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Monosilane Worlds: Sub-Neptunes with Atmospheres Shaped by Reduced Magma Oceans

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Pith's one-line read Water dissolved in magma lets monosilane persist in sub-Neptune skies

desk verdict H2O dissolution into reduced magma oceans flips the predicted SiH4 abundance in sub-Neptune atmospheres; the effect is real, but the 0.1–10% persistence claim rides on an SiO-rainout assumption the authors themselves flag. read the letter →

arxiv 2505.03200 v1 pith:SLVH7V7S submitted 2025-05-06 astro-ph.EP

Yuichi Ito , Tadahiro Kimura , Kazumasa Ohno , Yuka Fujii , Masahiro Ikoma This is my paper · ORCID
classification astro-ph.EP
keywords sub-NeptunesmagmaoceansmonosilaneSiH4chemicalequilibriumatmosphericchemistrywaterdissolutionhydrogen-dominatedatmospheres
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that sub-Neptune atmospheres overlying FeO-free, highly reduced magma oceans can be rich in monosilane gas, SiH4, all the way up to the observable 0.1 bar layer. The key added ingredient is the dissolution of water into the magma ocean, which previous H-O-Si atmospheric models left out. In the model, that dissolution lowers atmospheric H2O enough to shift the Si-O-H equilibrium so SiH4 reaches molar fractions of 0.1 to 10 percent and stays there instead of reoxidizing to silicates. If the claim holds, detecting SiH4 in a sub-Neptune's spectrum would be direct evidence for a rocky core capped by a reduced magma ocean.

What carries the argument

The argument rides on a closed H-O-Si mass balance at the magma-atmosphere interface. SiO2 liquid vaporizes (R1), the released oxygen forms H2O with H2 (R2), and SiO plus H2 makes SiH4 (R3); a water-solubility law (Eq. 7) ties the mass of H2O dissolved in the magma to the ground H2O partial pressure, while condensation of SiO (R5) and/or SiO2 (R4) with complete rainout removes oxygen and silicon aloft. Solving the dissolved-water and gas reservoirs together through Eq. (24) is what makes SiH4 the third-most-abundant gas and prevents its reoxidation in the upper atmosphere.

What would settle it

A cloud-microphysics calculation or laboratory experiment that determines whether SiO or SiO2 is the dominant condensate and how completely grains rain out would settle the claim: if SiO2 dominates or rainout is inefficient, the predicted SiH4 fraction at 0.1 bar should drop well below 0.1 percent across the parameter space, contradicting the paper's central result.

Watch

Extended reading notes

Core claim

The central claim is that on a sub-Neptune with an FeO-free magma ocean, dissolution of H2O into the melt makes the atmosphere more reduced and thereby allows SiH4 to remain abundant from the ground up to 0.1 bar. In their one-dimensional chemical-equilibrium model, the dissolution lowers the ground H2O fraction, which by Le Chatelier's principle drives the reaction SiO + 3H2 ⇌ SiH4 + H2O toward SiH4; with SiO condensation and complete rainout removing oxygen aloft, SiH4 stays near its ground value instead of collapsing to fractions below $10^{-5}$. The paper states the result directly: the dissolution of H2O enhances the SiH4 molar fraction to levels of 0.1 to 10 percent, preventing it from reverting to silicates in the upper atmospheric layers. This SiH4-rich regime occupies a broad parameter space at ground temperatures of 2000–6000 K and hydrogen pressures of $10^2$–$10^5$ bar.

Load-bearing premise

The persistence of SiH4 at 0.1 bar rests on the assumption that silicon monoxide vapor condenses and the grains fall out completely, stripping oxygen from the gas; if silicon dioxide dominates condensation or the rainout is incomplete, the extra oxygen would reoxidize SiH4 and deplete it in the observable layer.

Editorial extensions

If this is right

  • SiH4-rich atmospheres should exist across a wide range of ground temperatures and hydrogen pressures, reaching molar fractions above 0.1 percent at 0.1 bar over most of the explored parameter space.
  • Such atmospheres have a high mean molecular weight (up to about 6.2 times the hydrogen atom mass), reducing the scale height and planetary radius, while SiH4's high heat capacity raises the tropopause temperature.
  • SiH4-rich atmospheres would be depleted in C-, N-, and O-bearing gases, and they could contain other silanes such as SiH2, Si2H6, and Si3H8, especially in hotter upper layers.
  • Transmission spectra of these atmospheres show four characteristic SiH4 bands near 2–3, 3–4, 4–7, and 7–18 microns, distinguishable from H2O- and CH4-rich spectra.
  • A confirmed SiH4 detection in a sub-Neptune would indicate a highly reduced, FeO-free magma ocean in contact with a hydrogen-dominated atmosphere; most sub-Neptunes already observed with H2O or carbon-bearing molecules are unlikely to be in this regime.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A testable extension is to replace the imposed temperature-pressure profile with a radiative-convective equilibrium calculation once SiH4 opacity shortward of 2 microns is measured, which could either widen or narrow the region where SiH4 persists.
  • The most sensitive hinge is condensation microphysics: if SiO2 rather than SiO turns out to be the dominant condensate, or if rainout is incomplete, the predicted SiH4 fraction at 0.1 bar should drop substantially, so this is the first place to look for a contradiction.
  • Because alternative water-solubility laws with $\beta = 0.5$ give even higher dissolved-water fractions, the paper's nominal case is likely a conservative estimate of the SiH4-rich parameter space rather than an upper bound.
  • Observationally, featureless sub-Neptune spectra now attributed to high mean molecular weight or hazes could be re-examined as candidate silane worlds, since the model predicts both high mean molecular weight and strong SiH4 absorption.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper proposes that monosilane (SiH4) can be abundant and persist to observable pressures (0.1 bar) in sub-Neptune atmospheres overlying FeO-free (SiO2) magma oceans, provided that H2O dissolution into the magma is taken into account. The authors construct a 1D chemical-equilibrium model of a hydrogen-dominated atmosphere with H-O-Si chemistry, mass balance at the surface (Eqs. 16 and 24), a prescribed adiabatic/isothermal temperature profile, and rainout of SiO and SiO2 condensates. They find that H2O dissolution lowers the atmospheric H2O fraction, which enhances SiH4 at the surface and, together with SiO condensation/rainout that depletes H2O in the upper atmosphere, allows SiH4 to survive to 0.1 bar at molar fractions of 0.1-10% across a broad parameter space (Tgr = 2000-6000 K, PH2,gr = 1e2-1e5 bar). The paper also computes planetary radii and transmission spectra for these 'silane worlds' and discusses redox-state, magma-depth, and opacity caveats.

