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- W2045621839 abstract "An experimentally verifiable model is developed to explain the discrepancy between detected TeV γ-ray pulsed periods and neutron star spin periods in X-ray binary systems. It assumes that the TeV γ-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 4 × 10−5. 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." @default.
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- W2045621839 date "1997-06-01" @default.
- W2045621839 modified "2023-09-25" @default.
- W2045621839 title "The source of TeV gamma-rays in Cen X-3 and Vela X-1" @default.
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- W2045621839 doi "https://doi.org/10.1016/s0927-6505(96)00076-x" @default.
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