With recent improvements in observational techniques, the orientation of the rotational spin-axis of an exoplanet has been constrained (e.g., 2MASS J01225093–2439505 favors a misaligned planetary spin-axis as shown by Bryan et al. 2020). It remains unclear, however, how the spin states of planets are excited during the formation of planetary systems. In this presentation, I will demonstrate the feasibility of high obliquity excitation of planetary bodies via secular spin-orbit resonances under the influence of the protoplanetary disk. Specifically, I will show how the disk profile of the circumstellar and circumplanetary disks affect the spin evolution; and also characterize the effects due to a satellite. Understanding the efficiency in the enhancement of spin-inclination and its dependence on various disk and planet properties will also constrain the formation processes of planets in disks.