Estimates of excess volatile substances released from Earth’s interior is given in the table.

Earth’s initial accretion by the agglomeration of solid particles occurred about 4.56 billion years ago. 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 a liquid iron core and the gross internal zonation of Earth. It has been concluded that formation of Earth’s core took about 500 million years. It is likely that core formation resulted in the escape of an original primitive atmosphere and its replacement by one derived from loss of volatile substances from Earth’s interior. Whether most of this degassing took place during core formation or soon afterward or whether there has been significant degassing of Earth’s interior throughout geologic time is uncertain. Recent models of Earth formation, however, suggest early differentiation of Earth into three major zones (core, mantle, and crust) and attendant early loss of volatile substances from the interior. It is also likely that Earth, after initial cold agglomeration, reached temperatures such that the whole Earth approached the molten state. As the planet’s initial crust solidified, volatile gases would be released to form an atmosphere that would contain water, later to become the hydrosphere; carbon gases, such as carbon dioxide, methane, and carbon monoxide; sulfur gases, mostly hydrogen sulfide; and halogen compounds, such as hydrochloric acid. Nitrogen also may have been present, along with minor amounts of other gases. Gases of low atomic number, such as hydrogen and helium, would escape Earth’s gravitational field. Substances degassed from the planetary interior have been called excess volatiles because their masses cannot be accounted for simply by rock weathering.

At an initial crustal temperature of about 600 °C (about 1,100 °F), almost all these compounds, including water (H₂O), would be in the atmosphere. The sequence of events that occurred as the crust cooled is difficult to construct. Below 100 °C (212 °F) all the H₂O would have condensed, and the acid gases would have reacted with the original igneous crustal minerals to form sediments and an initial ocean. There are at least two possible pathways by which these initial steps could have been accomplished.

One pathway assumes that the 600 °C atmosphere contained, together with other compounds, water (as vapour), carbon dioxide, and hydrochloric acid in the ratio of 20:3:1 and would cool to the critical temperature of water. The water vapour therefore would have condensed into an early hot ocean. At this stage, the hydrochloric acid would be dissolved in the seawater of the period (about 1 mole per litre), but most of the carbon dioxide would still be in the atmosphere with about 0.5 mole per litre in the ocean water. This early acid ocean would react vigorously with crustal minerals, dissolving out silica and cations and creating a residue that consisted principally of aluminous clay minerals that would form the sediments of the early ocean basins. This pathway of reaction assumes that reaction rates were slow relative to cooling.

A second pathway of reaction, which assumes that cooling was slow, is also possible. In this case, at a temperature of about 400 °C (about 750 °F) most of the water vapour would be removed from the atmosphere by hydration reactions with pyroxenes and olivines. Under these conditions, water vapour would not condense until some unknown temperature was reached, and Earth might have had at an early stage in its history an atmosphere rich in carbon dioxide and no ocean: the surface would have been much like that of present-day Venus.

The pathways described are two of several possibilities for the early surface environment of the planet. In either case, after Earth’s surface had cooled to 100 °C, it would have taken only a short time geologically for the acid gases to be used up in reactions involving minerals from igneous rock. The presence of bacteria and possibly algae in the fossil record of rocks older than three billion years attests to the fact that Earth’s surface had cooled to temperatures lower than 100 °C by this time and that the neutralization of the original acid gases had taken place. If most of the degassing of primary volatile substances from Earth’s interior occurred early, the chloride released by reaction of hydrochloric acid with rock minerals would be found in the oceans and seas or in evaporite deposits, and the oceans would have a salinity and volume comparable to those that they have today.

This conclusion is based on the assumption that there has been no drastic change in the ratios of volatiles released through geologic time. The overall generalized reaction indicative of the chemistry leading to formation of the early oceans can be written in the form: primary igneous rock minerals + acid volatiles + H₂O = sedimentary rocks + oceans + atmosphere. Notice from this equation that if all the acid volatiles and H₂O were released early in Earth’s history and in the proportions found today, then the total original sedimentary rock mass produced would be equal to that of the present time, and ocean salinity and volume would be near what they are now. If, on the other hand, degassing were linear with time, then the sedimentary rock mass would have accumulated at a linear rate, as would oceanic volume. However, the salinity of seawater would remain nearly the same if the ratios of volatiles degassed did not change with time. The most likely situation is that presented here—namely, that major degassing occurred early in Earth’s history, after which minor amounts of volatiles were released episodically or continuously for the remainder of geologic time. The salt content of seawater in the oceans based on the constant proportions of volatiles released would depend primarily on the ratio of sodium chloride (NaCl) locked up in evaporites to that dissolved in the oceans. If all the sodium chloride in evaporites were added to seawater today, the salinity would be roughly doubled. This value gives a sense of the maximum salinity the oceans could have attained throughout geologic time.

One component missing from the early terrestrial surface was free oxygen, because it would not have been a constituent released from the cooling crust. As noted earlier, early production of oxygen was by photodissociation of water in the atmosphere as a result of absorption of ultraviolet light. The reaction is 2H₂O + hν = O₂ + 2H₂, in which hν represents a photon of ultraviolet light. The hydrogen produced would escape into space, and the O₂ would react with the early reduced gases by reactions such as 2H₂S + 3O₂ = 2SO₂ + 2H₂O. Oxygen production by photodissociation gave the early reduced atmosphere a start toward present-day conditions, but it was not until the appearance of photosynthetic organisms approximately 3.3 billion years ago that it was possible for the accumulation of oxygen in the atmosphere to proceed at a rate sufficient to lead to today’s oxygenated environment. The photosynthetic reaction leading to oxygen production may be written 6CO₂ + 6H₂O + hν = C₆H₁₂O₆ + 6O₂, in which C₆H₁₂O₆ represents sugar.