Significance. If the central claim holds, the paper identifies a new, observationally testable pathway to SiH4 in sub-Neptune atmospheres, with clear spectral signatures (2-18 μm) and a high mean molecular weight that affects transit radii. The core mechanism is clean: mass balance and the x_SiH4 ∝ x_H2O^-2 relation (Eq. 21) are transparent, and the no-dissolution control (Fig. 2b) demonstrates that H2O dissolution is the cause of the SiH4 enhancement. The authors provide sensitivity tests for water-solubility parameters, magma-ocean mass fraction, and non-ideal EOS effects, and they candidly acknowledge missing SiH4 opacity and uncertain condensation physics. The prediction is falsifiable with JWST/Ariel observations. These strengths make the paper valuable despite the uncertainties discussed below.

major comments (3)
  1. [Secs. 2.2.2, 3.2, and 4.4 (rainout and condensate identity)] The persistence of SiH4 to 0.1 bar and the pressure boundaries in Fig. 5a rest on two mechanistically load-bearing assumptions: (i) SiO(c) (R5), not SiO2(c) (R4), is the dominant condensate, and (ii) condensates completely rain out at every altitude. The paper states in Sec. 4.4 that equilibrium chemistry alone cannot establish the dominant condensate, and it cites a measured SiO sticking coefficient of 0.016 (Kimura et al. 2022), implying inefficient growth and therefore incomplete rainout. If SiO2(c) dominates, or if rainout is incomplete so that condensed oxygen returns to the gas, the O/Si removal ratio changes and the back-reaction of R3 (SiH4 + H2O → SiO + 3H2) may consume SiH4 before the 0.1-bar layer is reached. The sentence in Sec. 4.4 that the model is a 'lower estimate' if SiO2 dominates is not supported by a quantitative demonstration, and it does not address the separate issue of finite rainout efficiency, which would likely reduce SiH4. Since the quantitative 0.1-10% abundances and even part of the parameter space in Fig. 5a are contingent on this scheme, I ask the authors to (a) explicitly test the sensitivity to the condensate identity by imposing SiO2-only rainout, (b) introduce a rainout-efficiency parameter (e.g., the fraction of condensate removed per scale height) and show how the 0.1-bar SiH4 fraction and the boundaries in Fig. 5a respond, or (c) clearly reframe the persistence claim as conditional on efficient SiO rainout and state what observational or experimental evidence would be needed to validate this assumption.
  2. [Secs. 2.1.2 and 4.3.2 (extrapolation of water solubility)] The water solubility law (Eq. 7) is calibrated with α and β fitted to experiments at 900-1700 K and 1-3e4 bar (Papale 1997; Schaefer et al. 2016), yet the model applies it at ground temperatures up to 6000 K and hydrogen pressures up to 1e5 bar. The sensitivity tests in Fig. 9 use alternative solubility laws that are also calibrated at low temperatures (≤2173 K), so none of them constrain the 3000-6000 K regime. Because the surface SiH4 abundance scales as x_H2O^-2 (Eq. 21), this extrapolation directly propagates into the claimed 0.1-10% values. The authors should either present a scaling argument for how the solubility law might behave at extreme temperatures (e.g., a thermodynamic model of H2O speciation in SiO2 melt at high T and P) or explicitly state that the quantitative abundance range is subject to unquantified extrapolation error, and identify the experiments needed to reduce this uncertainty.
  3. [Secs. 2.2 and 4.5.2 (imposed temperature profile)] The temperature-pressure profile is prescribed (adiabatic up to Prcb, isothermal above) because SiH4 opacity data are unavailable. The altitude at which SiO condensation and rainout occur, and thus the efficiency of H2O depletion, depends on the T-P profile. A radiative-convective or conductive profile, such as those explored by Misener et al. (2023), could place the condensation level at a different pressure or temperature, potentially shifting the boundary where SiH4 survives to 0.1 bar. The authors acknowledge this limitation, but since the 0.1-bar persistence is the central observational claim, they should include a brief exploration of how the results change under alternative plausible T-P profiles (e.g., warmer or colder deep atmospheres) or state more rigorously what profile assumptions are needed for the conclusion to hold.
minor comments (6)
  1. [Sec. 2.2.2 (typo)] In the sentence 'These condensates are assumed to completelly rain out', 'completelly' should be 'completely'.
  2. [Sec. 2.1.3 (notation)] Equations (11) and (12) use the same symbols N_O and N_Si on the left-hand side (the new quantities) and on the right-hand side (the exotic oxygen/silicon terms). Please rename the exotic terms (e.g., N_O^ex, N_Si^ex) to avoid confusion.
  3. [Secs. 3.2 and 4.3.1 (reaction numbering)] The text refers to 'the reaction producing SiH4 from SiO and H2 (R4)' in two places; the correct reaction is R3, not R4. R4 is the SiO2(c) condensation reaction.
  4. [Fig. 5 caption (typo)] In the caption of Figure 5, 'at grand' should be 'at ground'.
  5. [Sec. 4.6.1 (typo)] In the discussion of silane decomposition, 'archived' should be 'achieved'.
  6. [Sec. 3.1 (clarity)] In the paragraph explaining the Si/O = 1 boundary, the sentence 'the fraction of SiH4 relative to H2 at ground approximately equals to that of H2O' could be clarified by stating explicitly that this corresponds to x_SiH4 ≈ x_H2O when O2 is negligible.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the SiH4 enhancement is derived from independent equilibrium constants and solubility data, and the remaining caveats are model limitations rather than circular reductions.

