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Stellar evolution

Stellar evolution

Date: 04 March 2018
Copyright: ESA

Artist's impression of some possible evolutionary pathways for stars of different initial masses.

Some proto-stars, brown dwarfs, never actually get hot enough to ignite into fully-fledged stars, and simply cool off and fade away.

Red dwarfs, the most common type of star, keep burning until they have transformed all their hydrogen into helium, turning into a white dwarf.

Sun-like stars swell into red giants before puffing away their outer shells into a colourful nebula while their cores collapse into a white dwarf.

The most massive stars collapse abruptly once they have burned through their fuel, triggering a supernova explosion or gamma-ray burst, and leaving behind a neutron star or black hole.

Last Update: 1 September 2019
24-Feb-2024 12:54 UT

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