Stellar evolution
Lesson 6 / 7
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I can describe life cycles of stars and the variations that depend on the mass of a star.
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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.
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