Erratum: Liquid water on Enceladus from observations of ammonia and 40Ar in the plume

Waite, J. H.; Lewis, William S.; Magee, B.; Lunine, Jonathan I.; McKinnon, William B.; Glein, Christopher R.; Mousis, O.; Young, D. T.; Brockwell, T.; Westlake, J. H.; Nguyen, M.-J.; Teolis, B. D.; Niemann, H. B.; McNutt, R. L.; Perry, Mark; Ip, Wing-Huen

doi:10.1038/nature08352

Nature

2009

DOI: 10.1038/nature08352

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Erratum: Liquid water on Enceladus from observations of ammonia and 40Ar in the plume

J. H. Waite¹,

William S. Lewis²,

B. Magee³

et al.

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Cited by 7 publications

(9 citation statements)

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“…We assume infrequent gas-phase collisions between original species after impact, consistent with low plume or atmospheric densities observed at Enceladus and Titan [3]. The fractions for H 2 , O 2 , H 2 O, CO, and CO 2 production as a function of impact energy are consistent with INMS data reported by Waite and colleagues [2], with two exceptions: (i) larger release of O 2 as a function of impact energy from our simulations (all impactors), and (ii) CO 2 fraction is larger and remains inversely proportional to the impact velocity through E5 (i.e., no inflection point between E3 and E5). Both cases are influenced by a underpredicted Ti-O surface bond energy in the ReaxFF description.…”

supporting

confidence: 77%

“…Accurate fractions and rates of change predicted for H 2 O, H 2 , and CO production, compared to INMS data from Ref. [2]. Correct trend for CO 2 and O 2 production, except for a decrease in CO 2 between E3-E5 and albeit overpredicted magnitudes.…”

mentioning

confidence: 99%

“…Here, we focus on predicting the influence of specific factors on the interpretation of INMS data: namely, the effect of encounter velocity (energy) on molecular fragmentation processes, the molecular topology effects from different isomers on fragmentation patterns, the INMS TiO 2 surface reactivity or composition changes from HV impact of ice clusters or cosmic dust, and the probability of physisorbed or chemisorbed species on the TiO 2 INMS surfaces. The results are analyzed using INMS data at the encounter velocities E2 (8 km=s), E3 (14:41 km=s), and E5 (17:73 km=s) [2] with Enceladus' plume, and the October 26 2004 Titan fly-by at $6 km=s [4].…”

mentioning

confidence: 99%

“…[2]. Correct trend for CO 2 and O 2 production, except for a decrease in CO 2 between E3-E5 and albeit overpredicted magnitudes.…”

mentioning

confidence: 99%

“…Enceladus' plume has been sampled during five fly-bys (E1-E5) and found to be composed predominantly of H 2 O, with CO 2 as the second most abundant species. The latest encounters have yielded data with high signal-to-noise ratios, enabling the identification of trace species, including complex organics such as benzene, that were not distinguishable in INMS data from the earlier fly-bys [2]. Cassini's INMS is a quadrupole mass spectrometer equipped with two separate ion sources, a closed source and an open source.…”

mentioning

confidence: 99%

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Hypervelocity Impact Effect of Molecules from Enceladus’ Plume and Titan’s Upper Atmosphere on NASA’s Cassini Spectrometer from Reactive Dynamics Simulation

Jaramillo-Botero

Cheng

et al. 2012

Phys. Rev. Lett.

