The current generation of observatories has confirmed that ultra-high-energy cosmic rays are not composed solely of protons. In particular, analyses of the distributions of shower-maximum depths have revealed an increasing trend in the mass composition of particles with energies above approximately $2 \: \rm EeV$. Given that photodisintegration is the primary interaction for nuclei heavier than protons propagating through intergalactic space, accurately modeling this process is essential for uncovering their astrophysical origins. To address this need, we present revisions to the Monte Carlo propagation code SimProp, emphasizing the implementation of photodisintegration interactions in its upcoming version: SimProp Sirente. Using the latest results from TALYS, a software for nuclear reaction simulations, we compared the total inelastic cross sections with those from one of the current models in SimProp, focusing not only on the cross sections themselves but also on their impact on the energy loss length of the particles. Moreover, we began testing the single-nucleon emission approximation to predict the outgoing nucleus after the interaction occurs, assessing the code's performance in this context and identifying potential improvements in the Sirente version for future applications, such as in-source interactions.