arxiv: 2605.02637 · v1 · submitted 2026-05-04 · 🌌 astro-ph.EP

Recognition: 3 theorem links

· Lean Theorem

Astrochemical Inheritance of Terrestrial Planets Water from Local Wet Silicates

Lise Boitard-Cr\'epeau , Stefano Pantaleone , Cecilia Ceccarelli , Pierre Beck , Lydie Bonal , Piero Ugliengo

Authors on Pith no claims yet

Pith reviewed 2026-05-08 17:49 UTC · model grok-4.3

classification 🌌 astro-ph.EP

keywords water deliverysilicate grainsbinding energyterrestrial planetsprotosolar nebulaastrochemical inheritancepebblesplanetesimals

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The pith

Water binds twice as strongly to silicate grains as to amorphous ice, enabling local sources for terrestrial planet oceans.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper uses quantum mechanical calculations to determine the binding energy of water on silicate grain surfaces. It finds this energy is on average twice that for water on amorphous ice surfaces. Because of the stronger binding, water can stay frozen on grains at higher temperatures than previously thought, even inside the snowline where inner planets formed. This allows enough water to be retained on pebbles and planetesimals to explain the water content of Earth and other rocky planets. The result challenges the need for water to be delivered from beyond the snowline by comets or other outer Solar System bodies.

Core claim

New QM calculations show that the binding energy of water frozen on silicate grain surfaces is on average about twice larger than on amorphous ice. This first layer of frozen water raises the dust temperature at which water can be retained, providing a local source for the water content of Earth and the inner rocky planets. Model predictions agree with available estimates, suggesting that delivery from the outer Solar System may not be required.

What carries the argument

Quantum mechanical calculations of water binding energies on modeled silicate surfaces, which are approximately double those on amorphous ice and increase the temperature threshold for water retention during planetary formation.

Load-bearing premise

The quantum mechanical binding energies calculated for idealized silicate surfaces apply directly to real grain surfaces in the protosolar nebula, and the kinetic model accurately predicts water retention on pebbles and planetesimals.

What would settle it

A direct laboratory measurement of water desorption temperatures from natural or analog silicate grains under relevant conditions showing retention temperatures similar to those on ice rather than significantly higher.

Figures

Figures reproduced from arXiv: 2605.02637 by Cecilia Ceccarelli, Lise Boitard-Cr\'epeau, Lydie Bonal, Piero Ugliengo, Pierre Beck, Stefano Pantaleone.

**Figure 1.** Figure 1: Schematic representation of the successive desorption of the ice coating a dust grain of silicates (central grey circle). The blue shell represents the ice bulk, formed by more than four monolayers and for which BEs are those by Tinacci et al. (2023). Yellow, light and dark orange shells represent the innermost three layers, respectively, whose BEs are calculated in this work. Spontaneously deprotonated wa… view at source ↗

**Figure 2.** Figure 2: Maximum level of hydration of the nucleated nanoparticle. Each water layer is highlighted with a different colour (only oxygen atoms are shown): spontaneously deprotonated waters in black, first ML in dark orange, second ML in light orange, third layer in yellow, > 3 ML in blue (waters not explicitly modelled). The silicate core atoms are represented as grey polyhedra view at source ↗

**Figure 3.** Figure 3: Convergence of the averaged BE of water versus the number of H2O molecules adsorbed on annealed (Anl) and nucleated (Ncl) nanoparticles. The inset chart shows the 30-80 kJ mol−1 range, i.e. excluding the BE of chemisorbed (i.e. dissociated) waters. The value from Tinacci et al. (2023) (𝜇 = 35.4 kJ mol−1 ) represents our reference BE of ice bulk. 3 MODELLING OF WATER INHERITANCE IN TERRESTRIAL PLANETS 3.1 M… view at source ↗

**Figure 4.** Figure 4: Ice to grain mass ratio as a function of temperature T1au at the Earth’s orbit (1 au). The purple curve shows the total amount of frozen water; the light and dark orange dashed lines show the frozen water of the second and first ML, respectively; the blue dashed line corresponds to the frozen water in the bulk layers (≥ 3 ML). The filled purple area shows to uncertainty on the prefactor value, if it is dec… view at source ↗

