Energy is liberated through fusion reactions, producing heavier and heavier elements. There are two transient elements heavier than iron which are produced by standard stellar nucleosynthesis, but these are short lived and decay into lighter elements. Iron is the heaviest element forged in the heart of a star via standard stellar evolution.
All elements heavier than iron are the byproduct of a supernova, wherein atomic nuclei are smashed together with such force energy is consumed in the nuclear reaction. This is why there tends to be an abundance of stable isotopes as light as iron, but elements heavier than iron are much more rare. Lead is an exception to this general rule as it is the end product of a long radioisotope decay sequence.
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.
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.
Main Sequence
it is the cycle of stellar evolution
Gravity effects stellar evolution by pulling down force on the stars while they are forming. Mass will determine how long the star stays alive and burning.