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REVIEW 3 major objections 4 minor 79 references

Modeling Atmospheric Alteration on Titan: Hydrodynamics and Shock-Induced Chemistry of Meteoroid Entry

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Meteoroid entry into Titan's atmosphere drives shock chemistry that makes HCN so efficiently that about one hundred 1-km entries could supply the observed hydrogen cyanide, while also destroying water vapor and leaving nitrogen stable.

desk verdict Solid shock-chemistry framework, but the '100 events' HCN claim is undone by the paper's own photochemical loss timescale and rate-coefficient uncertainty. read the letter →

arxiv 2507.10369 v1 pith:TWMEVV3M submitted 2025-07-14 astro-ph.EP

Ryushi Miyayama , Laura Kay Schaefer , Hiroshi Kobayashi , Andrea Zorzi This is my paper
classification astro-ph.EP
keywords Titanmeteoroidatmosphericentrybowshocknon-equilibriumchemistrychemicalkineticsquenchingHCNsynthesishydrodynamicalsimulation
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

Meteoroids entering Titan's atmosphere generate bow shocks that heat the surrounding nitrogen–methane gas to thousands of kelvin, after which the gas cools by expansion so quickly that its chemical reactions freeze out before equilibrium is reached. The paper shows that this non-equilibrium, 'quenched' chemistry sets the post-entry composition and is far more productive than equilibrium chemistry: the simulated HCN molar fraction reaches about $10^{-2}$, against roughly $4\times10^{-6}$ at equilibrium. Integrated over the heated column, a single 1-km object entering at 10 km/s yields about $1.5\times10^{11}$ mol of HCN, so only about 100 such events would be needed to account for the HCN observed in Titan's atmosphere today. The same mechanism removes water vapor efficiently while leaving the dominant $\mathrm{N}_2$ component stable, and the simulated yields agree with laser-induced plasma experiments on Titan-like gas mixtures. If the claim holds, meteoroid entry is a major abiotic, non-photochemical source of a prebiotic feedstock in Titan's lower atmosphere, where ultraviolet radiation no longer drives photochemistry.

What carries the argument

The load-bearing mechanism is chemical quenching in the post-shock expansion flow: the cooling timescale $\tau_{\mathrm{cool}}\sim R_{\mathrm{com}}/v_{\mathrm{ent}}$ is set purely by meteoroid size and entry velocity, and once expansion outruns the reaction timescales the gas composition freezes at non-equilibrium values. The method couples the Athena++ hydrodynamic solver, which produces the bow-shock flow and the secondary shock in the meteoroid's co-moving frame, with the Cantera kinetics package integrating the GRI-Mech 3.0 C/H/N/O network along test-particle streamlines. Three reactions carry most of the HCN production: $\mathrm{CH} + \mathrm{N}_2 \to \mathrm{HCN} + \mathrm{N}$ (49%), $\mathrm{H}_2\mathrm{CN} \to \mathrm{HCN} + \mathrm{H}$ (40%), and $\mathrm{CH}_3 + \mathrm{N} \to \mathrm{HCN} + \mathrm{H}_2$ (9.4%). The equilibrium-versus-non-equilibrium contrast is the analytical pivot: because expansion cooling beats the reactions except at the hottest instants, the final mixture is set by quench temperatures of roughly 500–1000 K rather than by thermodynamic equilibrium.

What would settle it

A shock-tube or laser-plasma measurement of $\mathrm{CH} + \mathrm{N}_2 \to \mathrm{HCN} + \mathrm{N}$ at 2000–3000 K would settle the main quantitative claim: the rate used in the paper is $8.0\times10^{-17}$ m$^3$ molecule$^{-1}$ s$^{-1}$ at 2447 K, while the experimental values it cites span $4.9\times10^{-14}$ to $2.8\times10^{-12}$ m$^3$ molecule$^{-1}$ s$^{-1}$, nearly two orders of magnitude, and the integrated HCN yield scales with this rate. A definitive measurement would confirm or rescale the inferred 'about 100 events' by the corresponding factor. A complementary atmospheric test is to measure HCN mixing ratios in Titan's 40–100 km altitude range: if entry chemistry is the dominant source there, the abundance should be reproducible from the meteoroid influx alone and should not follow the photochemical vertical profile.

Watch

Extended reading notes

Core claim

The paper's central claim is that the chemical aftermath of meteoroid entry must be modeled as a time-dependent, non-equilibrium process rather than as a sequence of equilibrium states. By tracking gas parcels along streamlines through the three-dimensional bow-shock flow and feeding each parcel's temperature–pressure history into a chemical kinetics solver, the authors find that products freeze at quench temperatures of roughly 500–1000 K, well below the 1000–3000 K range typically assumed for impact vapors. The result is a strong enhancement of HCN: the non-equilibrium molar fraction is about three orders of magnitude above the equilibrium prediction, and three reactions dominate the yield, led by $\mathrm{CH} + \mathrm{N}_2 \to \mathrm{HCN} + \mathrm{N}$ at nearly half. Applied to Titan, the integrated yields imply that on the order of 100 entry events of 1-km objects at 10 km/s could supply the present HCN abundance, that water vapor is reduced by about four orders of magnitude with oxygen converted into CO, and that $\mathrm{N}_2$ remains stable, a pattern the authors state is inconsistent with equilibrium-chemistry assumptions. The simulated production yields also agree with the molecule-per-joule values measured in laser-induced plasma experiments on $\mathrm{N}_2$–$\mathrm{CH}_4$ mixtures, and the simulations reveal a secondary shock behind the meteoroid, a feature absent from previous one-dimensional entry models, which reheats the gas but leaves already-quenched species such as HCN unaltered.