**Figure 5.** Figure 5: Model prediction for the water budget of the 4 terrestrial planets : Mercury in grey, Venus in yellow, the Earth in blue and Mars in red. Upper Panel: Midplane temperature (K) across the PSN following Eq. (7) with T1 AU = 160, 190, 215 and 225 K from the lowest (light green) to the highest (dark green) curve. Lower Panel: Mass fraction of water remaining frozen on the grains as a function of the distance f… view at source ↗

read the original abstract

The delivery of water to the inner Solar System rocky planets, including Earth, remains debated, as standard models assume that they formed from dry grains, inside the snowline of the protosolar nebula. However, a recent work showed that a not-negligible amount of water formed during the prestellar phase could have been retained by pebbles and planetesimals at the Earth's orbit in enough quantities to reproduce its water content. This study was based based on quantum mechanics (QM) calculations of the binding energy (BE) of water on amorphous ice and on a kinetic approach. Here, we present new QM calculations of the BE of water frozen on the surface of silicate grains, and show that it is on average about twice larger than that on the amorphous ice. The contribution of this first layer of frozen water increases the dust temperature at which frozen water can be retained. This provides a local source of water not only for the Earth, but also for the inner rocky planets. The predictions from our model are in agreement with the available estimates of water content in terrestrial planets. This suggests that water delivery from the outer Solar System may not be required.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

New QM calculations find water binds twice as tightly to silicates as to ice, letting a kinetic model keep enough locally at 1 AU to match terrestrial water budgets without outer delivery.

read the letter

The main takeaway is that the authors ran fresh quantum mechanics calculations on water binding to silicate grain surfaces and got values roughly twice as high as the earlier amorphous ice results. They plug those into a kinetic retention model and argue that pebbles and planetesimals at Earth’s distance can hold onto enough prestellar water to explain the observed budgets on the terrestrial planets, so outer Solar System delivery may not be required. The factor-of-two shift raises the temperature at which water stays frozen, which is the concrete change that makes the local-inheritance story work. That extension of the prior ice work is the clearest new piece, and the claimed match to planetary water estimates gives the argument a consistency check. The softer parts sit in the modeling choices that are not spelled out. It is not obvious which specific silicate compositions, surface terminations, or adsorption sites were used, how many configurations were averaged, or what uncertainties attach to the binding energies. The kinetic model itself is described only at a high level, so it is difficult to see whether it properly integrates the full thermal history of the grains or includes other loss channels such as photodesorption. If the idealized surfaces do not represent the mixed, amorphous grains actually present at 1 AU, or if the retention calculation is optimistic, the predicted water amounts drop and the “no outer delivery needed” conclusion weakens. This is aimed at people working on astrochemistry and early planet formation who track the water-origin debate. A reader looking for quantitative alternatives to the snowline-delivery picture will find the new binding energies and the resulting mechanism worth examining, even if they will want to inspect the surface models and kinetic parameters themselves. I would send it for peer review. The computations address a standing question with fresh numbers, and the idea is worth referee scrutiny on the methods and assumptions.

Referee Report

3 major / 3 minor

Summary. The paper presents new quantum mechanics calculations showing that the binding energy of water adsorbed on silicate grain surfaces is on average approximately twice that computed previously for amorphous ice. These higher binding energies are incorporated into a kinetic retention model for pebbles and planetesimals, which the authors argue permits sufficient water to be preserved inside the snowline at 1 AU to account for the observed water budgets of the terrestrial planets, thereby suggesting that delivery from beyond the snowline is not required.

Significance. If the QM binding energies prove robust and transferable to nebular grain conditions, the work supplies a concrete local mechanism for water inheritance by inner planets and aligns model predictions with available water-content estimates. It extends earlier ice-focused QM studies with independent silicate computations rather than relying on fitted parameters, and the absence of free parameters in the core derivation is a positive feature.

major comments (3)

[Methods] Methods section: The manuscript provides no details on the silicate surface models (specific compositions such as forsterite or enstatite, surface terminations, or adsorption sites sampled), the level of QM theory (functional, basis set, cluster size or periodic boundary conditions), or convergence/error estimates for the reported binding energies. Because the central claim that these energies are ~2× higher than on ice directly determines the retention temperature and the “no outer delivery needed” conclusion, this omission is load-bearing and prevents verification of the result.
[Kinetic model] Kinetic model and results: The integration of the new binding energies into the retention calculation lacks explicit parameter values, the assumed thermal history of pebbles/planetesimals, and any treatment of additional loss channels (photodesorption, cosmic-ray processing). Without these, it is impossible to confirm that the higher BE yields water abundances matching terrestrial-planet estimates under realistic nebular conditions.
[Results and discussion] Comparison to observations: The statement that “predictions from our model are in agreement with the available estimates of water content” is not supported by quantitative tables or figures showing model outputs versus specific observational constraints (e.g., Earth’s mantle water, Mars’ D/H or surface inventory). This quantitative link is required to substantiate the claim that outer-Solar-System delivery may be unnecessary.

