The main sequence is a continuous and distinctive band of stars that appears on the Hertzsprung-Russell diagram, where stars spend the majority of their lifetime fusing hydrogen into helium in their cores. This phase represents a critical stage in stellar evolution, as it is during this time that a star achieves stability, balancing the inward pull of gravity with the outward pressure from nuclear fusion. The main sequence includes stars of various masses and temperatures, providing insights into their life cycles and eventual transformations.
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