Owing to the proximity of the PSR J0437-4715 system, relative changes in the positions of the Earth and pulsar result in both annual and secular evolution of the line of sight to the pulsar. Although the changes are miniscule, the effects on the projected orbital parameters are detectable in our data at a high level of significance, necessitating the implementation of an improved timing model.
In addition to producing estimates of astrometric parameters with unparalleled precision, the study has also yielded the first three-dimensional orbital geometry of a binary pulsar. This includes the first classical determination of the orbital inclination, providing the unique opportunity to verify the shape of the Shapiro delay and thereby independently confirm a general relativistic prediction.
With a current post-fit arrival time residual r.m.s. of merely 130 ns over four years, the unrivaled quality of the timing data presented herein may eventually provide the most stringent limit on the energy density of the proposed stochastic gravitational wave background. Continuing the quest for even greater timing precision, a detailed study of the polarimetry of PSR J0437-4715 was undertaken. This effort resulted in the development of a new, phase-coherent technique for calibrating the instrumental response of the observing system.
Observations were conducted at the Parkes 64-m radio telescope in New
South Wales, Australia, using baseband recorder technologies developed
at York University, Toronto, and at the California Institute of
Technology. Data were processed offline at Swinburne University using
a beowulf-style cluster of high-performance workstations and custom
software developed by the candidate as part of this thesis.
Final version of dissertation: str03.ps.gz (773 kB) wvanstratenthesis.pdf (3 MB)