Planetary Formation

Planetary formation is the process by which planets develop from a protoplanetary disk composed of gas, dust, and other materials surrounding a young star. This process involves several stages, beginning with the gravitational collapse of the disk, leading to the accumulation of solid particles into larger bodies called planetesimals. These planetesimals collide and coalesce, forming protoplanets, which may eventually become full-fledged planets.

The formation process is influenced by various factors, including the chemical composition of the material in the disk, the distance from the central star, and the dynamics of the disk itself. Theories of planetary formation include the core accretion model, where solid cores form first and then attract surrounding gas, and the gravitational instability model, where regions of the disk collapse directly into giant planets.

Overall, planetary formation is a critical aspect of astrophysics and helps explain the diversity of planetary systems observed in the universe today.