Water delivery in the inner solar nebula

Monte Carlo simulations of forsterite hydration

¹ Zernike Institute for Advanced Materials, University of Groningen, PO Box 221 9700 AE Groningen, The Netherlands
e-mail: dangelomartinka@gmail.com
² Kapteyn Astronomical Institute, University of Groningen, PO Box 800 9747 AV Groningen, The Netherlands
e-mail: kamp@astro.rug.nl
³ Faculty of Aerospace Engineering, Delft University of Technology, Delft, The Netherlands
⁴ University of Leiden, PO Box 9513 2300 RA Leiden, The Netherlands
⁵ Max Planck Institute for Extraterrestrial Physics, Gießenbachstrasse 1, 85741 Garching, Germany
⁶ SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, UK

Received: 25 June 2018
Accepted: 2 September 2018

Abstract

Context. Endogenous or exogenous, dry or wet, various scenarios have been depicted for the origin of water on the rocky bodies in our solar system. Hydrated silicates found in meteorites and in interplanetary dust particles, together with observations of abundant water reservoirs in the habitable zone of protoplanetary disks, are evidence that support aqueous alteration of silicate dust grains by water vapor condensation in a nebular setting.

Aims. We investigate the thermodynamics (temperature and pressure dependencies) and kinetics (adsorption rates and energies, surface diffusion and cluster formation) of water adsorption on surfaces of forsterite grains, constraining the location in the solar nebula where aqueous alteration of silicates by water vapor adsorption can occur efficiently and leads to the formation of phyllosilicates. We analyze the astrophysical conditions favorable for such hydration mechanism and the implications for water on solid bodies.

Methods. The protoplanetary disk model (ProDiMo) code is tuned to simulate the thermochemical disk structure of the early solar nebula at three evolutionary stages. Pressure, temperature, and water vapor abundance within 1 au of the protosun were extracted and used as input for a Monte Carlo code to model water associative adsorption using adsorption energies that resemble the forsterite [1 0 0] crystal lattice.

Results. Hydration of forsterite surfaces by water vapor adsorption could have occurred within the nebula lifetime already at a density of 10⁸ cm⁻³, with increasing surface coverage for higher water vapor densities. Full surface coverage is attained for temperatures lower than 500 K, while for hotter grain surfaces water cluster formation plays a crucial role. Between 0.5 and 10 Earth oceans can arise from the agglomeration of hydrated 0.1 μm grains into an Earth-sized planet. However, if grain growth occurs dry and water vapor processes the grains afterward, this value can decrease by two orders of magnitude.

Conclusions. This work shows that water cluster formation enhances the water surface coverage and enables a stable water layer to form at high temperature and low water vapor density conditions. Finally, surface diffusion of physisorbed water molecules shortens the timescale for reaching steady state, enabling phyllosilicate formation within the solar nebula timescale.