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The stars twinkling in the night sky are distant suns, giant balls of burning hot gas, primarily consisting of:
Hydrogen: This is the most abundant element in the universe, making up about 70% of a star’s mass for most stars like our Sun. Hydrogen fuel powers the star through a process called nuclear fusion.
Helium: The second most abundant element, helium is a byproduct of nuclear fusion and makes up about 28% of a star’s mass.
Trace Elements: Stars also contain smaller amounts of other elements like oxygen, carbon, nitrogen, and iron. These trace elements typically make up about 2% of a star’s mass but are crucial for various stellar processes and the formation of heavier elements later in a star’s life cycle.
Here’s a breakdown of how these elements come together in a star:
Formation: Stars are born from giant clouds of gas and dust in space. Gravity pulls these clouds inward, causing them to heat up and spin faster.
Nuclear Fusion: As the pressure and temperature at the star’s core become immense, hydrogen atoms fuse together to form helium in a process called nuclear fusion. This releases tremendous energy, which radiates outward as light and heat, making the star shine.
Stellar Evolution: Throughout its life, a star’s composition and structure change as it burns its fuel and evolves. The heavier elements play a role in these later stages, and some stars can even create even heavier elements before exploding in a supernova.