Load-bearing premise

The 'about 100 events' result depends on the rate coefficients that the GRI-Mech 3.0 network assigns to HCN formation, and the paper itself reports that the dominant reaction, $\mathrm{CH} + \mathrm{N}_2 \to \mathrm{HCN} + \mathrm{N}$, has measured rate coefficients spanning nearly two orders of magnitude at 2447 K, with no reliable data at all for the other two dominant reactions.

Editorial extensions

If this is right

  • Meteoroid entry becomes a viable non-photochemical HCN source in Titan's lower atmosphere, below about 100 km, where the ultraviolet radiation that drives photochemistry is effectively absent.
  • On the order of 100 entries of 1-km objects at 10 km/s could supply the present HCN reservoir, and because the early impact flux on Titan may have exceeded 1000 such events, entry chemistry plausibly shaped the organic content of the early atmosphere.
  • The same shock processing gives a natural explanation for Titan's present low water abundance: a single entry reduces water vapor by about four orders of magnitude and channels the oxygen into CO.
  • Because the HCN yield is nearly independent of the $\mathrm{N}_2$:$\mathrm{CH}_4$ ratio, the mechanism operates consistently across Titan's history even as the bulk atmospheric composition evolved.
  • Aerodynamic entry chemistry can rival impact-vaporization chemistry as a driver of atmospheric change, especially on rocky-surfaced worlds where 10 km/s impacts vaporize little surface material.

Reading between the lines

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

  • The same quenching mechanism should operate in any $\mathrm{N}_2$–$\mathrm{CH}_4$ atmosphere receiving a meteoroid influx, so the framework transfers to other reducing atmospheres such as an early Earth or a Pluto-like body, with yields set by the ratio of object radius to entry velocity.
  • Because the HCN yield is tied directly to the rate of the dominant reaction, and the paper quotes experimental values for it spanning nearly two orders of magnitude, the 'about 100 events' figure is best read as an order-of-magnitude estimate; a better rate measurement would rescale the event count without overturning the qualitative non-equilibrium enhancement.
  • The secondary shock's selectivity, perturbing $\mathrm{C}_2\mathrm{H}_6$ and $\mathrm{C}_2\mathrm{H}_4$ but not already-quenched HCN, suggests that relative abundances of shock products may record the entry-velocity and size distribution of the impacting population, a diagnostic future observations of Titan's lower atmosphere could exploit.
  • If entry chemistry is the dominant sub-100 km HCN source, Titan's HCN mixing ratios below 100 km should be reproducible from the meteoroid influx alone and should not follow the photochemical vertical profile; sounding or in situ measurements could test this directly.
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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 / 4 minor

Summary. The paper presents axisymmetric (labeled 3D) Athena++ hydrodynamic simulations of a 1-km, 10 km/s meteoroid entering Titan's atmosphere, combined with Cantera/GRI-Mech 3.0 chemical kinetics along test-particle trajectories. It reports bow-shock structure, a secondary shock behind the object, and chemical quenching controlled by adiabatic expansion cooling. The authors claim that non-equilibrium shock chemistry strongly enhances HCN production relative to equilibrium calculations, that a single event can remove water vapor efficiently while leaving N2 stable, that simulated yields agree with laser-plasma experiments, and that roughly 100 such entry events could account for the present HCN abundance on Titan, with emphasis on early Titan's history.

Significance. If the quantitative claims were supported, the paper would establish meteoroid entry as an important non-photochemical, abiotic source of prebiotic feedstock in Titan's lower atmosphere and would strengthen the case for time-dependent, non-equilibrium modeling over equilibrium approximations. The methodological core is credible and useful: the coupling of a shock-resolving hydrodynamic simulation to a kinetic network, the test-particle thermodynamic treatment, the iSALE-based check of the ideal-gas equation of state for the projectile, and the comparison with both Cassini abundances and Scattergood et al. (1989) laser experiments are all constructive steps. Credit is also due to the authors for explicitly discussing the uncertain rate coefficients in Section 4.1.4 and the azimuthal-resolution limitation in Section 2.1. However, the headline 'about 100 events' result is not currently supported: the present gas-phase inventory is not a cumulative reservoir in the presence of the photochemical loss timescale quoted by the authors themselves, and the dominant HCN formation rate coefficient carries an uncertainty far larger than the paper's own wording suggests.

