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The Earth's First 1billion Years | Sutori

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The Earth's First 1billion Years

Earth's Puberty before humans

Planetary Accretion

Formation of the Earth and the other terrestrial planets of our Solar System (Mercury, Venus and Mars) commenced 4.567 billion years ago and occurred on a time scale of about 100 million years. These planets grew by the process of accretion, which involved numerous collisions with smaller (Moon- to Mars-size) bodies. The energy of such collisions caused large-scale melting and the formation of deep “magma oceans”. Such magma oceans enabled liquid metal to separate from liquid silicate, sink and accumulate to form the metallic cores of the planets. Thus core formation in terrestrial planets was a multistage process, intimately related to major collisions during accretion, which determined the resulting chemistry of planetary mantles. The aim of this interdisciplinary ERC project is to integrate astrophysical models of planetary accretion with geochemical models of planetary differentiation, with cosmochemical constraints also being provided by meteorites. The research will involve integrating new models of planetary accretion with core formation models based on the partitioning of elements between liquid metal and liquid silicate that we will determine experimentally at pressures up to about 100 gigapascals (equivalent to 2400 km deep in the Earth). By comparing our results with the known physical and chemical characteristics of the terrestrial planets, we will obtain a comprehensive understanding of how these planets formed, grew and evolved, both physically and chemically, with time.

Outer Core Formation

The outer core of the Earth is a fluid layer about 2,300 km (1,400 mi) thick and composed of iron and nickel that lies above Earth's solid inner core and below its mantle. Its outer boundary lies 2,890 km (1,800 mi) beneath Earth's surface. The transition between the inner core and outer core is located approximately 5,150 km (3,200 mi) beneath the Earth's surface.

 Formation of the Moon

The giant-impact hypothesis, sometimes called the Big Splash, or the Theia Impact suggests that Earth's Moon formed out of the debris left over from an indirect collision between Earth and an astronomical body the size of Mars, approximately 4.5 billion years ago, in the Hadean eon; about 20 to 100 million years after the solar system coalesced.

Planetary Cooling

A planetary body, whether the body is a planet or a moon, has to cool off. The warmth contained inside a body controls what sort of surface activity, atmospheric activity, and interior activity which the body has. As planetary bodies cool slowly, heat diminishes, and the activities diminish to nothing. Examination of a body for various kinds of activities tells scientists what stage a body is in it's history of cooling off.

End of Heavy Bombardment

About 4 to 3.8 billion years ago a period of intense comet and asteroid bombardment is thought to have peppered all the planets including the Earth. Many of the numerous Craters found on the Moon and other bodies in the Solar System record this event.

● Planetary Accretion

● Planetary Cooling

● Outer Core Formation

● Formation of the Moon

● End of Heavy Bombardment