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The NASA/ESA Cassini probe of Saturn analyzed the molecular composition of plumes emanating from one of its moons, Enceladus, and the upper atmosphere of another, Titan. However, interpretation of this data is complicated by the hypervelocity (HV) flybys of up to $18 km= sec that cause substantial molecular fragmentation. To interpret this data we use quantum mechanical based reactive force fields to simulate the HV impact of various molecular species and ice clathrates on oxidized titanium surfaces mimicking those in Cassini's neutral and ion mass spectrometer (INMS). The predicted velocity dependent fragmentation patterns and composition mixing ratios agree with INMS data providing the means for identifying the molecules in the plume. We used our simulations to predict the surface damage from the HV impacts on the INMS interior walls, which we suggest acts as a titanium sublimation pump that could alter the instrument's readings. These results show how the theory can identify chemical events from hypervelocity impacts in space plumes and atmospheres, providing in turn clues to the internal structure of the corresponding sources (e.g., Enceladus). This may be valuable in steering modifications in future missions. The Cassini Saturn orbiter has returned a wealth of data from its Ion and Neutral Mass Spectrometer (INMS) [1] on the composition of Titan's upper atmosphere and the plumes of Enceladus. Enceladus' plume has been sampled during five fly-bys (E1-E5) and found to be composed predominantly of H 2 O, with CO 2 as the second most abundant species. The latest encounters have yielded data with high signal-to-noise ratios, enabling the identification of trace species, including complex organics such as benzene, that were not distinguishable in INMS data from the earlier fly-bys [2]. Cassini's INMS is a quadrupole mass spectrometer equipped with two separate ion sources, a closed source and an open source. The composition of the Enceladus plumes and the upper atmosphere of Titan have been obtained primarily with the closed source, which is made up of a spherical titanium (Ti) antechamber connected to a hot filament electron impact ionizer by means of a transfer tube [1]. The 70 eV ionizer fragments and ionizes the incident molecules before they are focused in the quadrupole for mass analysis. Atmospheric gas molecules enter the antechamber through an entrance aperture, and are thermalized through collisions with the antechamber walls before entering the ionizer. This arrangement achieves a direction-dependent ram enhancement of the gas pressure in the antechamber above that of the ambient gas due to the high velocity of the spacecraft [3].Interpretation of the INMS spectra requires careful deconvolution of a complex pattern of mass peaks that represent the parent species and dissociative ionization products resulting from the ionizer and from hypervelocity (HV) impacts with the INMS chamber walls. The fundamental physical and chemical properties of HV molecular collisions are largely unknown for the species of ...

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supporting

confidence: 77%

mentioning

confidence: 99%

mentioning

confidence: 99%

“…[2]. Correct trend for CO 2 and O 2 production, except for a decrease in CO 2 between E3-E5 and albeit overpredicted magnitudes.…”

mentioning

confidence: 99%

mentioning

confidence: 99%

See 3 more Smart Citations

Hypervelocity Impact Effect of Molecules from Enceladus’ Plume and Titan’s Upper Atmosphere on NASA’s Cassini Spectrometer from Reactive Dynamics Simulation

Jaramillo-Botero

Cheng

et al. 2012

Phys. Rev. Lett.

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An inorganic silicate simulant to represent the interior of enceladus

Hamp,

Olsson-Francis,

Schwenzer

et al. 2024

Planetary and Space Science

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Partitioning of Crystalline and Amorphous Phases During Freezing of Simulated Enceladus Ocean Fluids

Fox-Powell

Cousins

2021

JGR Planets

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Saturn's ice‐covered moon Enceladus may contain the requisite conditions for life. Its potentially habitable subsurface ocean is vented into space as large cryovolcanic plumes that can be sampled by spacecraft, acting as a window to the ocean below. However, little is known about how Enceladus’ ocean fluids evolve as they freeze. Using cryo‐imaging techniques, we investigated solid phases produced by freezing simulated Enceladean ocean fluids at endmember cooling rates. Our results show that under flash‐freezing conditions (>10 K s−1), Enceladus‐relevant fluids undergo segregation, whereby the precipitation of ice templates the formation of brine vein networks. The high solute concentrations and confined nature of these brine veins means that salt crystallization is kinetically inhibited and glass formation (vitrification) can occur at lower cooling rates than typically required for vitrification of a bulk solution. Crystalline salts also form if flash‐frozen fluids are re‐warmed. The 10 µm‐scale distribution of salt phases produced by this mechanism differs markedly from that of gradually cooled (∼1 K min−1) fluids, showing that they inherit a textural signature of their formation conditions. The mineralogy of cryogenic carbonates can be used as a probe for cooling rate and parent fluid pH. Our findings reveal possible endmember routes for solid phase production from Enceladus’ ocean fluids and mechanisms for generating compositional heterogeneity within ice particles on a sub‐10 µm scale. This has implications for understanding how Enceladus' ocean constituents are incorporated into icy particles and delivered to space.

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Erratum: Liquid water on Enceladus from observations of ammonia and 40Ar in the plume

Cited by 7 publications

References 1 publication

Hypervelocity Impact Effect of Molecules from Enceladus’ Plume and Titan’s Upper Atmosphere on NASA’s Cassini Spectrometer from Reactive Dynamics Simulation

Hypervelocity Impact Effect of Molecules from Enceladus’ Plume and Titan’s Upper Atmosphere on NASA’s Cassini Spectrometer from Reactive Dynamics Simulation

An inorganic silicate simulant to represent the interior of enceladus

Partitioning of Crystalline and Amorphous Phases During Freezing of Simulated Enceladus Ocean Fluids

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