Physics
Scientific paper
Aug 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001icrc....6.2517a&link_type=abstract
Proceedings of the 27th International Cosmic Ray Conference. 07-15 August, 2001. Hamburg, Germany. Under the auspices of the Int
Physics
Scientific paper
We discuss theoretical models that could explain the existing data from γ-ray observations of Cen X-3. Because of the high energetics required, any reasonable option for γ-ray production in Cen X-3 must be connected with jets emerging from the inner accretion disc of the neutron star. A large-scale quasi-stationary source (on a time scale of days or longer) powered by shocks driven by such jets into the Rs ≥ 1013 cm surrounding the binary could explain the bulk of the γ-radiation features, except for a modulation of the γ-ray signal with the pulsar spin period. These modulations, if genuine, would require an alternative source with Rs 1011 cm. We consider two principal models, hadronic and leptonic, for such a compact source in the jet. Both models predict that the pulsed γ-ray emission should be episodic, and can be expected only at the initial stages (typically less than a few hours) of powerful γ-ray flares, and that γ-ray pulsations should be significantly shifted from the pulsar frequency. Such a source would generally fade, due to expansion, in a few days.
Atoyan Armen M.
Aye Klaus-Michael
Chadwick Paula M.
Daniel M. K.
Lyons Kelly
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