By Y. Ryabov, G. Yankovsky
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4 The Formation of the Earth 29 The thin, newly formed Earth’s crust, consisting of light silicates, swam on the surface of the sea of magma. It was often broken apart by collision with planetesimals of various sizes. The formation of the crust was a complex process, many details of which are as yet not understood. This admission points to the fact that we do not have much geological evidence from this early phase of the Earth’s formation. A vital event in the further development of the Earth was its collision with a smaller planet, possibly as big as Mars.
Sulphobes are spherical in form, with a diameter between 1 and 100 μm, and can interact with their surroundings; thus they can adsorb dyestuffs. In some ways, they resemble the coacervates studied by Oparin and his school (Sect. 2). Another type of experiment on chemical evolution was due first to Groth and Suess and later to Garrison. They studied the type of energy which must be applied to a simulated primeval atmosphere in order to form organic building blocks for biomolecules, starting from inorganic materials.
Apart from their cores, these planets have a similar composition to that of the sun. Between the planets Mars and Jupiter, there is a large zone which should really contain another planet. It 26 2 The Cosmos, the Solar System and the Primeval Earth seems clear that the huge mass of Jupiter prevented the formation of a planet from the planetesimals, which already had diameters measured in kilometres. Thus, in this part of the solar system, we find only asteroids orbiting the sun. It has been estimated that the asteroid belt contains around 50,000 objects, only about 10% of which have so far been identified; asteroids can measure up to 900 km in diameter.