Fully describes the formation of the solar system including the words; gravity, accretion and condensation
The formation of the solar system is believed to have started around 4.6 billion years ago from a massive rotating cloud of gas and dust known as the solar nebula. Gravity played a crucial role in this process, pulling together the material within the nebula and causing it to collapse under its own weight.
As the solar nebula collapsed, it started to spin faster, causing it to flatten into a spinning disk. The central region of this disk began to heat up and form the protosun, which eventually became the Sun. Meanwhile, the remaining material in the disk began to cool and condense.
Accretion is the process by which small particles stick together and gradually grow larger due to mutual collisions. Within the disk, dust particles started to collide and stick together, eventually forming planetesimals. These planetesimals continued to collide and merge, building up mass over time.
As the planetesimals grew larger, their increased gravity allowed them to attract even more material, including gas from the solar nebula. This gas accumulation led to the formation of giant gas planets such as Jupiter and Saturn, which grew to become the largest bodies in the solar system.
Within the inner region of the disk, where it was hotter, only rocky and metallic materials could condense. These condensed particles eventually formed terrestrial planets like Earth, Mars, Venus, and Mercury. These planets are primarily composed of rock and metal.
As the system continued to evolve, the solar wind from the Sun blew away much of the remaining gas and dust in the disk. This marked the end of the formation process and left behind the planets, moons, asteroids, comets, and other objects that constitute our solar system today.
In summary, the formation of the solar system was driven by gravity, which caused the collapse of the solar nebula. Accretion and condensation then took place, leading to the formation of planets through the accumulation of material and the growth of protoplanetary disks.