Origin of Earth's Water: Delivery by Planetary Embryos or Local Adsorption from Primordial Nebula?

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The origin of Earth's water is one of the most outstanding unanswered questions in planetary science. It is generally believed that the Earth’s local environment during its formation was sufficiently hot to prevent the hydration of planetesimals and protoplanets. That is, the Earth’s nearby building blocks were likely devoid of water and water must have been delivered to Earth from large distances. The two paradigms for the delivery of water, namely, the cometary impacts and delivery through planetesimals and planetary embryos have their own uncertainties. The measured values of the D/H ratio in some comets are approximately twice the terrestrial value which may preclude comets as a source of Earth’s water. Also, the Os isotopes in Earth’s mantle play against water delivery by means of planetesimals and protoplanets. A third scenario suggests that Earth might have formed wet and its water could have its origin in the water vapor that was adsorbed on dust grains (which later contributed to its formation) in the primordial nebula. We have carried out extensive simulations of the formation of Earth in a disk where the distribution of water follows the adsorbtion model. Results of our simulations indicate that, when compared with the current value of Earth’s water budget, the scenario of the wet formation of Earth introduces too much water to the inner part of the solar system. However, when this scenario is limited to a small region and is combined with the model based on the delivery of water through planetesimals and planetary embryos, the accumulated amount of water on Earth will become more realistic. In other words, a more viable scenario for the origin of Earth’s water seems to be a combination of these two models. We present the results of our study and discuss their implications for water on terrestrial planets.

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