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Water Delivery by Pebble Accretion to Rocky Planets in Habitable Zones in Evolving Disks by Shigeru Ida; Takeru Yamamura; Satoshi Okuzumi is a Physics and Astronomy article available to read on EtoBox.

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__Context.__The ocean mass of the Earth is only 2.3 × 10^−4^of the whole planet mass. Even including water in the interior, the water fraction would be at most 10^−3^−10^−2^. Ancient Mars may have had a similar or slightly smaller water fraction. What controlled the amount of water in these planets has not been clear, although several models have been proposed. It is important to clarify the control mechanism to discuss water delivery to rocky planets in habitable zones in exoplanetary systems, as well as that to Earth and Mars in our solar system. __Aims.__We consider water delivery to planets by icy pebbles after the snowline inwardly passes planetary orbits. We derive the water mass fraction (__f__~water~) of the final planet as a function of disk parameters and discuss the parameters that reproduce a small value of__f__~water~comparable to that inferred for the Earth and ancient Mars. __Methods.__We calculated the growth of icy dust grains to pebbles and the pebble radial drift with a 1D model, by simultaneously solving the snowline migration and dissipation of a gas disk. With the obtained pebble mass flux, we calculated accretion of icy pebbles onto planets after the snowline

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Author

Shigeru Ida; Takeru Yamamura; Satoshi Okuzumi

Publisher

EDP Sciences (ISSN 0004-6361)

Published

2019

Language

EN

Field

Physics and Astronomy (Physical Sciences)