full rationale

The central derivation is self-contained. Ground composition is obtained by solving chemical equilibrium for R1-R5 with equilibrium constants from JANAF and Gail et al. (2013), together with water solubility from Papale (1997)/Schaefer et al. (2016) and the mass-balance relation NO = 2NSi. The predicted SiH4 enhancement follows algebraically from the equilibrium expressions (notably x_SiH4 proportional to x_H2O^-2, Eq. 21) once water dissolution lowers the ground H2O abundance through Eqs. (22)-(24). No parameter is fitted to the target SiH4 abundance, and the no-dissolution case (Fig. 2b) provides a genuine control that removes the effect. The condensation/rainout scheme (R4/R5 with complete rainout) is an assumed physical process, and Sec. 4.4 explicitly states that the dominance of SiO over SiO2 condensates and the efficiency of particle growth/rainout are not established by equilibrium chemistry; these are model uncertainties, not cases where a predicted quantity is identical to an input by construction. Self-citations (e.g., Seo et al. 2024; Ohno et al. 2025) appear only in contextual or observational remarks and are not load-bearing for the paper's claims. No circular step is present.

Assumptions & free parameters 3 free parameters · 7 assumptions · 0 invented entities

The model rests on an FeO-free pure SiO2 magma ocean, a prescribed T-P structure, ideal-gas thermodynamics, and a small H-O-Si reaction network. The free parameters (zeta, alpha, beta, XH2O cap) are either chosen by hand or fitted in prior experiments, not to the target SiH4 abundances. The most fragile input is the combination of complete SiO rainout and a fixed temperature profile, because both control whether SiH4 survives to 0.1 bar.

free parameters (3)
  • zeta (magma ocean mass fraction in core) = 0.5 nominal; 0.1 and 0.01 in sensitivity runs
    Controls the size of the H2O reservoir via Eq. (10); chosen by hand, not derived from the model. The persistence of SiH4 in the upper atmosphere disappears for zeta=0.01 (Sec. 4.2, Fig. 8).
  • alpha and beta in water solubility law = alpha = 3.44e-4.3 bar^-0.74, beta = 0.74
    Fitted to experimental solubility data (Papale 1997; Schaefer et al. 2016), Eq. (7). The SiH4 fraction at 0.1 bar is sensitive to these values (Sec. 4.3.2, Fig. 9), and the law is extrapolated beyond its 900-1700 K, 1 bar to 3e4 bar calibration range.
  • XH2O upper limit = 10 wt%
    Arbitrary cap at the onset of full miscibility (Sec. 2.1.2); reached only for Tgr >= 5000 K and PH2,gr >= 10^4.8 bar (Appendix A).
assumptions (7)
  • domain assumption FeO-free magma ocean with unity SiO2 activity (a_SiO2(l)=1), representing a highly reduced interior with no FeO buffering.
    The entire scenario is built on this. If FeO is present, the oxygen buffer changes and SiH4 is depleted (Sec. 2, Sec. 4.1).
  • domain assumption Elemental ratio NO = 2 NSi, i.e., all O and Si in the atmosphere plus magma derive from SiO2 vaporization with negligible exotic O, C, N, S.
    Eq. (15) and mass balance in Sec. 2.1.3. Invalid if Fe-oxides or accreted volatiles supply oxygen. The authors state this explicitly.
  • domain assumption Ideal gas and unity fugacity coefficients for all species, including H2 and H2O, up to 10^5 bar.
    Sec. 2.1.1. Deviations of H2/H2O fugacity are known above about 1000 bar (Kite et al. 2020) and are neglected for consistency with unknown SiH4 data.
  • domain assumption Adiabatic temperature profile from ground to tropopause and isothermal above, with the tropopause at Prcb (1 to 100 bar).
    Sec. 2.2. The vertical location of SiO condensation, which determines SiH4 persistence, depends on this assumed T-P profile. Radiative-convective equilibrium cannot be computed due to missing SiH4 opacity (Sec. 4.5.2).
  • domain assumption Thermodynamic data from JANAF are valid, including extrapolation of SiO2(l) data above 4500 K to 6000 K (Eq. 6) and water solubility law extrapolated to 2000 to 6000 K and up to 10^5 bar.
    Sec. 2.1.1 and Sec. 2.1.2. The paper states these extrapolations and their uncertainties (60 percent agreement for SiO2 vapor pressure; solubility consistent within 60 percent over the calibration range).
  • domain assumption Complete rainout of condensates and chemical equilibrium at every altitude.
    Sec. 2.1.1 and Sec. 2.2.2. The removal of SiO(c) is what depletes H2O and preserves SiH4. The sticking coefficient of SiO grains is low (0.016), so perfect rainout is an idealization (Sec. 4.4).
  • domain assumption Reaction network limited to H-O-Si species; C-, N-, and S-bearing gases are neglected.
    Sec. 4.5.3. SiC, Si3N4, and SiS are more refractory than SiO2 and could deplete SiH4 if C, N, or S are present. The authors give a solar-metallicity order-of-magnitude argument but do not model it in detail.

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Cite this review

Pith. "Pith review of Monosilane Worlds: Sub-Neptunes with Atmospheres Shaped by Reduced Magma Oceans." pith.science (2026). https://pith.science/paper/SLVH7V7S

@misc{pith2026250503200,
  author       = {Pith},
  title        = {Pith review of: Monosilane Worlds: Sub-Neptunes with Atmospheres Shaped by Reduced Magma Oceans},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/SLVH7V7S}},
  note         = {Machine review of arXiv:2505.03200}
}
abstract

High-precision infrared spectroscopic measurements now enable detailed characterization of sub-Neptune atmospheres, potentially providing constraints on their interiors. Motivated by this, atmospheric models have been developed to explore chemical interactions between hydrogen-dominated atmospheres and possibly underlying magma oceans with various redox states. Recent models have predicted monosilane (SiH$_4$) as a potential atmospheric species derived from magma oceans in sub-Neptunes, but suggested that it is highly depleted in the observable atmospheric layers. Here, we propose that SiH$_4$ can persist throughout the atmospheres of sub-Neptunes with FeO-free reduced magma oceans by considering the dissolution of H$_2$O into the magma oceans, a factor not accounted for in previous models. We construct a one-dimensional atmospheric model to simulate the chemical equilibrium composition of hydrogen-dominated atmospheres overlying FeO-free magma oceans, incorporating H-O-Si chemistry. Our results show that the dissolution of H$_2$O enhances the SiH$_4$ molar fraction to levels of 0.1--10~\%, preventing it from reverting to silicates in the upper atmospheric layers. We find that SiH$_4$-rich atmospheres can exist across a broad parameter space with ground temperatures of 2000--6000~K and hydrogen pressures of 10$^2$--10$^5$~bar. We discuss that SiH$_4$-rich atmospheres could contain the other silanes but lack C-/N-/O-bearing species. The detection of SiH$_4$ in future observations of sub-Neptunes would provide compelling evidence for the presence of a rocky core with a reduced magma ocean. However, the accuracy of our model is limited by the lack of data on the non-ideal behavior and radiative properties of SiH$_4$, highlighting the need for further numerical and laboratory investigations.

