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Higher temperatures imply higher concentrations of atmospheric water vapour, while lower temperatures suggest lower atmospheric levels. Since the early formation of the hydrosphere, the amount of water vapour in the atmosphere has been regulated by the temperature of Earth’s surface-hence its radiation balance. This low rate can be readily explained: the very cold temperatures of the upper atmosphere result in a cold trap at an altitude of about 15 km (about 9.3 miles), where most of the water vapour condenses and returns to lower altitudes, thereby escaping photodissociation. Only about 4.8 × 10 −4 cubic km (about 0.0005 cubic mile) of water vapour is presently destroyed each year by photodissociation. The hydrogen is lost to space and the oxygen remains behind. Water loss in the upper atmosphere is by photodissociation, the breakup of water vapour molecules into hydrogen and oxygen due to the energy of ultraviolet light. Gains would be from continuous degassing of Earth the present degassing rate of juvenile water has been determined as being only 0.3 cubic km (about 0.07 cubic mile) per year. It is likely that the hydrosphere attained its present volume early in Earth’s history, and since that time there have been only small losses and gains. Whether most of the degassing took place during core formation or shortly thereafter or whether there has been significant degassing of Earth’s interior throughout geologic time remains uncertain. A large cool Earth most certainly served as a better trap for water than a small hot body because the lower the temperature, the less likelihood for water vapour to escape, and the larger the planetary mass, the stronger its gravitational attraction for water vapour. Once the planet’s surface had cooled sufficiently, water contained in the minerals of the accreted material and released at depth could escape to the surface and, instead of being lost to space, cooled and condensed to form the initial hydrosphere. Other scientists claim that most of Earth’s water came from chemical reactions within the planet’s interior. Both of these celestial objects have been shown to contain ice. Some scientists argue that much of the water on the planet was delivered by comet and meteor impacts.
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It is likely that core formation resulted in the escape of an original primitive atmosphere and its replacement by one derived from the loss of volatile substances from the planetary interior ( see evolution of the atmosphere).Īt an early stage, Earth thus did not have water or water vapour at its surface, and the topic of how water arrived on Earth’s surface is a matter of substantial debate. It has been concluded that Earth’s core formed over a period of about 500 million years. Heating of this initially cool, unsorted conglomerate by the decay of radioactive elements and the conversion of kinetic and potential energy to heat resulted in the development of Earth’s liquid iron core and the gross internal zonation of the planet (i.e., differentiation into core, mantle, and crust). Some of these particles had compositions similar to that of carbonaceous chondrite meteorites, which may contain up to 20 percent water. This gaseous matter condensed into small particles that coalesced to form a protoplanet, which in turn grew by the gravitational attraction of more particulates.
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