Protoplanetary disks are structures of gas and dust that surround a newly formed star. These disks are critical in the process of planet formation, as the material within them gradually coalesces to form planets, moons, asteroids, and other celestial bodies. Typically observed in the early stages of stellar development, protoplanetary disks reflect the initial conditions of the solar system and other planetary systems across the universe.
The disks are composed mainly of hydrogen, helium, and heavier elements, and their dynamics can be influenced by factors such as gravity, temperature, and magnetic fields. As the material in the disk spirals inward toward the star, it can form various structures, including gaps and rings, due to the gravitational interactions between the forming planets and the surrounding material.
Research into protoplanetary disks enhances our understanding of the origins of planetary systems and the evolutionary processes that govern them. Observations of these disks, especially in different wavelengths of light, provide astronomers with key insights into the disk’s composition, structure, and the nature of the planets that may form within them.