper

Ultra-high-energy (UHE) γ-ray emission from Cygnus X-3 and the several other binary X-ray sources has been observed at γ-ray energies ≥1015eV. Also, collisionless shocks are expected to form in accretion flows onto neutron stars or black holes. The authors consider the diffusive shock acceleration of ions as the mechanism responsible for the γ-ray emission observed. The shock can accelerate ions to energies near 1016eV. The subsequent proton-proton (p-p) collisions and photodissociation of 4He can produce a flux of neutrons that escapes from the acceleration site despite the high magnetic fields (≡108G). These neutrons, by interacting with the binary companion, produce the observed UHE radiation.

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