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[[File:The_Mysterious_Case_of_the_Disappearing_Dust.jpg|The Mysterious Case of the Disappearing Dust|thumb]] '''Formation and Evolution of the Solar System'''

The '''formation and evolution of the Solar System''' began approximately 4.6 billion years ago with the gravitational collapse of a small part of a giant molecular cloud. Most of the collapsing mass collected in the center, forming the [[Sun]], while the rest flattened into a protoplanetary disk out of which the [[planets]], [[moons]], [[asteroids]], and other [[solar system]] bodies formed.

==Formation==
The process of the Solar System formation is theorized to have begun with the gravitational collapse of a fragment of a giant molecular cloud. The cloud was composed primarily of [[hydrogen]], [[helium]], and small amounts of heavier elements forged by previous generations of stars. As the region that would become the Solar System, known as the pre-solar nebula, collapsed, it began to spin faster and flattened into a disk. This is known as the [[nebular hypothesis]], first proposed in its modern form by [[Kant]] and [[Laplace]] in the 18th century.

Within this disk, small particles of dust and ice began to stick together in a process known as accretion, forming clumps that eventually became planetesimals. Through further collisions and accretion, these planetesimals grew into the proto-planets. Over time, gravitational interactions and collisions shaped the nascent planets and their orbits, leading to the formation of a relatively stable Solar System.

==Evolution==
The early Solar System was a turbulent place, and its evolution was marked by frequent collisions. One significant theory suggests that a Mars-sized body, sometimes referred to as [[Theia]], collided with the early [[Earth]], leading to the formation of the [[Moon]].

Over billions of years, the planets have undergone significant changes. The inner, rocky planets, including [[Earth]], [[Mars]], [[Venus]], and [[Mercury]], cooled down, with some developing atmospheres through volcanic outgassing. The outer gas giants, such as [[Jupiter]] and [[Saturn]], grew massive enough to capture large atmospheres of hydrogen and helium. The ice giants, [[Uranus]] and [[Neptune]], accumulated their mass in the colder outer regions of the Solar System.

The [[asteroid belt]], located between Mars and Jupiter, and the [[Kuiper belt]], beyond Neptune, are remnants of the early Solar System, containing many small bodies that never coalesced into planets. The [[Oort Cloud]], a theoretical cloud of icy objects far beyond Neptune, is thought to be the source of long-period [[comets]] that visit the inner Solar System.

==Current Understanding and Future Studies==
Our understanding of the formation and evolution of the Solar System has been significantly advanced by space missions, such as the [[Voyager]] probes, the [[Galileo]] spacecraft, and the [[Cassini]] probe, as well as observations from telescopes like the [[Hubble Space Telescope]]. Future missions and advances in technology promise to further our knowledge, potentially revising our theories as new data becomes available.

==See Also==
* [[Exoplanet]]
* [[Nebular hypothesis]]
* [[Planetary differentiation]]
* [[Solar nebula]]

[[Category:Astronomy]]
[[Category:Solar System]]
[[Category:Planetary science]]

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Formation and evolution of the Solar System - Revision history

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