| In this thesis we have, through the use of numerical methods, simulated a relativistic binary star system composed of a black hole and pulsar. The purpose of the exercise is to determine the observations that would distinguish the differences between binary systems containing a black hole and those without black holes present. By integrating the Schwarzschild spacetime geodesic equations for massless particles, and examining independent physical parameters such as the pulsar spin rate, we were able to calculate the pulse arrival times expected from such a system. Of particular interest were the profiles of pulses that undergo large deflections after passing close to the black hole. Realistic pulse profiles were then computed after the intensities of the pulses had been calculated. For the case of binary systems close enough to resolve the position of the pulsar, the apparent positions of multiple images formed from gravitational lensing were also computed. |
