Stellar evolution states that stars are powered by a hydrogen fusion reaction. When a star has burned up its hydrogen, this reaction runs out, and its core will contract and heat up causing the hydrogen shell to ignite. This causes the star to expand into a giant star. Depending on the solar mass of the star, it will evolve into different objects. If its mass is in the 0.3 to 3 range, its core, now fusing helium will degenerate before the helium has a chance to ignite, and the explosion that results will be absorbed into the star itself. A star with a mass less than 0.4 will evolve into a white dwarf. If its mass is between 0.4 and 0.3, it will become a red giant and then burn out into a white dwarf. Stars that are more massive will collapse explosively as a super nova, and if it is larger than 25 stellar masses, it will be a neutron star.
phase plane in stellar structure
The longest stage of stellar evolution is the main sequence phase.
Main Sequence
Our Sun is currently on the Main Sequence stage of it's evolution.
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The first stage of stellar evolution is nebula.
You can find an overview of stelar evolution in the Wikipedia article entitled "Stellar evolution".
The main sequence stage is a point in the stellar evolution of stars in the universe at which every star converts hydrogen into helium in its cores and releases huge amounts of energy.
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Helium burning is most durable stage in stellar evolution.
Stellar evolution is the term for the changes a star undergoes during its lifetime.
Nuclear fusion affects stellar evolution by essentially halting all mitosis and miosis that any cells in a stellar evolution could experience, and they stunt the growth of the object.
Star clusters are collections of same-age stars that remain intact for billions of years. When plotted on a H-R diagram, a cutoff point of stars leaving the main sequence and massive stars further evolved are shown, confirming the theory of stellar evolution.