Figures

Figures reproduced from arXiv: 2505.03200 by the authors.

Figure 1
Figure 1. Schematic illustration of chemical interaction between an hydrogen-dominated atmosphere and a magma ocean in sub-Neptune with an oxidized FeO-containing magma ocean (left panel) and a reduced FeO-free magma ocean. Note that the focus of this study is the chemical in￾teraction in sub-Neptune with a reduced FeO-free magma ocean. See the text for details. 2. MODEL In this study, we model a hydrogen-dominated atmo￾spher… view at source ↗
Figure 2
Figure 2. Atmospheric structure with water dissolution into magma ocean (a) and without it (b) for a tropopause pressure of 10 bar, a ground H2 pressure of 3×104 bar and a ground temperature of 3000 K. The vertical distributions of SiH4 (purple), H2O (green), SiO (cyan) and the sum of H2 and He (orange), and temperature (black) are shown as functions of pressure from the ground pressure to 0.1 bar. The red dotted lines repres… view at source ↗
Figure 3
Figure 3. Molar fractions of H2O in the magma ocean (= XH2O ×60/18) (orange), atmospheric SiH4 (purple), H2O (green), and SiO (cyan) at the ground, and the ground temperature, Tgr (black), are shown as functions of the ground pressure, Pgr, for a resultant tropopause tempera￾ture, Trcb = 500 K, and Prcb = 10 bar. For comparison, the dashed lines represent the results obtained when H2O dissolution into the magma ocean is ignor… view at source ↗
Figures from the paper (11 more)
Figure 5
Figure 5. Figure 5: Atmospheric molar fractions of SiH4 at 0.1 bar (a) and at grand (b), that of H2O (c) and SiO (d) at ground, H2O mass concentration in magma (e), and H2 ground pressure (f) for different ground pressure, Pgr, and temperature, Tgr. Contour counters and lines shows the lo…
Figure 6
Figure 6. Figure 6: Planetary radius at 0.1 bar (left column) and tropopause temperature (right column) for different ground pressure, Pgr, and temperature, Tgr. For the pressure of radiative convective boundary, Prcb, we assume 100 bar (a), 10 bar (b) and, 1 bar (c). Dotted lines in left…
Figure 7
Figure 7. Figure 7: Redox state of magma ocean expressed as ∆IW (a) and O2 ground pressure (b) for different ground pressure, Psurf, and temperature, Tgr. Color counter and lines show the value of ∆IW calculated from the oxygen pressure and the reported function of the oxygen fugacity of …
Figure 8
Figure 8. Figure 8: Molar fractions of H2O in the magma ocean (= XH2O ×60/18) (orange), atmospheric SiH4 (purple), H2O (green), and SiO (cyan) at the ground, and the ground tem￾perature, Tgr (black), are shown as functions of the ground pressure, Pgr, for Trcb = 500 K and Prcb = 10 bar. U…
Figure 9
Figure 9. Figure 9: Molar fractions of SiH4 at 0.1 bar for different α and β values in water solubility law: 2.15 × 10−4 bar−0.7 and 0.7 (a), 5 × 10−4 bar−0.5 and 0.5 (b), and 10 × 10−4 bar−0.5 and 0.5 (c). Contour counters and lines show the log10 values of the fractions. Black dotted li…
Figure 10
Figure 10. Figure 10: Difference of planetary radius at 0.1 bar between our nominal calculation ( [PITH_FULL_IMAGE:figures/full_fig_p018_10.png]
Figure 11
Figure 11. Figure 11: Relative mole fractions of SiH3/SiH4 (purple), SiH2/SiH4 (green), and SiH/SiH4 (light blue) are shown as a function of hydrogen pressure for three isothermal tem￾peratures of 1000 K (solid), 1250 K (dashed) and 1500 K (dotted). Therefore, these metal hydrides could se…
Figure 12
Figure 12. Figure 12: Transmission spectrum for the atmosphere of a planet orbiting a star with a radius of 0.2 R⊙ under the same conditions as in [PITH_FULL_IMAGE:figures/full_fig_p021_12.png]
Figure 13
Figure 13. Figure 13: The parameter space of ground temperature and hydrogen ground pressure where XH2O reaches the upper limit in our results is shown as a red shaded region. APPENDIX A. PARAMETER SPACE WHERE WATER FRACTION IN MAGMA REACHES ITS UPPER LIMIT We set the upper limit of a H2O …
Figure 14
Figure 14. Figure 14: h (Eq. B1) are shown as functions of xH2O for five combinations of ground temperature and hydrogen ground pressure; Tgr = 2000 K and PH2,gr = 103 bar (purple), 2000 K and 104 bar (green), 2000 K and 105 bar (cyan), 4000 K and 104 bar (orange), and 6000 K and 104 bar (…
Figure 15
Figure 15. Figure 15: Approximated solution of pressure boundaries with a Si/O ratio of one is shown as a function of ground temperature for parameters assumed in our nominal simulation in Sec. 3. Dotted line represents the pressure boundaries calculated by our model, which is the same as …

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Works this paper leans on

106 extracted references · 1 canonical work pages · cited by 2 Pith papers

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    PDq;awfgwܹ_9agVS Nv+uO7̸ L @ @ @ @ @ @ @ @ @ @ @ hh4 (F * ^ 4A @ @ @ @ @ @ @ @ @ @ y @ Pp D H H H H H H H H H H H (W

