Origin and Early Evolution of Terrestrial Planet Atmospheres and Oceans
作者: 刘玲根 ：中央研究院地球科学研究所，台湾 台北;
Abstract: For as long as the terrestrial planets (Mercury, Venus, Earth, Moon and Mars) were accreted from planetesimals containing some carbonates and hydrous minerals, the majority of the materials that form today’s terrestrial planet atmospheres and oceans should be inherent. An amount of H2O that is roughly equivalent to today’s Earth oceans should be buried inside Venus, Earth and Mars during the early stage of accretion. After accretion, the proto-atmospheres of Venus, Earth and Mars likely consisted of more than 95% CO2 which are probably kept by both Venus and Mars till today. The fate of the Earth, on the other hand, had been changed by the Moon-forming giant impact. After the giant impact, the Earth gained its Moon and released most of its H2O contents into the CO2 proto-atmosphere. At such temperature and pressure conditions, H2O and CO2 would form a supercritical H2O-CO2 fluid which would later precipitate to yield the indigenous oceans when Earth’s surface temperature cooled down to 450˚C - 300˚C. The hot indigenous ocean reacted with feldspars, the most abundant surface minerals, to form carbonates, thus removing all CO2 from Earth’s proto-atmosphere eventually. The gravity force of Mars is too small to hold gaseous H2O in its atmosphere, but this does not necessarily imply that Mars’ interior or its surface materials do not contain H2O.
文章引用: 刘玲根 (2017) 内行星大气海洋的成因和初期演化。 天文与天体物理， 5， 45-51. doi: 10.12677/AAS.2017.54006
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