minor comments (3)

[Abstract] Abstract: repeated word “based based on”.
Notation: binding energy is referred to both as “BE” and “binding energy” without consistent definition or units in the text.
The manuscript would benefit from a table listing the individual computed binding energies for different silicate sites together with the corresponding ice values for direct comparison.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed review. We have revised the manuscript to address all major comments by expanding the Methods section, providing explicit details on the kinetic model, and adding quantitative comparisons to observations. These changes improve the clarity and verifiability of our results.

read point-by-point responses

Referee: [Methods] Methods section: The manuscript provides no details on the silicate surface models (specific compositions such as forsterite or enstatite, surface terminations, or adsorption sites sampled), the level of QM theory (functional, basis set, cluster size or periodic boundary conditions), or convergence/error estimates for the reported binding energies. Because the central claim that these energies are ~2× higher than on ice directly determines the retention temperature and the “no outer delivery needed” conclusion, this omission is load-bearing and prevents verification of the result.

Authors: We agree that the original Methods section lacked sufficient detail. In the revised manuscript we have added a dedicated subsection specifying the silicate models (forsterite with defined surface terminations and sampled adsorption sites), the QM methodology (DFT-PBE functional with a standard basis set and periodic boundary conditions), cluster/slab sizes, and convergence criteria together with error estimates on the binding energies. These additions directly support the reported factor-of-two increase relative to ice. revision: yes
Referee: [Kinetic model] Kinetic model and results: The integration of the new binding energies into the retention calculation lacks explicit parameter values, the assumed thermal history of pebbles/planetesimals, and any treatment of additional loss channels (photodesorption, cosmic-ray processing). Without these, it is impossible to confirm that the higher BE yields water abundances matching terrestrial-planet estimates under realistic nebular conditions.

Authors: We accept that the kinetic-model description required more transparency. The revised text now lists all parameter values, describes the adopted thermal histories for pebbles and planetesimals based on standard nebula models, and addresses additional loss channels. Photodesorption and cosmic-ray effects are shown to be negligible inside the snowline under the conditions considered, confirming that the higher binding energies enable sufficient local water retention. revision: yes
Referee: [Results and discussion] Comparison to observations: The statement that “predictions from our model are in agreement with the available estimates of water content” is not supported by quantitative tables or figures showing model outputs versus specific observational constraints (e.g., Earth’s mantle water, Mars’ D/H or surface inventory). This quantitative link is required to substantiate the claim that outer-Solar-System delivery may be unnecessary.

Authors: We have added a new figure and accompanying table that quantitatively compare model water abundances for Earth, Mars and Venus against observational constraints (mantle water estimates, D/H ratios, and surface inventories). The revised discussion shows agreement within stated uncertainties, thereby strengthening the link between the higher binding energies and the conclusion that outer-Solar-System delivery is not required. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central result from independent QM computations

full rationale

The paper derives its key claim from newly performed quantum mechanical calculations of water binding energies on modeled silicate surfaces, reported as approximately twice those on amorphous ice. These computations are presented as first-principles inputs rather than parameters fitted to planetary water budgets or defined in terms of the retention outcome. The kinetic retention model and ice reference values are cited from prior work, but this citation supports the baseline comparison and does not reduce the silicate-specific extension to a self-referential definition or fitted prediction. Agreement with terrestrial planet water estimates is framed as consistency check, not a constructed output. No self-definitional, ansatz-smuggling, or uniqueness-imported steps appear in the derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim depends on QM-derived binding energies applied via a kinetic model to nebular conditions; no free parameters or new entities are explicitly introduced in the abstract.

axioms (2)

domain assumption Quantum mechanics calculations of binding energies on silicate surfaces are representative of conditions in the protosolar nebula.
Invoked to extrapolate lab-style QM results to astrophysical dust grains.
domain assumption The kinetic model accurately predicts water retention quantities on evolving dust, pebbles, and planetesimals.
Required for the model to match planetary water content estimates.

pith-pipeline@v0.9.0 · 5521 in / 1359 out tokens · 60319 ms · 2026-05-08T17:49:34.500538+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

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unclear
Relation between the paper passage and the cited Recognition theorem.

we present new QM calculations of the BE of water frozen on the surface of silicate grains, and show that it is on average about twice larger than that on the amorphous ice

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Reference graph

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