Stars form in dense regions of molecular clouds, where gravity causes gas and dust to collapse into a protostar. Once nuclear fusion ignites in the core, a star enters its main sequence phase, burning hydrogen into helium. Over time, as hydrogen depletes, the star evolves based on its mass. Low-mass stars become red giants and eventually white dwarfs, while massive stars undergo supernova explosions, leaving behind neutron stars or black holes. Studying stellar life cycles provides insights into the universe's structure and element formation.
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Stars form from clouds of gas and dust in space, called nebulae, which collapse under gravity to create a dense core. This core heats up, igniting nuclear fusion, where hydrogen atoms combine to form helium, releasing energy. Over time, stars evolve based on their mass, becoming red giants or supergiants. Low-mass stars end as white dwarfs, while massive stars may explode as supernovae, leaving behind neutron stars or black holes. This life cycle recycles elements, contributing to cosmic evolution.
Stars form from clouds of gas and dust, primarily composed of hydrogen, that collapse under gravity, leading to nuclear fusion in the core, which marks the birth of a star. During its life, a star fuses hydrogen into helium, releasing energy in the process, and this balance of fusion and gravitational forces keeps the star stable. As the star exhausts its hydrogen fuel, it begins fusing heavier elements, causing it to expand into a red giant or supergiant. Eventually, the star's fate depends on its mass: low to medium-mass stars shed their outer layers and become white dwarfs, while massive stars explode in a supernova, leaving behind either a neutron star or a black hole. The death of a star plays a key role in enriching the universe with heavy elements, essential for the formation of planets and life.