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    2021

  4. [4]

    R., Seager , S., & Elkins-Tanton , L

    Adams , E. R., Seager , S., & Elkins-Tanton , L. 2008, , 673, 1160, 10.1086/524925

    doi:10.1086/524925 2008

  5. [5]

    F., Changeat , Q., Waldmann , I

    Al-Refaie , A. F., Changeat , Q., Waldmann , I. P., & Tinetti , G. 2021, , 917, 37, 10.3847/1538-4357/ac0252

    doi:10.3847/1538-4357/ac0252 2021

  6. [6]

    K., Gao , P., Adams Redai , J., et al

    Alam , M. K., Gao , P., Adams Redai , J., et al. 2025, , 169, 15, 10.3847/1538-3881/ad8eb5

    doi:10.3847/1538-3881/ad8eb5 2025

  7. [7]

    E., Wakeford , H

    Alderson , L., Batalha , N. E., Wakeford , H. R., et al. 2024, , 167, 216, 10.3847/1538-3881/ad32c9

    doi:10.3847/1538-3881/ad32c9 2024

  8. [8]

    S., Hirschmann, M

    Armstrong, L. S., Hirschmann, M. M., Stanley, B. D., Falksen, E. G., & Jacobsen, S. D. 2015, Geochimica et Cosmochimica Acta, 171, 283, https://doi.org/10.1016/j.gca.2015.07.007

    doi:10.1016/j.gca.2015.07.007 2015

Show all 106 references
  1. [9]

    G., Welbanks , L., Schlawin , E., et al

    Beatty , T. G., Welbanks , L., Schlawin , E., et al. 2024, , 970, L10, 10.3847/2041-8213/ad55e9

    2024 doi

  2. [10]

    2024, arXiv e-prints, arXiv:2403.03325, 10.48550/arXiv.2403.03325

    Benneke , B., Roy , P.-A., Coulombe , L.-P., et al. 2024, arXiv e-prints, arXiv:2403.03325, 10.48550/arXiv.2403.03325

    2024 doi arXiv

  3. [11]

    2002, American Mineralogist, 87, 1717, 10.2138/am-2002-11-1222

    Berndt , J., Liebske , C., Holtz , F., et al. 2002, American Mineralogist, 87, 1717, 10.2138/am-2002-11-1222

    2002 doi

  4. [12]

    J., Hakim , K., Sossi , P

    Bower , D. J., Hakim , K., Sossi , P. A., & Sanan , P. 2022, , 3, 93, 10.3847/PSJ/ac5fb1

    2022 doi

  5. [13]

    Brande , J., Crossfield , I. J. M., Kreidberg , L., et al. 2024, , 961, L23, 10.3847/2041-8213/ad1b5c

    2024 doi

  6. [14]

    2024, Nature Astronomy, 8, 463, 10.1038/s41550-023-02183-7

    Burn , R., Mordasini , C., Mishra , L., et al. 2024, Nature Astronomy, 8, 463, 10.1038/s41550-023-02183-7

    2024 doi

  7. [15]

    2021, , 917, 4, 10.3847/1538-4357/abfc48

    Chabrier , G., & Debras , F. 2021, , 917, 4, 10.3847/1538-4357/abfc48

    2021 doi

  8. [16]

    Chachan , Y., & Stevenson , D. J. 2018, , 854, 21, 10.3847/1538-4357/aaa459

    2018 doi

  9. [17]

    2023, , 674, A224, 10.1051/0004-6361/202245763

    Charnoz , S., Falco , A., Tremblin , P., et al. 2023, , 674, A224, 10.1051/0004-6361/202245763

    2023 doi

  10. [18]

    1998, NIST-JANAF Thermochemical Tables, 4th Edition (American Institute of Physics, -1)

    Chase, M. 1998, NIST-JANAF Thermochemical Tables, 4th Edition (American Institute of Physics, -1)

    1998

  11. [19]

    P., M^^c3^^a9vel, R., & Lacoste, D

    Chatelain, K. P., M^^c3^^a9vel, R., & Lacoste, D. A. 2020, Combustion and Flame, 217, 346, https://doi.org/10.1016/j.combustflame.2020.03.028

    2020 doi

  12. [20]

    2022, , 336, 291, 10.1016/j.gca.2022.09.012

    Dasgupta , R., Falksen , E., Pal , A., & Sun , C. 2022, , 336, 291, 10.1016/j.gca.2022.09.012

    2022 doi

  13. [21]

    2017, , 541, 521, 10.1038/nature20830

    Dauphas , N. 2017, , 541, 521, 10.1038/nature20830

    2017 doi

  14. [22]

    Davenport , B., Kempton , E. M. R., Nixon , M. C., et al. 2025, arXiv e-prints, arXiv:2501.01498, 10.48550/arXiv.2501.01498

    2025 doi arXiv

  15. [23]

    2004, Phys

    De Bleecker, K., Bogaerts, A., Gijbels, R., & Goedheer, W. 2004, Phys. Rev. E, 69, 056409, 10.1103/PhysRevE.69.056409

    2004 doi

  16. [24]

    E., STOLPER, E

    DIXON, J. E., STOLPER, E. M., & HOLLOWAY, J. R. 1995, Journal of Petrology, 36, 1607, 10.1093/oxfordjournals.petrology.a037267

    1995 doi

  17. [25]

    T., & Seager , S

    Elkins-Tanton , L. T., & Seager , S. 2008, , 688, 628, 10.1086/592316

    2008 doi

  18. [26]

    J., & Lagage , P.-O

    Falco , A., Tremblin , P., Charnoz , S., Ridgway , R. J., & Lagage , P.-O. 2024, , 683, A194, 10.1051/0004-6361/202347650

    2024 doi

  19. [27]

    1994, , 110, 117, 10.1006/icar.1994.1111

    Fegley , Bruce, J., & Lodders , K. 1994, , 110, 117, 10.1006/icar.1994.1111

    1994

  20. [28]

