The main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. Stars spend the majority of their lifetimes in this phase, where they are fusing hydrogen into helium in their cores.
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Stars on the main sequence are in hydrostatic equilibrium, balancing gravitational forces with pressure from nuclear fusion reactions.
The position of a star on the main sequence is primarily determined by its mass.
Main sequence stars can range from about 0.1 to 100 times the mass of our Sun.
The Sun is an example of a main sequence star, specifically classified as a G-type star.
As stars exhaust their hydrogen fuel, they leave the main sequence and evolve into red giants or other types of stars.
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H–R Diagram: A graphical tool that plots stars according to their luminosity and temperature, revealing patterns like the main sequence.