Origin of the world's oceans

There are thought to have been two primary sources for the primordial water that formed Earth's oceans, with debate as to their relative importance. One is out gassing of steam from the Earth's interior, which contributed to the atmosphere and, once the young planet had sufficiently cooled, produced rain; the other is the large numbers of comets which impacted with the Earth and added their water to it.
The origin of water on Earth, in particular the question of why there is clearly more water on the Earth than on the other planets of the solar system has, until today, not been clarified. There are various popular theories as to how the world's oceans were formed over the past 4.6 billion years. Some of the most likely contributing factors to the origin of the Earth's oceans are as follows:

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The cooling of hot gases were released causing "out gassing", potentially bringing water to Earth.
Comets, trans-Neptunian objects or water-rich asteroids (protoplanets) from the outer reaches of the asteroid belt colliding with a pre-historic Earth may have brought water to the world's oceans. Measurements of the ratio of the Hydrogen isotopes Deuterium and Protium point to asteroids, since similar percentage impurities in carbon-rich chondrites were found to oceanic water, whereas previous measurement of the isotopes’ concentrations in comets and trans-Neptunian objects correspond only slightly to water on the earth.
Liquid may have been "locked" in the Earth's rocks and leaked out over millions of years.
Photolysis. (Radiation can break down chemical bonds separating liquid from hard mass)
Rain and sandstorms may have pooled.
It is likely that more than one of these factors contributed to the vast oceans, covering more than 70% of the Earth's surface that we have today.

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When the earth was at the planetesimal stage, there was probably already water present. This water and other lightweight, fluid constituents such as Carbon Dioxide (CO2), Methane (CH4) and Nitrogen (N2) originated mostly from eruptions or out gassings of the primal earth and formed a young, water-vapor free primal earth atmosphere. These were, according to present models and simulations, carried away by the solar wind that at the time of the formation of the Earth was much stronger than today, and so escaped the Earth. Later through volcanism came the creation of a newer atmosphere, which may also have contained water-vapor released from the earth’s interior. With the development of a solid earth’s crust and further cooling down, the water vapor condensed and hence formed the first oceans.

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The large amount of water that is present on the Earth in comparison to other earth-like bodies cannot be alone explained by that released from the earth’s interior. The planetesimals formed in a period of the early Solar system, when there was relatively little water around. The closer to the sun one was, the higher the temperature and the less water present. First outside the solar ‘snow line’, which lay roughly where the Asteroid belt is today, water could be found in considerable abundance. Coal-rich chondrites, which it is generally agreed formed in the outer reaches of the asteroid belt, indicate a water content of sometimes more than 10% of their weight, whereas common condrites or enstatite condrites from the nearer regions of the asteroid belt comprise less than 0.1% of their weight in water.. Moreover it can be supposed that during the accretion of the planetesimals into planets and the loss of the primitive atmosphere would result in the larger proportion of the originally present water being lost. Hence it is in many cases assumed that the majority of the water present on the Earth today came from the outer regions of the Solar System.

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