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The formation of the solar system

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The planet, a well as the other extraterrestrial objects like asteroids, ws formed in the flat plane of the whirling disc of dust. Bth electrostatic forces and sticky carbon coatings made particles of dust stick together forming clusters, wich eventually stuck together forming rocks. Mtual gravity made these rocks come together, utimately to form planets in a process called accretion. Dring and after the Terrestrial planets were formed, tere was a cataclysmic bombardment by the remains of rocky planetesimals that cratered these planets’ surfaces. Te impacting material, tgether radioactivity as well as consequent gravitational concentration, gnerated adequate heat to melt as well as chemically separate the planets into three layers (crust, mntle, ad core) as per Holton et al.

Te Terrestrial planets’ atmospheres were created in this process and subsequently by outgassing from hot interiors of planets as well as from the impacting material. Btween Mars and Jupiter, i the asteroid belt, te solar nebula temperature was lower so that water and carbon-rich minerals could unite in the forming of planetesimals. Fom Jupiter outward, tmperatures were much large amounts of frozen water accumulate with the rocky matter in the planetesimals.

A colder temperatures, oher ices formed, lke methane and ammonia, gving those far-away planetesimals a mixed composition of ammonia, wter, a well as methane ice saturated with a small quantity of rocky matter (Karttunen et al. Acording to Solar Nebula Hypothesis, rcky planets formed in the centre of the protoplanetary disk where the temperatures were very high to prevent condensation of ice, wter and other materials into grains. Tis resulted in the coagulation of only grains later on into the creation of rocky planetesimals.

Fllowing small planetesimals formation, rnaway accretion began. Gowth hastens as mass builds up leading to the growth of bigger bodies by the destruction of minor bodies. Tis lasted approximately 10,000 to 100,000 years and ended when the biggest bodies exceeded about 1,000 km in diameter. Nxt, oigarch accretion started. Mny hundred of the largest bodies called oligarchs continued to accrete planetesimals. Tey grew impacting each other and forming a bigger body. Te outcome of the oligarchic phase was the of. ..

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