Water in the Early Earth

Marty, Bernard; Yokochi, Reika

doi:10.2138/rmg.2006.62.18

Cited by 86 publications

(46 citation statements)

References 148 publications

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“…Current models of the origin of water on Earth usually assume that hydrogen was contained in the chondritic material from which Earth accreted, with a possible contribution from icy objects that formed beyond the snow line in the outer solar system and were later scattered inward (Morbidelli et al, 2000;Marty and Yokochi, 2006;Rubie et al, 2011;Marty, 2012). Such models necessarily imply that planets formed close to the sun are relatively dry, compared to those formed at larger heliocentric distances.…”

Section: Discussionmentioning

confidence: 99%

Molecular hydrogen in mantle minerals

Yang¹,

Keppler²,

Li³

2016

Geochem. Persp. Let.

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doi: 10.7185/geochemlet.1616Current models assume that hydrogen was delivered to Earth already in oxidised form as water or OH groups in minerals; similarly, it is generally believed that hydrogen is stored in the present mantle mostly as OH. Here we show by experiments at 2-7 GPa and 1100-1300 °C that, under reducing conditions, molecular hydrogen (H 2 ) has an appreciable solubility in various upper mantle minerals. This observation suggests that during the accretion of the Earth, nebular H 2 could have been delivered to the growing solid planet by direct dissolution in a magma ocean and subsequent incorporation in silicates. Moreover, the presence of dissolved molecular H 2 in the minerals of the lower mantle could explain why magmas sourced in this region are rich in hydrogen, despite the fact that lower mantle minerals contain almost no OH groups.

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Section: Discussionmentioning

confidence: 99%

Molecular hydrogen in mantle minerals

Yang¹,

Keppler²,

Li³

2016

Geochem. Persp. Let.

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“…That is, distinctly, in contradiction with clear observational evidence both from within our Solar System and from extrasolar planetary systems (Marty & Yokochi 2006;Klein et al 2011). The fundamental problem is that rocky material is not particularly sticky.…”

Section: Introductionmentioning

confidence: 75%

Making Terrestrial Planets: High Temperatures, FU Orionis Outbursts, Earth, and Planetary System Architectures

Hubbard

2017

ApJL

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Current protoplanetary dust coagulation theory does not predict dry silicate planetesimals, in tension with the Earth. While remedies to this predicament have been proposed, they have generally failed numerical studies, or are in tension with the Earth's (low, volatility dependent) volatile and moderately volatile elemental abundances. Expanding on the work of Boley et al. (2014), we examine the implications of molten grain collisions and find that they may provide a solution to the dry silicate planetesimal problem. Further, the source of the heating, be it the hot inner disk or an FU Orionis scale accretion event, would dictate the location of the resulting planetesimals, potentially controlling subsequent planetary system architectures. We hypothesize that systems which did undergo FU Orionis scale accretion events host planetary systems similar to our own, while ones that did not instead host very close in, tightly packed planets such as seen by Kepler.

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“…Deciphering the delivery and origin of water on Earth therefore involves detailed understanding of planetary evolution, which is essentially an identical problem to the origin of terrestrial atmosphere. Further discussion on the origin of water on Earth can be found in Morbidelli et al (2000), Dauphas et al (2000), Abe et al (2000), Drake (2005), Marty and Yokochi (2006), and Mottl et al (2007).…”

Section: Overviewmentioning

confidence: 99%

Warm Season Flows

2015

Encyclopedia of Astrobiology

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Water in the Early Earth

Cited by 86 publications

References 148 publications

Molecular hydrogen in mantle minerals

Molecular hydrogen in mantle minerals

Making Terrestrial Planets: High Temperatures, FU Orionis Outbursts, Earth, and Planetary System Architectures

Warm Season Flows

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