major comments (3)
  1. [Sect. 4.1.3 and Table 1] The 'about 100 entry events' claim equates the integrated HCN production per event (1.5e11 mol, Table 1) with the present HCN column (1.4e13 mol) as though the atmosphere is a cumulative reservoir. The same section, however, states that the photochemical HCN timescale is only a few thousand years (Hébrard et al. 2012). With such a loss timescale, the present gas-phase abundance reflects the balance between recent production and loss, not the integral of all past production. A claim that ~100 ancient events supplied the present HCN inventory therefore requires either that those events occurred within the last few millennia, that HCN was stored in a condensed reservoir and later released, or that the loss timescale for the 100-km region is much longer than the quoted photochemical timescale. None of these options is specified. If the events are spread over 1e8 yr with the quoted 1000-yr loss timescale, the required rate is on the order of one event every ~10 yr, i.e., ~1e7 events, not 100. The Abstract and Section 5 repeat the 100-event claim without this caveat, so the paper's main quantitative conclusion is not currently supported.
  2. [Sect. 4.1.4 and Table 2] The paper states that the dominant HCN formation reaction, CH + N2 -> HCN + N (49% contribution), has experimental rate coefficients spanning nearly two orders of magnitude, but the actual numbers listed in Table 2 are 4.9e-14 to 280e-14 m3 molecule-1 s-1, while the adopted GRI-Mech value is 8.0e-17. Even if the intended comparison is only between the experimental extremes, the spread is a factor of roughly 60; relative to the adopted value, the discrepancy is orders of magnitude. No uncertainty propagation from Table 2 to the integrated yields in Table 1, to Figure 10, or to the inferred number of events is provided. Since the other two dominant reactions have no reliable high-temperature data, the quantitative HCN yield and the derived event count have an uncertainty that is large enough to change the central claim by an order of magnitude or more. The Conclusion should present the HCN yield and event count as a range, and Section 4.1.4 should reconcile the adopted rate with the cited experimental values or explain why the experimental values are not applicable at the shocked conditions.
  3. [Sect. 2.1 and Sect. 4.1.3] The derivation of the integrated yields in Table 1 is not described. Section 4.1.2 explains that Figure 10 uses cylindrical shells at three discrete radii (r0 = 1300, 1500, 1700 m), but the radial integration that produces the 'entire region heated' totals in Table 1 is not shown. The yield curve as a function of radius, the adopted outer cutoff, and the altitude extent over which the yields are integrated should be stated explicitly. Since the 100-event claim is a ratio of the Table 1 total to the observed column, the integration method is load-bearing for the headline result and needs to be reproducible from the text.
minor comments (4)
  1. [Title and Abstract; Sect. 2.1] The paper describes the simulations as three-dimensional, but Section 2.1 states that the azimuthal direction is resolved with only 2 cells and that axisymmetry is assumed. Please rephrase the title and abstract as 'axisymmetric' or 'quasi-3D' modeling, or justify the 2-cell azimuthal treatment as a full 3D calculation.
  2. [Sect. 4.1.2 and Fig. 10] The statement of 'good agreement' with Scattergood et al. (1989) is qualitative. The plotted yields differ among species by more than an order of magnitude, and no error bars or quantitative goodness-of-fit measure are provided. Please add a metric or a more precise statement of the agreement.
  3. [Sect. 2.2.2 and Eq. (8)] Equation (8) states tau_cool ~ Rcom/vent, but the text should define the reference temperature drop used to measure tau_cool and state whether the estimate is validated for all three cases in Figure 4 or only for the nearest streamline.
  4. [Sect. 4.1.3] The sentence citing Artemieva & Lunine (2005) says that a few billion years ago the number of entry events 'could have exceeded 1000.' Even setting aside the rate-uncertainty issue, 1000 events over several gigayears is far too low to maintain a steady-state HCN abundance with a few-thousand-year loss timescale, so this statement should be reconciled with the inventory calculation.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the HCN synthesis result is benchmarked against external Cassini abundances and Scattergood laser yields, with rates from the external GRI-Mech 3.0 network.

full rationale

The claimed derivation chain is self-contained: shock temperature and pressure histories come from independent Athena++ hydrodynamics, the kinetic network is the external GRI-Mech 3.0 mechanism evaluated in Cantera, and the Cassini abundances and Scattergood laser yields are external benchmarks applied after the chemistry is integrated. The '~100 events' number is a direct ratio of the Cassini HCN column (1.4e13 mol) to the simulated per-event yield (1.5e11 mol), with no parameter fitted to that target, so the headline claim is not forced by construction. The paper's own caveats about rate-coefficient scatter of nearly two orders for CH + N2 -> HCN + N and the absence of reference data for the other two dominant reactions are uncertainty statements, not circular steps. The skeptic's steady-state/loss-timescale objection to the '100 events' inference is a physical correctness concern, not a circularity: even if the inference is wrong, the yield calculation is not equivalent to its inputs. The only self-referential element is the citation of the authors' own impact-vapor model (Miyayama & Kobayashi 2024) in the Sect. 4.2 mass comparison; that is a non-load-bearing comparison for a separate mechanism and does not support the central HCN claim.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

The central claim rests on the fidelity of the flow solution, the applicability of GRI-Mech 3.0, and the test-particle assumption. None of these are fitted to the Cassini abundances; they are modeling axioms. The main free parameters are physical choices (radius, velocity, composition) and one numerical switch (the 6000 K equilibrium/non-equilibrium boundary).

