Preliminary Results in Dynamical Simulations of Water Origins for Earth-Like Planets

• Autor(a) principal: Souza Torres, K. de
• Data de Publicação: 2009
• Outros Autores: Winter, O. C. [UNESP], Meech, K. J., Keane, J. V., Mumma, M. J., Siefert, J. L., Werthimer, D. J.
• Tipo de documento: Artigo de conferência
• Idioma: eng
• Título da fonte: Repositório Institucional da UNESP
• Texto Completo: http://hdl.handle.net/11449/197400

In its gaseous and solid forms, water is present in the most distant galaxies, among the stars, in the Sun, in its planets and their satellites and ring systems, and in comets. In its liquid form, it has played an essential part in the appearance, development and maintenance of terrestrial life. The origin of water on Earth remains one of the most important subjects of debate and controversy in solar system formation science. Possible sources of water can be divided into endogenous and exogenous. The most accepted endogenous source is the direct absorption of water from gas onto grains in the accretion disk, and the exogenous one is that the bulk of the Earth's water may have come from the asteroid belt in the form of planetary embryos with up to 10% of water. However, none of them alone is enough to explain Earth's water as a whole. In the present work, we use dynamical simulations of planetary formation and water delivery to investigate the implications of both of the main composition theories using chemical constraints like D/H ratio as discriminator. The goal is to understand how terrestrial planets got their water in the solar system and expand it to extrasolar systems. From the results we can conclude that the composition model with both main theories better explains the D/H ratio of Earth's water. Future work will add a cometary component in the water quantity and D/H ratio of terrestrial planets.