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We develop a general approach to analytically calculate the perturbations$\Delta\delta\tau_\textrm{p}$ of the orbital component of the change$\delta\tau_\textrm{p}$ of the times of arrival of the pulses emitted by abinary pulsar p induced by the post-Keplerian accelerations due to the massquadrupole $Q_2$, and the post-Newtonian gravitoelectric (GE) andLense-Thirring (LT) fields. We apply our results to the so-far stillhypothetical scenario involving a pulsar orbiting the Supermassive Black Holein in the Galactic Center at Sgr A$^\ast$. We also evaluate the gravitomagneticand quadrupolar Shapiro-like propagation delays $\delta\tau_\textrm{prop}$. Byassuming the orbit of the existing S2 main sequence star and a time span aslong as its orbital period $P_\textrm{b}$, we obtain$\left|\Delta\delta\tau_\textrm{p}^\textrm{GE}\right|\lesssim10^3~\textrm{s},~\left|\Delta\delta\tau_\textrm{p}^\textrm{LT}\right|\lesssim0.6~\textrm{s},\left|\Delta\delta\tau_\textrm{p}^{Q_2}\right|\lesssim0.04~\textrm{s}$. Faster $\left(P_\textrm{b} = 5~\textrm{yr}\right)$ and moreeccentric $\left(e=0.97\right)$ orbits would imply net shifts per revolution aslarge as$\left|\left\langle\Delta\delta\tau_\textrm{p}^\textrm{GE}\right\rangle\right|\lesssim10~\textrm{Ms},~\left|\left\langle\Delta\delta\tau_\textrm{p}^\textrm{LT}\right\rangle\right|\lesssim400~\textrm{s},\left|\left\langle\Delta\delta\tau_\textrm{p}^{Q_2}\right\rangle\right|\lesssim10^3~\textrm{s}$, depending on the other orbital parameters and the initialepoch. For the propagation delays, we have$\left|\delta\tau_\textrm{prop}^\textrm{LT}\right|\lesssim0.02~\textrm{s},~\left|\delta\tau_\textrm{prop}^{Q_2}\right|\lesssim1~\mu\textrm{s}$. The expected precision in pulsar timing in Sgr A$^\ast$ is ofthe order of $100~\mu\textrm{s}$, or, perhaps, even $1-10~\mu\textrm{s}$.

Post-Keplerian perturbations of the orbital time shift in binary pulsars: an analytical formulation with applications to the Galactic Center