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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 longest stage of stellar evolution is the main sequence phase.
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.
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.
There is no known role of magnetism in stellar evolution.
Scientist believe that stellar evolution contained only hydrogen and then helium.
The endpoints of stellar evolution are: White Dwarf Neutron Star Black Hole The endpoint is dependent upon birth mass of the star.
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Stellar temperature can be measured by analysing the spectrum of light that stars emit; shorter wavelengths correspond to higher temperatures.