    A., Nakajima, Y., Campbell, A

    Fischer, R. A., Nakajima, Y., Campbell, A. J., et al. 2015, Geochimica et Cosmochimica Acta, 167, 177, https://doi.org/10.1016/j.gca.2015.06.026

    2015 doi

  21. [29]

    A., Hess , P

    Fogel , R. A., Hess , P. C., & Rutherford , M. J. 1989, , 53, 2735, 10.1016/0016-7037(89)90145-2

    1989 doi

  22. [30]

    J., Lupu , R

    Fortney , J. J., Lupu , R. E., Morley , C. V., Freedman , R. S., & Hood , C. 2019, , 880, L16, 10.3847/2041-8213/ab2a10

    2019 doi

  23. [31]

    J., Marley , M

    Fortney , J. J., Marley , M. S., & Barnes , J. W. 2007, , 659, 1661, 10.1086/512120

    2007 doi

  24. [32]

    French , B. M. 1966, Reviews of Geophysics and Space Physics, 4, 223, 10.1029/RG004i002p00223

    1966 doi

  25. [33]

    Frost , B. R. 1979, American Journal of Science, 279, 1033, 10.2475/ajs.279.9.1033

    1979 doi

  26. [34]

    J., & McCammon , C

    Frost , D. J., & McCammon , C. A. 2008, Annual Review of Earth and Planetary Sciences, 36, 389, 10.1146/annurev.earth.36.031207.124322

    2008

  27. [35]

    P., Wetzel , S., Pucci , A., & Tamanai , A

    Gail , H. P., Wetzel , S., Pucci , A., & Tamanai , A. 2013, , 555, A119, 10.1051/0004-6361/201321807

    2013 doi

  28. [36]

    2022, Earth and Planetary Science Letters, 577, 117255, 10.1016/j.epsl.2021.117255

    Gaillard , F., Bernadou , F., Roskosz , M., et al. 2022, Earth and Planetary Science Letters, 577, 117255, 10.1016/j.epsl.2021.117255

    2022

  29. [37]

    Gao , P., Piette , A. A. A., Steinrueck , M. E., et al. 2023, , 951, 96, 10.3847/1538-4357/acd16f

    2023 doi

  30. [38]

    1987, Combustion and Flame, 68, 43, https://doi.org/10.1016/0010-2180(87)90064-2

    Hartman, J., Famil-Ghiriha, J., Ring, M., & O'Neal, H. 1987, Combustion and Flame, 68, 43, https://doi.org/10.1016/0010-2180(87)90064-2

    1987 doi

  31. [39]

    Haynes , W. M. 2014, CRC Handbook of Chemistry and Physics, 95th edition

    2014

  32. [40]

    R., & Tsai , S.-M

    Heng , K., Lyons , J. R., & Tsai , S.-M. 2016, , 816, 96, 10.3847/0004-637X/816/2/96

    2016 doi

  33. [41]

    M., Withers , A

    Hirschmann , M. M., Withers , A. C., Ardia , P., & Foley , N. T. 2012, Earth and Planetary Science Letters, 345, 38, 10.1016/j.epsl.2012.06.031

    2012 doi

  34. [42]

    M., Ghiorso , M

    Hirschmann , M. M., Ghiorso , M. S., Davis , F. A., et al. 2008, Geochemistry, Geophysics, Geosystems, 9, Q03011, 10.1029/2007GC001894

    2008 doi

  35. [43]

    Holloway, J. R. 1981, Volatile Interactions in Magmas, ed. R. C. Newton, A. Navrotsky, & B. J. Wood (New York, NY: Springer New York), 273--293, 10.1007/978-1-4612-5871-1_13

    1981 doi

  36. [44]

    R., & Blank, J

    Holloway, J. R., & Blank, J. G. 1994, Chapter 6. APPLICATION OF EXPERIMENTAL RESULTS TO C-O-H SPECIES IN NATURAL MELTS, ed. M. R. Carroll & J. R. Holloway (Berlin, Boston: De Gruyter), 187--230, doi:10.1515/9781501509674-012

    1994 doi

  37. [45]

    2024, , 683, L2, 10.1051/0004-6361/202348238

    Holmberg , M., & Madhusudhan , N. 2024, , 683, L2, 10.1051/0004-6361/202348238

    2024 doi

  38. [46]

    2000, American Mineralogist, 85, 682, 10.2138/am-2000-5-604

    Holtz, F., Roux, J., Behrens, H., & Pichavant, M. 2000, American Mineralogist, 85, 682, 10.2138/am-2000-5-604

    2000 doi

  39. [47]

    W., Prakapenka , V., Chariton , S., Speziale , S., & Shim , S

    Horn , H. W., Prakapenka , V., Chariton , S., Speziale , S., & Shim , S. H. 2023, , 4, 30, 10.3847/PSJ/acab03

    2023 doi

  40. [48]

    E., Isella , A., et al

    Izidoro , A., Schlichting , H. E., Isella , A., et al. 2022, , 939, L19, 10.3847/2041-8213/ac990d

    2022 doi

  41. [49]

    2010, Earth and Planetary Science Letters, 293, 259, https://doi.org/10.1016/j.epsl.2010.02.033

    Javoy, M., Kaminski, E., Guyot, F., et al. 2010, Earth and Planetary Science Letters, 293, 259, https://doi.org/10.1016/j.epsl.2010.02.033

    2010 doi

  42. [50]

    2018, , 853, 163, 10.3847/1538-4357/aa9f1e

    Jin , S., & Mordasini , C. 2018, , 853, 163, 10.3847/1538-4357/aa9f1e

    2018 doi

  43. [51]

    Kempton , E. M. R., Zhang , M., Bean , J. L., et al. 2023, , 620, 67, 10.1038/s41586-023-06159-5

    2023 doi

  44. [52]

    C., Wasserburg , G

    Kennedy , G. C., Wasserburg , G. J., Heard , H. C., & Newton , R. C. 1962, American Journal of Science, 260, 501, 10.2475/ajs.260.7.501

    1962 doi

  45. [53]

    2023, Proceedings of the National Academy of Science, 120, e2309786120, 10.1073/pnas.2309786120

