Larger stars burn through their hydrogen fuel more rapidly, leading to shorter lifespans. The amount of time a star spends in the main sequence stage depends on its mass. This reaction releases a tremendous amount of energy in the form of light and heat, causing the star to shine. The energy radiated by stars comes from nuclear fusion, a process in which hydrogen atoms combine to form helium. ![]() _ The Fuel of the Cosmos: Nuclear Fusion Nuclear Fusion This state of hydrostatic equilibrium allows stars to shine brightly for millions or even billions of years. During this stage, stars maintain a delicate balance between the gravitational forces pulling them inward and the pressure from nuclear fusion pushing outward. Once a protostar has amassed enough mass, nuclear fusion begins in its core, marking the birth of a main sequence star. _ Main Sequence Stars: The Prime of Stellar Life A Delicate Balance: Hydrostatic Equilibrium As these embryonic stars accumulate more mass, the pressure and temperature at their cores increase, setting the stage for nuclear fusion. Protostars are not yet stars, but they’re well on their way. The Gravitational Dance: Protostars Emerge ProtostarsĪs gravity pulls the gas and dust in a nebula closer together, dense regions known as protostars begin to form.
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