free parameters (5)
  • Meteoroid radius Rcom = 1 km
    Chosen to exceed the Melosh breakup radius Rcrit ~ 700 m; sets the cooling timescale tau_cool ~ Rcom/vent and the heated atmospheric mass.
  • Entry velocity vent = 10 km/s
    Chosen near the gravitational lower limit (8.3 km/s) for Titan; controls shock temperature and secondary shock timing.
  • Initial atmospheric composition N2:CH4 = 9:1 with 7:3 variant
    Representative Titan lower-atmosphere mix; central to HCN yields, though the paper argues HCN is insensitive to this ratio.
  • Equilibrium/non-equilibrium switch temperature = 6000 K
    Above this T the GRI-Mech network extrapolates unreliable thermodynamic data, so the paper assumes equilibrium until cooling below 6000 K; choice affects early high-temperature composition.
  • Azimuthal cell count = 2 cells
    Coarse resolution dictated by Athena++ lacking cylindrical symmetry; makes the simulation effectively axisymmetric and suppresses wake instabilities.
assumptions (5)
  • domain assumption Ideal-gas hydrodynamics with gamma=1.4 describes both Titan's atmosphere and the solid meteoroid body.
    Used throughout Sect. 2. Validated against iSALE/Tillotson EOS only for density morphology, not for temperature or chemistry yields (Appendix B).
  • ad hoc to paper Azimuthal symmetry with 2 cells in phi captures the shock heating and streamline thermodynamics relevant to chemistry.
    Sect. 2.1 states non-axisymmetric instabilities are suppressed but are expected to occur in the wake; the paper neglects their chemical contribution.
  • ad hoc to paper GRI-Mech 3.0 is a valid kinetic network for the C/H/N/O system at post-shock temperatures up to 6000 K.
    Sect. 3.1 uses GRI-Mech 3.0; Sect. 4.1.4 admits limited C3 chemistry and order-of-magnitude rate uncertainties for the dominant HCN reactions.
  • domain assumption Gas cools purely by adiabatic expansion; heat conduction and radiation are negligible on the quenching timescale.
    Appendix A estimates tau_heat ~ 10^12 s and tau_rad ~ 10^5 s versus tau_cool ~ 10^-2 s, but radiative cooling near the meteoroid head may be underestimated by the blackbody scaling.
  • domain assumption A single test-particle thermodynamic history represents the chemical evolution of an entire cylindrical shell.
    Sect. 3.2 and Figs. 6 and 7 use T/P histories from discrete r0 positions; Appendix C shows only weak pressure and density dependence with altitude, but shell integration assumes the same history applies across a 20 m radial thickness and full height.

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Cite this review

Pith. "Pith review of Modeling Atmospheric Alteration on Titan: Hydrodynamics and Shock-Induced Chemistry of Meteoroid Entry." pith.science (2026). https://pith.science/paper/TWMEVV3M

@misc{pith2026250710369,
  author       = {Pith},
  title        = {Pith review of: Modeling Atmospheric Alteration on Titan: Hydrodynamics and Shock-Induced Chemistry of Meteoroid Entry},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TWMEVV3M}},
  note         = {Machine review of arXiv:2507.10369}
}
read the original abstract

Meteoroid entry into planetary atmospheres generates bow shocks, resulting in high-temperature gas conditions that drive chemical reactions. In this paper, we perform three-dimensional hydrodynamic simulations of meteoroid entry using the Athena++ code, coupled with chemistry calculations via Cantera to model the non-equilibrium chemistry triggered by atmospheric entry. Our aerodynamical simulations reveal the formation of complex shock structures, including secondary shock waves, which influence the thermodynamic evolution of the gas medium. By tracking thermodynamic parameters along streamlines, we analyze the effects of shock heating and subsequent expansion cooling on chemical reaction pathways. Our results demonstrate that chemical quenching occurs when the cooling timescale surpasses reaction rates, leading to the formation of distinct chemical products that deviate from equilibrium predictions. We show that the efficiency of molecular synthesis depends on the object\textquotesingle s size and velocity, influencing the composition of the post-entry gas mixture. Applying our model to Titan, we demonstrate that organic matter can be synthesized in the present environment of Titan. Also, we find that nitrogen, the dominant atmospheric component, remains stable, while water vapor is efficiently removed, a result inconsistent with equilibrium chemistry assumptions. Moreover, we compare our simulation results with laser experiments and find good agreement in chemical yields. Finally, we also evaluate the impact on Titan\textquotesingle s atmosphere as a whole, showing that meteoroid entry events could have played a significant role in supplying molecules such as HCN during early Titan\textquotesingle s history.

Figures

Figures reproduced from arXiv: 2507.10369 by the authors.

