  The values of the bending delays in the signal of a radio pulsar in a binary
with a stellar mass black hole as a companion have been calculated accurately
within a full general relativistic framework considering the Schwarzchid
spacetime near the companion. The results match with the pre-existing
approximate analytical expressions unless both of the orbital inclination angle
and the orbital phase are close to $90^{\circ}$. For such a case, the
approximate analytical expressions underestimate the value of the bending
delay. On the other hand, for systems like the double pulsar, those expressions
are valid throughout the orbital phase, unless its inclination angle is very
close to 90 degrees. For a pulsar-black hole binary, the bending phenomenon
also increases the strength of the pulse profile and sometimes can lead to a
small low intensity tail.
