What Happens to Low Mass Stars (< 8 solar masses)?
STAGE 1: Main Sequence
A star's life begins when nuclear reactions start deep in the core. Hydrogen nuclei are fused to form a helium nucleus. Each helium nucleus has slightly less mass than the hydrogen nuclei that formed it. The missing mass is converted into energy. This energy released in the core creates high temperatures and pressures. The high internal pressure would blow the star apart if not for the weight of the outer layers pressing down upon the core.
When a star joins the main sequence, that means it has stabilized. It is no longer being compressed by gravity or blown apart by the intense temperatures and pressures in the core. The two are in perfect balance. And as long as the fuel supply holds out, this balance is maintained. The star spends almost all of its life on the main sequence as a very average star.