E.5.2—Fusion in stars
- Syllabus
- First assessment 2025
- Objective
- —
- Level
- SL
Use fusion as a stellar source
In stellar fusion, light nuclei combine to form more tightly bound nuclei. The mass difference is released as energy, which powers the star and supports its pressure balance.
E_{\text{released}}=B_{\text{products}}-B_{\text{reactants}}=\Delta mc^2
Worked example — deuterium–tritium fusion
For 2H+3H→4He+n, the binding energies are 2(1.11)=2.22MeV, 3(2.83)=8.49MeV and 4(7.07)=28.28MeV. Therefore E=28.28−2.22−8.49=17.57MeV. The product is more tightly bound, so energy is released.
Follow nucleosynthesis
Fusion in stars can build elements up to iron through successive reactions. Elements heavier than iron are mainly formed in explosive environments and neutron-capture processes rather than ordinary core fusion.
Compare fusion and fission
Fusion can offer high energy per mass and potentially fewer long-lived waste products, but it requires extreme temperature and confinement conditions.
Common trap
Do not say all heavy elements are made by fusion in ordinary stars. The pathway changes around iron.
Questions compare fusion with fission or outline how elements heavier than hydrogen and helium formed.
Outline / State
Mention stellar nucleosynthesis/fusion for elements up to iron, then supernova or neutron capture for heavier elements.
Claiming fusion alone forms every element or ignoring the comparison condition in an advantage question.
Retrieve stellar balance
Fusion releases energy, outward thermal/radiation pressure balances inward gravity, and high temperature and density allow fusion in the core.
Retrieve stellar inference
Mass controls evolution; HR regions classify stars; parallax gives distance; and L=4πR2σT4 gives stellar radius from luminosity and temperature.