Other
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...425..782m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 425, no. 2, p. 782-786
Other
4
Gamma Rays, High Energy Interactions, Neutron Stars, Particle Acceleration, Particle Production, Gamma Ray Observatory, Hadrons, Magnetopause, Pions, Shock Wave Propagation, Stellar Mass Accretion, X Ray Binaries
Scientific paper
We develope here a model for ultra-high-energy gamma-ray production in Cygnus X-3 based on our earlier suggestion that in the presence of a strong soft X-ray field around the putative neutron star, the most dominant mechanism for cooling of the ultra-high-energy (UHE) protons should be the photomeson process which, in turn, should give rise to Very-High-Energy (VHE) - UHE gamma-rays. We envisage the spherical accretion shock around the neutron star to be specially conducive to acceleration of protons following supposed minor enhanced mass accretion and concomitant recession of the magnetopause due to enhanced radiation pressure at suitable orbital phases. It is also assumed that the accretion shock is quasi-perpendicular to enable fastest possible acceleration of protons. Relatively lower energy protons remain trapped in the magnetosphere yielding relatively lower energy pi0s and then photons. On the other hand, the highest energy protons stream out of the magnetopause (to reach a region of much lower magnetic field) and give rise to UHE gamma-rays. However, in most of the realistic cases, there may be a significant reduction of the high-energy photon luminosity because of magnetic degradation of the photons.
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