Figure 1
Figure 1. Schematic depiction of a bow shock flow. Mete￾oroid entry results in the bow shock wave (red line). The box illustrates stream lines around the object. Heated medium due to the bow shock immediately cools down with expansion process. Turbulent flow happens at the tail region through a growth of an instability, leading to mixing of material ab￾lated from the projectile with the atmosphere. with the comet and are comp… view at source ↗
Figure 2
Figure 2. Overview of the bow-shock formation. These panels show the zoomed-in views around the cometary body at t = 0.2, 0.3 and 1.0 s. Colors illustrate the changes in density (right half) and temperature (left half) caused by the bow shock. White arrows indicate the velocity direction, with lengths scaled to 1. acceleration. Each quantity with the subscript 0 indi￾cates its value at the surface. We set ρ0 = 1.2 kg/m3 , T =… view at source ↗
Figure 3
Figure 3. Tracking particles in bow-shock flow. In the left panel, the bow shock is illustrated in temperature and density with trajectories of each test particle included, each of which has an individual initial position. In the upper right panel, entropy increases for each particle are described as a function of time. In the bottom panel, the evolution of density and pressure are shown. The Gray curve and line are Hugoniot … view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: Cooling time scales via adiabatic expansion. A line illustrates the temperature of a test particle with an initial position R0 at each time. These colors shows three different simulations. As for the labels in this picture, Rc and v is the comet radius and velocity. In…
Figure 5
Figure 5. Figure 5: Temperature and mixing ratio of cometary and atmospheric components. In the right side (r > 0), red rep￾resents comet-derived components, while blue indicates at￾mospheric components. ing non-equilibrium chemical kinetics, thermodynamic properties, and combustion proce…
Figure 6
Figure 6. Figure 6: Time evolution of chemical species after shock heating. In this figure, the density of atmosphere, the entry velocity, and the altitude are set to 1.2 kg/m3 , 10 km/s and 100 km, respectively. Each color shows different chemical components, while the black curve displa…
Figure 7
Figure 7. Figure 7: illustrates two results of chemical evolu￾tion from different simulations: equilibrium and non￾equilibrium. Solid lines correspond to non-equilibrium case, and equilibrium case is represented as dashed lines. In the equilibrium calculations, chemical abundances are ass…
Figure 8
Figure 8. Figure 8: Dependence of initial fraction of chemical species. This figure is for a simulation with the same impact param￾eters (density, velocity, and altitude) as in [PITH_FULL_IMAGE:figures/full_fig_p010_8.png]
Figure 9
Figure 9. Figure 9 [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]
Figure 10
Figure 10. Figure 10: Chemical production rates from our simula￾tions and laser experiments by Scattergood et al. (1989). The black circles represent the experimental results. Col￾ored symbols show our simulation results at three different radial distances (r0) from the projectile, each co…
Figure 11
Figure 11. Figure 11: Temperature profile due to bow shock heating for an impactor with Rcom = 1 km. Both lines show the maximum temperature at each radial distance. The color difference corresponds to altitude of the comet. Black line indicates a fitting line of T ∝ r −2 . According to ou…
Figure 12
Figure 12. Figure 12: Impact induced vapor as a function of impact velocity. This figure is modified version of a figure from Miyayama & Kobayashi (2024). The amount of vapor MV is scaled by a projectile mass Mp. This assumes a verti￾cal collision between same material, and each color indi…
Figure 13
Figure 13. Figure 13: Two density profiles by solid and ideal-gas EoS. Right and left panels show density color maps by using different EoS-model–the ideal-gas EoS (a) and the solid EoS (b). Meteoroid bodies move with an entry velocity vent = 20 km/s to bottom side of medium with homogeneo…
Figure 14
Figure 14. Figure 14: Altitude dependence of the chemistry. Fig. (a) indicates the results for a test particle initially located at (r0, z0) = (1500 m, 60 km), and Fig. (b) for one initially located at (r0, z0) = (1500 m, 40 km) [PITH_FULL_IMAGE:figures/full_fig_p020_14.png]

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Works this paper leans on

79 extracted references · 42 canonical work pages

  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]

    ͆ t2<P?Y R[ ayzk ŏţ_M

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -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 o...

    work page 2017

  4. [4]

    1985, Lunar and Planetary Science Conference Proceedings, 90, C545

    Abe , Y., & Matsui , T. 1985, Lunar and Planetary Science Conference Proceedings, 90, C545

    work page 1985

  5. [5]

    1988, Journal of the Atmospheric Sciences, 45, 3081, 10.1175/1520-0469(1988)045<3081:EOAIGH>2.0.CO;2

    ---. 1988, Journal of the Atmospheric Sciences, 45, 3081, 10.1175/1520-0469(1988)045<3081:EOAIGH>2.0.CO;2

    doi:10.1175/1520-0469(1988)045 1988

  6. [6]

    A., Ruppel, H

    Amsden, A. A., Ruppel, H. M., & Hirt, C. W. 1980, SALE: a simplified ALE computer program for fluid flow at all speeds, 10.2172/5176006

    work page doi:10.2172/5176006 1980

  7. [7]

    Artemieva , N., & Lunine , J. I. 2005, , 175, 522, 10.1016/j.icarus.2004.12.005

    work page doi:10.1016/j.icarus.2004.12.005 2005

  8. [8]

    Benlow , A., & Meadows , A. J. 1977, , 46, 293, 10.1007/BF00644376

    work page doi:10.1007/bf00644376 1977

Show all 79 references
  1. [9]

    L., & Walker , J

    Chameides , W. L., & Walker , J. C. G. 1981, Origins of Life, 11, 291, 10.1007/BF00931483

