Cosmic-gamma-ray emission at low-luminosity from CCO 1E 1207.4-5209 and its Host SNR G296.5+10.0

The origin and acceleration mechanisms of energetic particles in the universe remain enigmatic in contemporary astrophysics. Recent efforts have focused on identifying Galactic sources capable of accelerating particles to 1 PeV, known as PeVatrons, and also identifying sources contributing to the spectrum at lower energies. The different morphology of galactic supernova remnants is directly related to the type of stellar explosion and the existence of a possible Compact Central Object (CCO), which possess intense radiative-gravitational fields on their surfaces. These CCOs, due to their strong fields and interactions with surrounding magnetic clouds, are potential candidates for gamma ray production. Through observations of the compact X-ray source 1E 1207.4-5209, located near the remnant G296.5+10.0, and using the enhanced GALPROP code, we analyze the emission of gamma-ray and cosmic-ray production through propagation. Additionally, we calculate the contribution of the G296.5+10.0 source to the overall observed Galactic cosmic-ray flux, taking into account cosmic-ray propagation within the Galaxy, which includes energy losses and particle interactions. Our findings suggest that this setup offers a fertile environment for producing a wide range of cosmic-ray energies at low energy within the Galaxy.