Stars form from clouds of dust and gas.
Gravitational forces make the clouds become increasingly dense, forming a 'Protostar'.
As a Protostar becomes denser, it gets hotter. If it becomes hot enough, the nuclei of hydrogen atoms start to fuse together.
Stars radiate energy because of the hydrogen fusion in the core. This is the main stage in the life of a star. It can continue for billions of years until the star runs out of hydrogen nuclei to fuse together.
The inward force of gravity is balanced by the outward pressure of radiation from the core, so the star is stable. During this stable period the star is called a 'main sequence star'.
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