    1981 doi

  2. [10]

    1992, , 355, 125, 10.1038/355125a0

    Chyba , C., & Sagan , C. 1992, , 355, 125, 10.1038/355125a0

    1992 doi

  3. [11]

    F., Thomas , P

    Chyba , C. F., Thomas , P. J., Brookshaw , L., & Sagan , C. 1990, Science, 249, 366, 10.1126/science.11538074

    1990 doi

  4. [12]

    F., Thomas , P

    Chyba , C. F., Thomas , P. J., & Zahnle , K. J. 1993, , 361, 40, 10.1038/361040a0

    1993 doi

  5. [13]

    1998, , 336, L85

    Coustenis , A., Salama , A., Lellouch , E., et al. 1998, , 336, L85

    1998

  6. [14]

    E., Caldwell , J

    Danielson , R. E., Caldwell , J. J., & Larach , D. R. 1973, , 20, 437, 10.1016/0019-1035(73)90016-X

    1973 doi

  7. [15]

    G., Hartman , H., & Watkins , G

    Fegley , Jr., B., Prinn , R. G., Hartman , H., & Watkins , G. H. 1986, , 319, 305, 10.1038/319305a0

    1986 doi

  8. [16]

    E., & Chyba , C

    Flowers , E. E., & Chyba , C. F. 2023, , 4, 127, 10.3847/PSJ/acdfc9

    2023 doi

  9. [17]

    2005, , 435, 397, 10.1051/0004-6361:20042201

    Foglizzo , T., Galletti , P., & Ruffert , M. 2005, , 435, 397, 10.1051/0004-6361:20042201

    2005 doi

  10. [18]

    2005, , 438, 785, 10.1038/nature04314

    Fulchignoni , M., Ferri , F., Angrilli , F., et al. 2005, , 438, 785, 10.1038/nature04314

    2005 doi

  11. [19]

    2005, , 433, 842, 10.1038/nature03360

    Genda , H., & Abe , Y. 2005, , 433, 842, 10.1038/nature03360

    2005 doi

  12. [20]

    V., Ivanov , B

    Gerasimov , M. V., Ivanov , B. A., Yakovlev , O. I., & Dikov , Y. P. 1998, Earth Moon and Planets, 80, 209, 10.1023/A:1006322032494

    1998 doi

  13. [21]

    G., Moffat , H

    Goodwin , D. G., Moffat , H. K., Schoegl , I., Speth , R. L., & Weber , B. W. 2023, Cantera: An Object-oriented Software Toolkit for Chemical Kinetics, Thermodynamics, and Transport Processes , 3.0.0, Zenodo, 10.5281/zenodo.8137090

    2023 doi

  14. [22]

    L., Abe , Y., & Sugita , S

    Hashimoto , G. L., Abe , Y., & Sugita , S. 2007, Journal of Geophysical Research (Planets), 112, E05010, 10.1029/2006JE002844

    2007 doi

  15. [23]

    C., Bergeat , A., & Hickson , K

    H \'e brard , E., Dobrijevic , M., Loison , J. C., Bergeat , A., & Hickson , K. M. 2012, , 541, A21, 10.1051/0004-6361/201218837

    2012 doi

  16. [24]

    H \"o rst , S. M. 2017, Journal of Geophysical Research (Planets), 122, 432, 10.1002/2016JE005240

    2017 doi

  17. [25]

    2011, , 741, L10, 10.1088/2041-8205/741/1/L10

    Ishimaru , R., Sekine , Y., Matsui , T., & Mousis , O. 2011, , 741, L10, 10.1088/2041-8205/741/1/L10

    2011 doi

  18. [26]

    2010, , 210, 411, 10.1016/j.icarus.2010.06.016

    Ishimaru , R., Senshu , H., Sugita , S., & Matsui , T. 2010, , 210, 411, 10.1016/j.icarus.2010.06.016

    2010 doi

  19. [27]

    P., Rae , A

    Itcovitz , J. P., Rae , A. S. P., Citron , R. I., et al. 2022, PSJ, 3, 115, 10.3847/PSJ/ac67a9

    2022 doi

  20. [28]

    1997, International Journal of Impact Engineering, 20, 411, https://doi.org/10.1016/S0734-743X(97)87511-2

    Ivanov, B., Deniem, D., & Neukum, G. 1997, International Journal of Impact Engineering, 20, 411, https://doi.org/10.1016/S0734-743X(97)87511-2

    1997 doi

  21. [29]

    D., & Lewis , J

    Jones , T. D., & Lewis , J. S. 1987, , 72, 381, 10.1016/0019-1035(87)90181-3

    1987 doi

  22. [30]

    2023, , 945, 39, 10.3847/1538-4357/acb7ea

    Kitajima , K., & Inutsuka , S.-i. 2023, , 945, 39, 10.3847/1538-4357/acb7ea

    2023 doi

  23. [31]

    Krasnopolsky , V. A. 2009, , 201, 226, 10.1016/j.icarus.2008.12.038

    2009 doi

  24. [32]

    2023, , 957, 67, 10.3847/1538-4357/acfe0a

    Kurosaki , K., Hori , Y., Ogihara , M., & Kunitomo , M. 2023, , 957, 67, 10.3847/1538-4357/acfe0a

