Laboratory measurement of volatile ice vapor pressures with a quartz crystal microbalance

Grundy, W.M.; Tegler, S.C.; Steckloff, J.K.; Tan, S.P.; Loeffler, M.J.; Jasko, A.V.; Koga, K.J.; Blakley, B.P.; Raposa, S.M.; Engle, A.E.; Thieberger, C.L.; Hanley, J.; Lindberg, G.E.; Gomez, M.D.; Madden-Watson, A.O.

doi:10.1016/j.icarus.2023.115767

Cited by 9 publications

(10 citation statements)

References 46 publications

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“…Along the sublimation at 27 K, the mass spectrometer recorded a maximum pressure of 9.5 × 10 −5 Pa (P gauge ). From the plot obtained in Grundy et al (2024) for this temperature, a pressure of 8.2 × 10 −5 Pa would correspond approximately with that actually experienced by the QCMB surface in our experimental setup.…”

Section: Theoretical Expression To Obtain the Vapor Pressuresupporting

confidence: 54%

“…Vapor pressure is a relevant quantity that is used to calculate the escape of molecules from KBOs and TNOs, and this, in turn, has an important weight on the composition of both ices and atmospheres of these solar system objects. In Figure 6, the vapor pressures for CO, CH 4 , and N 2 obtained in our laboratory have been compared with the previous results reported by L-F and F-S, which needed to have been extrapolated to the range considered in this study, together with the very recent reported by Grundy et al (2024).…”

Section: Application To Volatiles On Cold Bodies In the Solar Systemmentioning

confidence: 95%

“…The vapor pressures that have been included in the present study for CO and CH 4 were obtained through experimentation and cover temperatures between 20 and 50 K. Together with the work of Grundy et al (2024) this means that they better represent the values found on KBOs. In addition, data for C 2 H 6 are also presented covering a temperature range of around 20 K above the temperatures found in the solar system context, but closer than the experimental data referred to in the study by F-S.…”

Section: Introductionmentioning

confidence: 99%

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Experimental Vapor Pressure Determination for C₂H₄, C₂H₆, CH₃OH, CH₄, CO, CO₂, H₂O, and N₂ Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

Millán,

Luna,

Domingo

et al. 2024

ApJ

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Vapor pressure is a relevant quantity that is necessary in order to improve the study of the atmosphere dynamics that take place within astrophysical scenarios. The aim of this study was to obtain the vapor pressure values of the following molecules: C2H4, C2H6, CH3OH, CH4, CO, CO2, H2O, and N2 through experimentation, as well as to determine their empirical relationship with the temperature, applying the results to the persistence of volatiles in trans-Neptunian objects (TNOs) and Kuiper Belt objects (KBOs). The experimental determination was performed by measuring the sublimation rate for each molecule at different temperatures. The Hertz–Knudsen equation was used to obtain the vapor pressures for the aforementioned molecules, taking the necessary considerations into account, and the sublimation rate was measured using a quartz crystal microbalance. In order to check the validity of the methods used, the results obtained for water ice were compared with those of previous studies from the literature. The values obtained for CO, N2, and CH4 are of particular interest in the study of the TNOs' and KBOs' atmosphere composition. The results of this study improve the understanding of the surface and atmospheric composition of objects in the cold scenarios of the solar system, in particular, in KBOs and TNOs.

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Section: Theoretical Expression To Obtain the Vapor Pressuresupporting

confidence: 54%

Section: Application To Volatiles On Cold Bodies In the Solar Systemmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Experimental Vapor Pressure Determination for C₂H₄, C₂H₆, CH₃OH, CH₄, CO, CO₂, H₂O, and N₂ Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

Millán,

Luna,

Domingo

et al. 2024

ApJ

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“…We present absorbance spectra of CO + CO 2 ice mixtures measured in the Astrophysical Materials Laboratory at Northern Arizona University (Tegler et al 2024). These cocondensed ices were made by mixing CO and CO 2 gases at room temperature before condensing as thin films on a gold mirror held at 20 K (see Tegler et al 2024;Grundy et al 2024a, for more details on laboratory procedures). We also compared the Ariel data to spectra of radiolyzed CO 2 ices processed by 100 keV protons (Raut & Baragiola 2013).…”

