Statistics – Computation
Scientific paper
Mar 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...370..345m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 370, March 20, 1991, p. 345-354.
Statistics
Computation
18
Energetic Particles, Gamma Ray Astronomy, Particle Acceleration, Pulsars, X Ray Binaries, Accretion Disks, Computational Astrophysics, Shock Waves, Stellar Evolution, Stellar Luminosity, Stellar Mass Accretion
Scientific paper
All the major viable acceleration mechanisms suggested so far in order to explain the energy of the gamma-rays observed from Cygnus X-3 are critically reviewed. It is argued that Cyg X-3 must be an accretion-fed strong X-ray binary with negligible orbital eccentricity and cannot contain a young active pulsar. It is shown that, for reasonable assumptions, the accretion disk unipolar inductor model can be ruled out as the gamma-ray source in Cyg X-3. It is confirmed that, within the framework of standard magnetospheric theories, there is little scope for extremely efficient diffusive acceleration at the accretion shock. It is concluded that the basic 'beam-dumping' model cannot be applicable to Cyg X-3, and that the proton luminosity requirements of the source can be met if the TeV-PeV gamma-ray flux is generated by photomeson reaction on its strong X-ray field.
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