    2023 doi

  25. [33]

    2013, Origins of Life and Evolution of the Biosphere, 43, 221, 10.1007/s11084-013-9339-0

    Kurosawa , K., Sugita , S., Ishibashi , K., et al. 2013, Origins of Life and Evolution of the Biosphere, 43, 221, 10.1007/s11084-013-9339-0

    2013 doi

  26. [34]

    2015, , 257, 290, 10.1016/j.icarus.2015.05.007

    Kuwahara , H., & Sugita , S. 2015, , 257, 290, 10.1016/j.icarus.2015.05.007

    2015 doi

  27. [35]

    D., & Lifshitz , E

    Landau , L. D., & Lifshitz , E. M. 1959, in Fluid mechanics (Oxford: Pergamon Press)

    1959

  28. [36]

    A., & Ahrens , T

    Lange , M. A., & Ahrens , T. J. 1982, , 51, 96, 10.1016/0019-1035(82)90031-8

    1982 doi

  29. [37]

    C., H \'e brard , E., Dobrijevic , M., et al

    Loison , J. C., H \'e brard , E., Dobrijevic , M., et al. 2015, , 247, 218, 10.1016/j.icarus.2014.09.039

    2015 doi

  30. [38]

    E., Zahnle , K., Marley , M

    Lupu , R. E., Zahnle , K., Marley , M. S., et al. 2014, , 784, 27, 10.1088/0004-637X/784/1/27

    2014 doi

  31. [39]

    P., Scattergood , T

    McKay , C. P., Scattergood , T. W., Pollack , J. B., Borucki , W. J., & van Ghyseghem , H. T. 1988, , 332, 520, 10.1038/332520a0

    1988 doi

  32. [40]

    Melosh , H. J. 1981, in Multi-ring basins: Formation and Evolution, ed. R. B. Merill & P. H. Schultz , 29--35

    1981

  33. [41]

    Melosh , H. J. 2007, M&PS, 42, 2079, 10.1111/j.1945-5100.2007.tb01009.x

    2007

  34. [42]

    1997, Int

    Miller , J., & Walch , S. 1997, Int. J. Chem. Kinet., 29, 253

    1997

  35. [43]

    E., Foustoukos , D

    Miller , K. E., Foustoukos , D. I., Cody , G. D., & Alexander , C. M. O. 2025, , 390, 38, 10.1016/j.gca.2024.12.026

    2025 doi

  36. [44]

    2024, , 688, A103, 10.1051/0004-6361/202450177

    Miyayama , R., & Kobayashi , H. 2024, , 688, A103, 10.1051/0004-6361/202450177

    2024 doi

  37. [45]

    M., et al

    Moreno , R., Lellouch , E., Lara , L. M., et al. 2012, , 221, 753, 10.1016/j.icarus.2012.09.006

    2012 doi

  38. [46]

    M., Gerasimov , M

    Mukhin , L. M., Gerasimov , M. V., & Safonova , E. N. 1989, , 340, 46, 10.1038/340046a0

    1989 doi

  39. [47]

    B., Atreya , S

    Niemann , H. B., Atreya , S. K., Bauer , S. J., et al. 2005, , 438, 779, 10.1038/nature04122

    2005 doi

  40. [48]

    R., & Melosh , H

    Passey , Q. R., & Melosh , H. J. 1980, , 42, 211, 10.1016/0019-1035(80)90072-X

    1980 doi

  41. [49]

    Pearce , B. K. D., Molaverdikhani , K., Pudritz , R. E., Henning , T., & H \'e brard , E. 2020, , 901, 110, 10.3847/1538-4357/abae5c

    2020 doi

  42. [50]

    Pearce , B. K. D., H \"o rst , S. M., Cline , C. J., et al. 2024, , 5, 68, 10.3847/PSJ/ad283e

    2024 doi

  43. [51]

    J., & Bildsten , L

    Prust , L. J., & Bildsten , L. 2024, , 527, 2869, 10.1093/mnras/stad3405

    2024 doi

  44. [52]

    1996, Chem

    Rodgers , A., & Smith , G. 1996, Chem. Phys. Lett., 253, 313

    1996

  45. [53]

    W., McKay , C

    Scattergood , T. W., McKay , C. P., Borucki , W. J., et al. 1989, , 81, 413, 10.1016/0019-1035(89)90061-4

    1989 doi

  46. [54]

    2007, , 186, 462, 10.1016/j.icarus.2006.09.002

    Schaefer , L., & Fegley , B. 2007, , 186, 462, 10.1016/j.icarus.2006.09.002

    2007 doi

  47. [55]

    2010, , 208, 438, 10.1016/j.icarus.2010.01.026

    ---. 2010, , 208, 438, 10.1016/j.icarus.2010.01.026

    2010 doi

  48. [56]

    E., Sari , R., & Yalinewich , A

    Schlichting , H. E., Sari , R., & Yalinewich , A. 2015, , 247, 81, 10.1016/j.icarus.2014.09.053

    2015 doi

  49. [57]

