How was the solar system formed? Please explain.

The formation of the solar system is a complex process that occurred approximately 4.6 billion years ago. The most widely accepted theory for the formation of the solar system is the nebular hypothesis, which can be explained in several key steps:

Formation of the Solar Nebula:

• The process began with the gravitational collapse of a large molecular cloud composed mostly of hydrogen and helium, as well as traces of heavier elements.
• This collapse led to the formation of a spinning, flattened disk of gas and dust known as the solar nebula.

Formation of the Protostar:

• Within the center of the solar nebula, a concentration of material began to accumulate, forming a protostar—a hot and dense core surrounded by a swirling disk of gas and dust.

Accretion of Planetesimals:

• Small particles in the disk, called planetesimals, started to collide and stick together due to mutual gravitational attraction.
• These collisions and accretion processes led to the formation of larger bodies called protoplanets.

Differentiation and Formation of the Sun:

• In the center of the solar nebula, the protostar continued to grow and accumulate mass, undergoing nuclear fusion in its core.
• The Sun was formed as a result of these processes, becoming the central and dominant body in the solar system.

Formation of Planets:

• The remaining material in the disk began to clump together to form the planets. This process, known as accretion, involved the collision and merger of protoplanets and planetesimals.
• Near the Sun, where it was hotter, only rocky materials could condense, forming the terrestrial planets (like Earth). Farther out, where it was colder, ices could also condense, contributing to the formation of gas giants (like Jupiter and Saturn).