    Kim , T., Wei , X., Chariton , S., et al. 2023, Proceedings of the National Academy of Science, 120, e2309786120, 10.1073/pnas.2309786120

    2023 doi

  46. [54]

    K., Inatomi , Y., Ferguson , F

    Kimura , Y., Tanaka , K. K., Inatomi , Y., Ferguson , F. T., & Nuth , J. A. 2022, , 934, L10, 10.3847/2041-8213/ac8002

    2022 doi

  47. [55]

    S., Fegley , Bruce, J., Schaefer , L., & Ford , E

    Kite , E. S., Fegley , Bruce, J., Schaefer , L., & Ford , E. B. 2020, , 891, 111, 10.3847/1538-4357/ab6ffb

    2020 doi

  48. [56]

    W., & Patzer , A

    Kitzmann , D., Stock , J. W., & Patzer , A. B. C. 2024, , 527, 7263, 10.1093/mnras/stad3515

    2024 doi

  49. [57]

    A., Benneke , B., Deming , D., & Homeier , D

    Knutson , H. A., Benneke , B., Deming , D., & Homeier , D. 2014, , 505, 66, 10.1038/nature12887

    2014 doi

  50. [58]

    L., D \'e sert , J.-M., et al

    Kreidberg , L., Bean , J. L., D \'e sert , J.-M., et al. 2014, , 505, 69, 10.1038/nature12888

    2014 doi

  51. [59]

    1996, , 101, 14909, 10.1029/96JE00940

    Kuramoto , K., & Matsui , T. 1996, , 101, 14909, 10.1029/96JE00940

    1996 doi

  52. [60]

    2021, , 914, L4, 10.3847/2041-8213/ac0146

    Lichtenberg , T. 2021, , 914, L4, 10.3847/2041-8213/ac0146

    2021 doi

  53. [61]

    2021, , 217, 44, 10.1007/s11214-021-00825-8

    Lodders , K. 2021, , 217, 44, 10.1007/s11214-021-00825-8

    2021 doi

  54. [62]

    2023, , 956, L13, 10.3847/2041-8213/acf577

    Madhusudhan , N., Sarkar , S., Constantinou , S., et al. 2023, , 956, L13, 10.3847/2041-8213/acf577

    2023 doi

  55. [63]

    2009, , 690, 1056, 10.1088/0004-637X/690/2/1056

    Miller-Ricci , E., Seager , S., & Sasselov , D. 2009, , 690, 1056, 10.1088/0004-637X/690/2/1056

    2009 doi

  56. [64]

    Miller-Ricci Kempton , E., Zahnle , K., & Fortney , J. J. 2012, , 745, 3, 10.1088/0004-637X/745/1/3

    2012 doi

  57. [65]

    Misener , W., & Schlichting , H. E. 2022, , 514, 6025, 10.1093/mnras/stac1732

    2022 doi

  58. [66]

    E., & Young , E

    Misener , W., Schlichting , H. E., & Young , E. D. 2023, , 524, 981, 10.1093/mnras/stad1910

    2023 doi

  59. [67]

    1976, Journal of Crystal Growth, 33, 1, https://doi.org/10.1016/0022-0248(76)90072-5

    Murthy, T., Miyamoto, N., Shimbo, M., & Nishizawa, J. 1976, Journal of Crystal Growth, 33, 1, https://doi.org/10.1016/0022-0248(76)90072-5

    1976 doi

  60. [68]

    E., Brett , A., Beckett , J

    Newcombe , M. E., Brett , A., Beckett , J. R., et al. 2017, , 200, 330, 10.1016/j.gca.2016.12.026

    2017 doi

  61. [69]

    C., & Manning , C

    Newton , R. C., & Manning , C. E. 2008, Earth and Planetary Science Letters, 274, 241, 10.1016/j.epsl.2008.07.028

    2008 doi

  62. [70]

    2017, Geochimica et Cosmochimica Acta, 204, 68, https://doi.org/10.1016/j.gca.2016.12.042

    Novella, D., Dolej^^c5^^a1, D., Myhill, R., et al. 2017, Geochimica et Cosmochimica Acta, 204, 68, https://doi.org/10.1016/j.gca.2016.12.042

    2017 doi

  63. [71]

    I., Facchini , S., & Anderson , D

    \"O berg , K. I., Facchini , S., & Anderson , D. E. 2023, , 61, 287, 10.1146/annurev-astro-022823-040820

    2023 doi

  64. [72]

    J., et al

    Ohno , K., Schlawin , E., Bell , T. J., et al. 2025, , 979, L7, 10.3847/2041-8213/ada02c

    2025 doi

  65. [73]

    O'Neill , H. S. C. 2002, Journal of Petrology, 43, 1049, 10.1093/petrology/43.6.1049

    2002 doi

  66. [74]

    A., & Panfilov, V

    Onischuk, A. A., & Panfilov, V. N. 2001, Russian Chemical Reviews, 70, 321, 10.1070/RC2001v070n04ABEH000603

    2001 doi

  67. [75]

    Owens , A., Yachmenev , A., Thiel , W., Tennyson , J., & Yurchenko , S. N. 2017, , 471, 5025, 10.1093/mnras/stx1952

    2017 doi

  68. [76]

    1997, Contributions to Mineralogy and Petrology, 126, 237, 10.1007/s004100050247

    Papale , P. 1997, Contributions to Mineralogy and Petrology, 126, 237, 10.1007/s004100050247

    1997 doi

  69. [77]

    2024, , 974, L10, 10.3847/2041-8213/ad6f00

    Piaulet-Ghorayeb , C., Benneke , B., Radica , M., et al. 2024, , 974, L10, 10.3847/2041-8213/ad6f00

    2024 doi

  70. [78]

    R., Danielson , L., Pando , K., & Newville , M

    Righter , K., Sutton , S. R., Danielson , L., Pando , K., & Newville , M. 2016, American Mineralogist, 101, 1928, 10.2138/am-2016-5638

    2016 doi

  71. [79]

    Ringwood, A. E. 1977, GEOCHEMICAL JOURNAL, 11, 111, 10.2343/geochemj.11.111

    1977 doi

  72. [80]

