Main-Sequence Burning

Main-sequence burning is a fundamental process in stellar evolution, serving as the stable phase of hydrogen fusion that powers the majority of stars in the universe. This crucial stage occurs when a star settles into equilibrium, balancing the inward force of gravity with the outward pressure of nuclear fusion. Through this delicate balance, stars like our sun sustain their luminosity and stability for billions of years. Understanding main-sequence burning is pivotal in comprehending the life cycles of stars, from their formation in nebulae to the eventual transitions into different phases, shedding light on the intricate workings of the cosmos.