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The origin and acceleration mechanisms of energetic particles in the universeremain enigmatic in contemporary astrophysics. Recent efforts have focused onidentifying Galactic sources capable of accelerating particles to 1 PeV, knownas PeVatrons. The different morphology of galactic supernova remnants isdirectly related to the type of stellar explosion and the existence of apossible Compact Central Object (CCO), which possess intenseradiative-gravitational fields on their surfaces. These CCOs, due to theirstrong fields and interactions with surrounding magnetic clouds, are potentialcandidates for cosmic ray production. Through observations of the compact X-raysource 1E 1207.4-5209, located near the remnant G296.5+10.0, and using theenhanced GALPROP code, we analyze the emission of high-energy gamma rays (E >100 GeV) resulting from cosmic-ray acceleration and propagation. Additionally,we calculate the contribution of this association to the overall observedGalactic cosmic-ray flux, considering cosmic-ray propagation within the Galaxy,including energy losses and particle interactions. Our findings suggest thatthis setup offers a fertile environment for the production of a wide range ofcosmic-ray energies, ranging from GeV to TeV, and even extending up to PeV,within the Galaxy

Gamma-Ray emission from CCO 1E 1207.4-5209 and its host SNR G296.5+10.0