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GCSE Physics · key term
The long, stable stage of a star’s life during which hydrogen nuclei fuse into helium in its core.
Used by AQA, Edexcel and OCR
Specification 4.8.1.1, 4.8.1.2 · Paper 2
A stable stage of a star’s life in which fusion supplies energy and the star is in equilibrium.
Revise: Our solar systemThe Sun became a stable main-sequence star when fusion was established and these opposing effects reached equilibrium.
A stable stage of a star's life during which hydrogen nuclei fuse in its core.
Specification 7.16P, 7.18P · Paper 1
The long, stable stage of a star’s life during which hydrogen nuclei fuse to form helium in its core.
A stable star in which energy released by nuclear fusion provides an outward effect that balances gravitational contraction.
Specification P8.3c · Paper 2 (Foundation), Paper 4 (Higher)
Revise: Lifecycle of a starIn a stable main-sequence star, this outward effect balances the inward pull of gravity. This is an equilibrium: the Sun neither collapses under gravity nor expands without limit. Fusion also supplies the energy that the Sun radiates into space.
Use the exact order required by the specification: nebula → main-sequence star → red giant → white dwarf.
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