During the formation of the solar system, gravity played a crucial role in the collapse of a rotating cloud of gas and dust, called the solar nebula. As about 99% of the material in this cloud gathered toward the center, it formed a dense region that eventually became the Sun. Meanwhile, the remaining material in the flattened disc surrounding the central mass began to coalesce into various celestial bodies.
The process led to the creation of:
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The Sun: The central mass where the majority of the gas and dust was concentrated. As the material fell inward and the pressure increased, nuclear fusion ignited, marking the birth of the Sun.
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Planets: The remaining material in the disc began to clump together through the process of accretion, forming planetesimals that eventually coalesced into the planets we see today—such as Earth, Mars, Jupiter, and Saturn.
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Dwarf Planets: Some smaller bodies formed the basis of what we now recognize as dwarf planets, such as Pluto and Eris.
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Moons: Many of the planets captured material or formed their own moons through similar accretion processes.
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Asteroids and Comets: Not all material coalesced into planets; some remained as smaller bodies like asteroids in the asteroid belt and comets that inhabit the outer regions of the solar system.
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Other Small Bodies: The formation of small celestial bodies and debris, including meteoroids and other interplanetary objects.
This process laid the groundwork for the complex system of planets, moons, and other celestial entities present in our solar system today. It was a turbulent period, marked by collisions and the gradual clearing of the residual material to form a stable solar system.
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