    G., & Owen , J

    Rogers , J. G., & Owen , J. E. 2021, , 503, 1526, 10.1093/mnras/stab529

    2021 doi

  73. [81]

    1990, in Origin of the Earth, ed

    Sasaki , S. 1990, in Origin of the Earth, ed. H. E. Newsom & J. H. Jones , 195--209

    1990

  74. [82]

    R., et al

    Scarsdale , N., Wogan , N., Wakeford , H. R., et al. 2024, , 168, 276, 10.3847/1538-3881/ad73cf

    2024 doi

  75. [83]

    D., Berta-Thompson , Z., & Sasselov , D

    Schaefer , L., Wordsworth , R. D., Berta-Thompson , Z., & Sasselov , D. 2016, , 829, 63, 10.3847/0004-637X/829/2/63

    2016 doi

  76. [84]

    J., et al

    Schlawin , E., Ohno , K., Bell , T. J., et al. 2024, , 974, L33, 10.3847/2041-8213/ad7fef

    2024 doi

  77. [85]

    E., & Young , E

    Schlichting , H. E., & Young , E. D. 2022, , 3, 127, 10.3847/PSJ/ac68e6

    2022 doi

  78. [86]

    L., Sossi , P

    Seidler , F. L., Sossi , P. A., & Grimm , S. L. 2024, , 691, A159, 10.1051/0004-6361/202450546

    2024 doi

  79. [87]

    2024, arXiv e-prints, arXiv:2408.17056, 10.48550/arXiv.2408.17056

    Seo , C., Ito , Y., & Fujii , Y. 2024, arXiv e-prints, arXiv:2408.17056, 10.48550/arXiv.2408.17056

    2024 doi arXiv

  80. [88]

    2013, American Mineralogist, 98, 1604, 10.2138/am.2013.4434

    Shinozaki , A., Hirai , H., Ohfuji , H., et al. 2013, American Mineralogist, 98, 1604, 10.2138/am.2013.4434

    2013

  81. [89]

    2016, Physics and Chemistry of Minerals, 43, 277, 10.1007/s00269-015-0792-3

    Shinozaki , A., Kagi , H., Hirai , H., et al. 2016, Physics and Chemistry of Minerals, 43, 277, 10.1007/s00269-015-0792-3

    2016 doi

  82. [90]

    2014, American Mineralogist, 99, 1265, 10.2138/am.2014.4798

    Shinozaki , A., Kagi , H., Noguchi , N., et al. 2014, American Mineralogist, 99, 1265, 10.2138/am.2014.4798

    2014

  83. [91]

    Shorttle , O., Jordan , S., Nicholls , H., Lichtenberg , T., & Bower , D. J. 2024, , 962, L8, 10.3847/2041-8213/ad206e

    2024 doi

  84. [92]

    A., Burnham , A

    Sossi , P. A., Burnham , A. D., Badro , J., et al. 2020, Science Advances, 6, eabd1387, 10.1126/sciadv.abd1387

    2020 doi

  85. [93]

    A., Tollan , P

    Sossi , P. A., Tollan , P. M. E., Badro , J., & Bower , D. J. 2023, Earth and Planetary Science Letters, 601, 117894, 10.1016/j.epsl.2022.117894

    2023

  86. [94]

    2024, , 963, 157, 10.3847/1538-4357/ad217c

    Tian , M., & Heng , K. 2024, , 963, 157, 10.3847/1538-4357/ad217c

    2024 doi

  87. [95]

    2022, in European Planetary Science Congress, EPSC2022--1114, 10.5194/epsc2022-1114

    Tinetti , G., Eccleston , P., Lueftinger , T., et al. 2022, in European Planetary Science Congress, EPSC2022--1114, 10.5194/epsc2022-1114

    2022 doi

  88. [96]

    D., & O'Connell , R

    Valencia , D., Sasselov , D. D., & O'Connell , R. J. 2007, , 665, 1413, 10.1086/519554

    2007 doi

  89. [97]

    2013, , 767, L12, 10.1088/2041-8205/767/1/L12

    Visscher , C., & Fegley , Bruce, J. 2013, , 767, L12, 10.1088/2041-8205/767/1/L12

    2013 doi

  90. [98]

    2010, , 716, 1060, 10.1088/0004-637X/716/2/1060

    Visscher , C., Lodders , K., & Fegley , Bruce, J. 2010, , 716, 1060, 10.1088/0004-637X/716/2/1060

    2010 doi

  91. [99]

    L., Batalha , N

    Wallack , N. L., Batalha , N. E., Alderson , L., et al. 2024, , 168, 77, 10.3847/1538-3881/ad3917

    2024 doi

  92. [100]

    1981, Philosophical Transactions of the Royal Society of London Series A, 303, 287, 10.1098/rsta.1981.0203

    Wanke , H. 1981, Philosophical Transactions of the Royal Society of London Series A, 303, 287, 10.1098/rsta.1981.0203

    1981

  93. [101]

    Warren, P. H. 2011, Earth and Planetary Science Letters, 311, 93, https://doi.org/10.1016/j.epsl.2011.08.047

    2011 doi

  94. [102]

    Wilson , L., & Head , J. W. 1981, , 86, 2971, 10.1029/JB086iB04p02971

    1981 doi

  95. [103]

    M., Preston, T

    Wyller, G. M., Preston, T. J., Anjitha, S., Skare, M. O., & Marstein, E. S. 2020, Journal of Crystal Growth, 530, 125305, https://doi.org/10.1016/j.jcrysgro.2019.125305

    2020

  96. [104]

    M., Preston, T

    Wyller, G. M., Preston, T. J., Klette, H., et al. 2016, Energy Procedia, 92, 904, https://doi.org/10.1016/j.egypro.2016.07.100

    2016 doi

  97. [105]

    M., Preston, T

    Wyller, G. M., Preston, T. J., Mongstad, T. T., et al. 2017, Energy Procedia, 124, 814, https://doi.org/10.1016/j.egypro.2017.09.352

    2017 doi

  98. [106]

    2009, , 73, 2089, 10.1016/j.gca.2009.01.021

    Zhang , C., & Duan , Z. 2009, , 73, 2089, 10.1016/j.gca.2009.01.021

    2009 doi

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