  We calculate the amplitude of the Lyman discontinuity for an accretion disk
around a maximally rotating black hole. The locally emitted disk spectrum is
computed with a previously developed numerical model (Sincell and Krolik 1998)
and then a new general relativistic ray-tracing code is used to determine the
observed spectra as a function of inclination angle, theta_o. We find that
Lyman discontinuities are undetectable for disks viewed at inclinations
cos(theta_o) < 0.8, but a significant feature remains for disks seen face-on.
