Stellar evolution
I can describe life cycles of stars and the variations that depend on the mass of a star.
Stellar evolution
I can describe life cycles of stars and the variations that depend on the mass of a star.
These resources will be removed by end of Summer Term 2025.
Lesson details
Key learning points
- Radiation pressure from nuclear fusion pushes out from the centre of a star.
- Gravitational force pulls in towards the centre of a star.
- When a star is in balance, forces from radiation pressure are equal in size to gravitational forces.
- A main sequence star is a star in balance for millions of years, until it no can longer fuse hydrogen nuclei.
- After all available hydrogen has been fused, gravity contracts a star raising temperature until other nuclei can fuse.
Keywords
Main sequence star - a star which is fusing hydrogen in its core; these stars are stable for long periods of time
Red giant star - a larger, cooler, star formed after hydrogen in the core has been depleted
White dwarf star - the white hot core of a star after its outer layers have escaped into space
Supernova - an exploding star, caused by a gravitational collapse after the fuel is exhausted
Neutron star - an incredibly dense star, formed after a supernova
Common misconception
Stars just exist and do not change over time.
Explain the cause and effect of changes in stars and support pupils in explaining these ideas in their own words.
Licence
This content is © Oak National Academy Limited (2024), licensed on Open Government Licence version 3.0 except where otherwise stated. See Oak's terms & conditions (Collection 2).
Lesson video
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