    2011, Nature Geoscience, 4, 359, 10.1038/ngeo1147

    Sekine , Y., Genda , H., Sugita , S., Kadono , T., & Matsui , T. 2011, Nature Geoscience, 4, 359, 10.1038/ngeo1147

    2011 doi

  50. [58]

    2009, , 44, 1095, 10.1111/j.1945-5100.2009.tb01209.x

    Shuvalov , V. 2009, , 44, 1095, 10.1111/j.1945-5100.2009.tb01209.x

    2009

  51. [59]

    u hrt , E., de Niem , D., & W \

    Shuvalov , V., K \"u hrt , E., de Niem , D., & W \"u nnemann , K. 2014, , 98, 120, 10.1016/j.pss.2013.08.018

    2014 doi

  52. [60]

    2017, , 147, 38, 10.1016/j.pss.2017.05.011

    Shuvalov , V., Svetsov , V., Popova , O., & Glazachev , D. 2017, , 147, 38, 10.1016/j.pss.2017.05.011

    2017 doi

  53. [61]

    V., & Artemieva , N

    Shuvalov , V. V., & Artemieva , N. A. 2002, , 50, 181, 10.1016/S0032-0633(01)00079-4

    2002 doi

  54. [62]

    A., Boslough , M., Hocking , W

    Silber , E. A., Boslough , M., Hocking , W. K., Gritsevich , M., & Whitaker , R. W. 2018, Advances in Space Research, 62, 489, 10.1016/j.asr.2018.05.010

    2018 doi

  55. [63]

    A., Hocking , W

    Silber , E. A., Hocking , W. K., Niculescu , M. L., Gritsevich , M., & Silber , R. E. 2017, , 469, 1869, 10.1093/mnras/stx923

    2017 doi

  56. [64]

    M., Tomida , K., White , C

    Stone , J. M., Tomida , K., White , C. J., & Felker , K. G. 2020, , 249, 4, 10.3847/1538-4365/ab929b

    2020 doi

  57. [65]

    Strobel , D. F. 2010, , 208, 878, 10.1016/j.icarus.2010.03.003

    2010 doi

  58. [66]

    Svetsov , V. V. 2007, Solar System Research, 41, 28, 10.1134/S0038094607010030

    2007 doi

  59. [67]

    2016, , 589, A10, 10.1051/0004-6361/201527629

    Thun , D., Kuiper , R., Schmidt , F., & Kley , W. 2016, , 589, A10, 10.1051/0004-6361/201527629

    2016 doi

  60. [68]

    Tillotson , J. H. 1962, Metallic Equations of State For Hypervelocity Impact , General Atomic Report GA-3216. 1962. Technical Report

    1962

  61. [69]

    2007, , 188, 120, 10.1016/j.icarus.2006.10.031

    Vinatier , S., B \'e zard , B., Fouchet , T., et al. 2007, , 188, 120, 10.1016/j.icarus.2006.10.031

    2007 doi

  62. [70]

    A., et al

    Vinatier , S., B \'e zard , B., Nixon , C. A., et al. 2010, , 205, 559, 10.1016/j.icarus.2009.08.013

    2010 doi

  63. [71]

    V., Klippenstein , S

    Vuitton , V., Yelle , R. V., Klippenstein , S. J., H \"o rst , S. M., & Lavvas , P. 2019, , 324, 120, 10.1016/j.icarus.2018.06.013

    2019 doi

  64. [72]

    2016, , 829, 79, 10.3847/0004-637X/829/2/79

    Willacy , K., Allen , M., & Yung , Y. 2016, , 829, 79, 10.3847/0004-637X/829/2/79

    2016 doi

  65. [73]

    S., & Melosh , H

    W \"u nnemann , K., Collins , G. S., & Melosh , H. J. 2006, , 180, 514, 10.1016/j.icarus.2005.10.013

    2006 doi

  66. [74]

    C., Kral , Q., & Sinclair , C

    Wyatt , M. C., Kral , Q., & Sinclair , C. A. 2020, , 491, 782, 10.1093/mnras/stz3052

    2020 doi

  67. [75]

    F., & Pollack , J

    Zahnle , K., Kasting , J. F., & Pollack , J. B. 1990, , 84, 502, 10.1016/0019-1035(90)90050-J

    1990 doi

  68. [76]

    B., Grinspoon , D., & Dones , L

    Zahnle , K., Pollack , J. B., Grinspoon , D., & Dones , L. 1992, , 95, 1, 10.1016/0019-1035(92)90187-C

    1992 doi

  69. [77]

    2003, , 163, 263, 10.1016/S0019-1035(03)00048-4

    Zahnle , K., Schenk , P., Levison , H., & Dones , L. 2003, , 163, 263, 10.1016/S0019-1035(03)00048-4

    2003 doi

  70. [78]

    J., Lupu , R., Catling , D

    Zahnle , K. J., Lupu , R., Catling , D. C., & Wogan , N. 2020, , 1, 11, 10.3847/PSJ/ab7e2c

    2020 doi

  71. [79]

    B., & Raizer , Y

    Zel'dovich , Y. B., & Raizer , Y. P. 1967, Physics of shock waves and high-temperature hydrodynamic phenomena

    1967

Pith tools

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