Final answer:
The triple-α process is a nuclear fusion reaction where three helium nuclei combine to form a carbon nucleus at high temperatures and pressures in stellar cores, releasing substantial energy. This process occurs during the later stages of a star's life, allowing the star to continue to produce energy after exhausting its hydrogen fuel.
Step-by-step explanation:
The mass of helium-4 (^4He) is 4.0026032497 u, and we can use this data along with the mass of hydrogen to compute the energy produced during nuclear fusion in stars. When hydrogen is converted into helium, mass is lost and energy is produced, following Einstein's mass-energy equivalence principle. In stellar cores, when the temperature and pressure are sufficiently high, helium nuclei (alpha particles) undergo the triple-α process to form carbon.
The triple-α process involves three alpha particles (helium nuclei) combining to form a carbon nucleus. This process only occurs at extremely high temperatures and pressures and is crucial in stars heavier than the sun. The energy released during the conversion of helium to carbon is significant, providing a further source of energy once the hydrogen fusion phase in the star's life has ended.
With the triple-α process, stars can continue to shine despite the exhaustion of their hydrogen fuel. The balance of the star's structure and its subsequent fate is dependent upon the star's mass and the accumulation of heavier elements through nucleosynthesis.