The source of TeV gamma-rays in CEN X-3 and VELA X-1

Details The source of TeV gamma-rays in CEN X-3 and VELA X-1 The source of TeV gamma-rays in CEN X-3 and VELA X-1

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aph.....7...63r&link_type=abstract

ASTROPARTICLE PHYSICS, Volume 7, Issue 1-2, p. 63-71.

Physics

5

Scientific paper

An experimentally verifiable model is developed to explain the discrepancy between detected TeV gamma-ray pulsed periods and neutron star spin periods in X-ray binary systems. It assumes that the TeV gamma-rays are produced at the X-ray period and not on the neutron star itself, but somewhere else in the orbital plane. It was successfully applied to both Cen X-3 and Vela X-1. In the case of Cen X-3, an emission region was identified, with a 99.5% significance. This region trails the neutron star by 70^∘ and is situated between the neutron star orbit and the companion. For Vela X-1 an emission region outside the orbit of the neutron star was found, with a probability for chance occurrence of 4x10^-5. This region leads the neutron star by 90^∘. These detections were used to illustrate the characteristics of the model, especially parameters determining its applicability and possible limitations.

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