Speaker
Description
Cosmic rays are an important non-thermal component of active galac
tic 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 mecha
nisms in quasars and Low-Ionization Nuclear Emission-line Regions (LIN
ERs). We focus on photopion production, proton-proton collisions, mag
netic diffusion, and synchrotron cooling processes. In quasar environ
ments, intense radiation fields and strong magnetic activity enhance rel
ativistic particle energy losses through photopion interactions and syn
chrotron emission. In contrast, the weaker radiation and magnetic envi
ronments of LINERs may allow cosmic rays to survive for longer timescales
and contribute more effectively to sustained cosmic-ray pressure. Us
ing characteristic physical parameters from both AGN classes, we discuss
how environmental differences influence cosmic-ray evolution and pres
sure behavior. Our results suggest that quasars experience more efficient
cosmic-ray energy dissipation, while LINERs provide comparatively stable
conditions for cosmic-ray confinement.