SOLAR SYSTEM

Detailed explanation-1: -Clumps of interstellar matter left behind in the midplane of the solar disk as it contracted toward its centre gradually coalesced, through a process of accretion, to form grains, pebbles, boulders, and then planetesimals measuring a few kilometres to several hundred kilometres across.

Detailed explanation-2: -The disk is initially very hot and cools later in what are known as the “T Tauri Star (TTS)” stage by possible formation of small dust grains made of rocks and ices. The grains may eventually coagulate into kilometer-sized planetesimals.

Detailed explanation-3: -The Sun formed in the center, and the planets formed in a thin disk orbiting around it. In a similar manner, moons formed orbiting the gas giant planets. Comets condensed in the outer solar system, and many of them were thrown out to great distances by close gravitational encounters with the giant planets.

Detailed explanation-4: -Accretion disk: The matter around the center spins up and flattens into a disk, while heat vaporizes the dust. Protostar: Forms in the center, when the core becomes opaque; later will become the Sun.

Detailed explanation-5: -In astrophysics, accretion is the accumulation of particles into a massive object by gravitationally attracting more matter, typically gaseous matter, in an accretion disk. Most astronomical objects, such as galaxies, stars, and planets, are formed by accretion processes.