Welcome to Solar System! In this event, participants will demonstrate their knowledge of planet formation and structure within and beyond the Solar System.

Solar System

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The Formation Process Study Guide

Solar Nebula: The process begins with a giant rotating cloud of gas and dust known as the solar nebula. This nebula collapses under its own gravity, leading to the formation of a protostar at its center, which eventually becomes a star.

Protoplanetary Disk: As the protostar forms, the remaining material flattens into a rotating disk around it. This disk is composed of tiny particles, including ice, rock, and metal, which are the building blocks of planets.

Accretion of Planetesimals: Within this disk, particles collide and stick together, forming larger bodies called planetesimals. These planetesimals can range from small pebbles to larger objects several kilometers in diameter. Over time, they continue to collide and merge, growing larger through a process known as accretion.

Formation of Protoplanets: As planetesimals grow, they begin to clear their orbits of debris, becoming protoplanets. The gravitational pull of these larger bodies attracts more material, allowing them to grow even further. In the colder outer regions of the disk, icy planetesimals can form the cores of gas giants.

Differentiation and Final Stages: Eventually, the protoplanets undergo differentiation, where heavier materials sink to the center, forming a core, while lighter materials form the outer layers. This process leads to the formation of distinct planetary bodies, including rocky planets like Earth and gas giants like Jupiter and Saturn.

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