Cosmic rays are an important non-thermal component of active galactic nuclei (AGN) and may contribute significantly to the pressure balance and energy transport within galactic nuclei. The efficiency of cosmic-ray confinement and survival strongly depends on the surrounding plasma conditions, radiation fields, particle densities, and magnetic environments. In this study, we compare the dominant cosmic-ray energy loss mechanisms in quasars and Low-Ionization Nuclear Emission-line Regions (LIN ERs). We focus on photopion production, proton-proton collisions, magnetic diffusion, and synchrotron cooling processes. In quasar environments, intense radiation fields and strong magnetic activity enhance relativistic particle energy losses through photopion interactions and synchrotron emission. In contrast, the weaker radiation and magnetic environments of LINERs mayallow cosmic rays to survive for longer timescales and contribute more effectively to sustained cosmic-ray pressure. Using characteristic physical parameters from both AGN classes, we discuss how environmental differences influence cosmic-ray evolution and pressure behavior. Our results suggest that quasars experience more efficient cosmic-ray energy dissipation, while LINERs provide comparatively stable conditions for cosmic-ray confinement.