  This project examines the feasibility of using gravitational lensing to
measure the mass of compact objects in eclipsing X-ray binary (XRB) systems. We
investigate which kind of XRB would be most conducive for viewing the effect,
by modeling the amplification curves and determining if any feature of an XRB
system could potentially hinder observation of such a signal. We examine the
effect of accretion disks and stellar winds, as well as the compact object
mass, binary separation, and companion spectral type. Generally speaking, the
lensing signal is strongest for when the angular size subtended by the
companion is small, favoring relatively compact companion stars (LMXBs)
although evolved massive stars (such as certain WR stars) have signals that are
feasibly detectable. Interestingly, the self-lensing signal is stronger in
binaries with large separations, which is the exact opposite of the case for
all other techniques. Thus, a dedicated self-lensing survey would complement
X-ray and radial-velocity techniques, by extending the parameter space for
discovery of compact objects. Simultaneously, a self-lensing survey offers the
possibility of revealing the large population of non-accreting compact objects
in galactic binary systems.
