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An improved formula for the timing of binary pulsars that accounts for therelativistic deflection of light in the gravitational field of the pulsar'scompanion is presented, and the measurability of this effect together with itsvariance estimates are discussed. The deflection of the pulsar's beamtrajectory in the gravitational field of its companion leads to variation inthe pulsar's rotational phase. This variation appears as the narrow sharpgrowth of the magnitude of the post-fit pulsar timing residuals in the vicinityof the moment of the superior conjunction of the pulsar with its companion. Incontrast to the relativistic Shapiro effect the amplitude of the effect ofgravitational deflection of the pulsar radio beam has two peaks with oppositesigns, which become sharper as the inclination $i$ of the pulsar's orbitapproaches 90$^{\circ}$. The effect under consideration influences theestimation of parameters of the relativistic Shapiro effect in the binarypulsars with nearly edgewise orbits. Its inclusion in the fitting procedureprovide more careful measurement of sine of the orbital inclination $i$ as wellas the masses of the pulsar $m_p$ and its companion $m_c$. This permits animproved testing of alternative theories of gravity in the strong field regime.Moreover, the measurement of this effect permits independent geometricconstraints on the position of the pulsar rotational axis in space. The effectof the gravitational deflection of light has been numerically investigated forbinary pulsars with nearly edgewise orbits. It is shown that the effect isobserved in general only when $\cos i\leq 0.003.$ This estimate becomes lessrestrictive as the pulsar's spin axis approaches the line of the sight.Comment: 8 pages, uuencoded compressed PostScript file, 6 figures included.  Accepted for publication in MNRAS, 5-Jan-199

Relativistic effect of gravitational deflection of light in binary pulsars