Nuclear fusion in the sun occurs when hydrogen nuclei (protons) collide at extremely high temperatures and pressures, overcoming their electrostatic repulsion. This fusion process primarily converts hydrogen into helium, releasing a tremendous amount of energy in the form of light and heat. The energy produced supports the sun's luminosity and drives its stability, allowing it to shine for billions of years. This reaction occurs in the sun's core, where conditions are optimal for fusion to take place.
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