Figure 11: Solid line: predicted value of the Shapiro delay in PSR J0437–4715 as a function of orbital phase, based on the observed inclination angle of 42° ± 9°. For such low-eccentricity binaries, much of the Shapiro delay can be absorbed into the orbital Roemer delay; what remains is the periodicity shown. The points represent the timing residuals for the pulsar, binned in orbital phase, and in clear agreement with the shape predicted from the inclination angle. (Reprinted by permission from Nature [139], Ⓒ 2001, Macmillan Publishers Ltd.)