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Protoplanets are celestial bodies that form in the early stages of planetary system development. They are the precursors to fully formed planets and are typically found in protoplanetary disks, which are accumulations of gas, dust, and ice surrounding young stars. Protoplanets are believed to form through a process called accretion, where small dust particles collide and stick together, gradually growing larger over time.

The formation of protoplanets is a complex process that involves several stages. Initially, small dust grains in the protoplanetary disk collide and stick together, forming larger aggregates known as planetesimals. These planetesimals continue to grow through further collisions and accretion, eventually reaching sizes on the order of kilometers. At this point, they are often referred to as protoplanets.

Protoplanets can be classified into two main types based on their composition: rocky protoplanets and icy protoplanets. Rocky protoplanets are composed primarily of silicate minerals and metals, similar to the composition of Earth. Icy protoplanets, on the other hand, are rich in volatile compounds such as water, ammonia, and methane, and are often found in the outer regions of protoplanetary disks.

The study of protoplanets is crucial for understanding the formation and evolution of planetary systems. By observing protoplanetary disks and the protoplanets within them, astronomers can gain insights into the processes that shape planetary systems and the conditions necessary for the emergence of life. Protoplanets also play a significant role in the dynamics of planetary systems, influencing the orbits and interactions of other celestial bodies.