What predictions did NS-Capture make about the existence of the class of Be X-Ray Binaries?
When the NS-Capture Theory was discovered in 1974, it implied that there were many neutron stars in the Milky Way galaxy that randomly would collide and end up gravitationally bound to visible stars in the Galaxy.
Because giant stars provide much larger targets for collision and binding, it was expected that giant stars would be nearly half of the stars that would end up being bound in binary systems containing an ordinary visible star and a neutron star.
After the initial binding collision the neutron star would be in a highly eccentric orbit with a giant companion, and “periodically” re-collide with the companion at the periastron of the orbit, at which time the NS would accrete material from the companion and emit x-rays.
Therefore, the prediction of NS-Capture was and is that there should be a class of giant stars with NS companions that would begin to become NS pulsars as the continued to collide with the giant star.
In addition, because orbital energy would be lost in each collision, the orbit that initially was elliptical with high eccentricity would begin to circularize, and the NS would become a spinning pulsar that would spin faster and faster as the orbit circularized.
Since the discovery of Cen X-3 and Her X-1, many more binary x-ray pulsars have been discovered, and many of those have been in the class of “Be X-Ray Binaries” (BeXRB’s) that nearly exactly fit the model described above.
While other models have been proposed to explain the BeXRB’s, it is suggested here that NS-Capture provides a consistent model for unifying all of the x-ray binary systems and that, as shown in the diagrammatic proof, NS-Capture avoids the contradictions inherent in other known models.