SUMMARY
Gamma rays generated in the Sun's core are converted into visible light photons through a series of scattering processes, primarily Compton scattering and bremsstrahlung. As gamma rays scatter off free electrons and heavier ions, their energy decreases, resulting in the production of lower energy photons. This conversion occurs repeatedly until thermal equilibrium is achieved between the photon gas and the electron gas. The temperature of the photon gas decreases from the core to the photosphere, reaching approximately 5000 K near the surface, where the peak photon energy falls within the visible spectrum.
PREREQUISITES
- Understanding of Compton scattering
- Knowledge of bremsstrahlung radiation
- Familiarity with thermal equilibrium concepts
- Basic principles of photon energy and temperature relationships
NEXT STEPS
- Research Compton scattering in detail
- Explore bremsstrahlung radiation mechanisms
- Study thermal equilibrium in astrophysical contexts
- Investigate the temperature dependence of photon energy distributions
USEFUL FOR
Astronomers, physicists, and students studying astrophysics or thermodynamics, particularly those interested in stellar processes and radiation transfer mechanisms.