Section: Methodsmentioning

confidence: 99%

JWST Reveals CO Ice, Concentrated CO₂ Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior

Cartwright,

Holler,

Grundy

et al. 2024

ApJL

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The Uranian moon Ariel exhibits a diversity of geologically young landforms, with a surface composition rich in CO2 ice. The origin of CO2 and other species, however, remains uncertain. We report observations of Ariel’s leading and trailing hemispheres, collected with NIRSpec (2.87–5.10 μm) on the James Webb Space Telescope. These data shed new light on Ariel's spectral properties, revealing a double-lobed CO2 ice scattering peak centered near 4.20 and 4.25 μm, with the 4.25 μm lobe possibly representing the largest CO2 Fresnel peak yet observed in the solar system. A prominent 4.38 μm 13CO2 ice feature is also present, as is a 4.90 μm band that results from 12CO2 ice. The spectra reveal a 4.67 μm 12CO ice band and a broad 4.02 μm band that might result from carbonate minerals. The data confirm that features associated with CO2 and CO are notably stronger on Ariel’s trailing hemisphere compared to its leading hemisphere. We compared the detected CO2 features to synthetic spectra of CO2 ice and mixtures of CO2 with CO, H2O, and amorphous carbon, finding that CO2 could be concentrated in deposits thicker than ∼10 mm on Ariel’s trailing hemisphere. Comparison to laboratory data indicates that CO is likely mixed with CO2. The evidence for thick CO2 ice deposits and the possible presence of carbonates on both hemispheres suggests that some carbon oxides could be sourced from Ariel’s interior, with their surface distributions modified by charged particle bombardment, sublimation, and seasonal migration of CO and CO2 from high to low latitudes.

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“…Irradiation of transparent substrates may result in electrostatic charging and changes in the substrate properties (Clark & Crawford 1973;Teolis et al 2007). Third, it is possible to use a quartz crystal microbalance (QCM) as the substrate in reflectance geometry and obtain information about the density of the ice (Westley et al 1998;Loeffler et al 2006) and its vapor pressure (Hudson et al 2022;Grundy et al 2024). Because of these advantages, we decided to modify the algorithm by Gerakines & Hudson (2020a) for transmission geometry to work in reflection geometry.…”

Section: Introductionmentioning

confidence: 99%

Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy

Tegler,

Grundy,

Loeffler

et al. 2024

Planet. Sci. J.

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Laboratory-derived optical constants are essential for identifying ices and measuring their relative abundances on solar system objects. Almost all optical constants of ices important to planetary science come from experiments with transmission geometries. Here we describe our new experimental setup and the modification of an iterative algorithm in the literature to measure the optical constants of ices from experiments with reflectance geometries. We apply our techniques to CH4 ice and H2O ice samples and find good agreement between our values and those in the literature, except for one CH4 band in the literature that likely suffers from saturation. The work we present here demonstrates that labs with reflectance geometries can generate optical constants essential for the proper analysis of near- and mid-infrared spectra of outer solar system objects such as those obtained with the James Webb Space Telescope.

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Laboratory measurement of volatile ice vapor pressures with a quartz crystal microbalance

Cited by 9 publications

References 46 publications

Experimental Vapor Pressure Determination for C₂H₄, C₂H₆, CH₃OH, CH₄, CO, CO₂, H₂O, and N₂ Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

Experimental Vapor Pressure Determination for C₂H₄, C₂H₆, CH₃OH, CH₄, CO, CO₂, H₂O, and N₂ Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

JWST Reveals CO Ice, Concentrated CO₂ Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior

Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy

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Laboratory measurement of volatile ice vapor pressures with a quartz crystal microbalance

Cited by 9 publications

References 46 publications

Experimental Vapor Pressure Determination for C2H4, C2H6, CH3OH, CH4, CO, CO2, H2O, and N2 Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

Experimental Vapor Pressure Determination for C2H4, C2H6, CH3OH, CH4, CO, CO2, H2O, and N2 Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

JWST Reveals CO Ice, Concentrated CO2 Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior

Optical Constants of Ices Important to Planetary Science from Laboratory Reflectance Spectroscopy

Contact Info

Product

Resources

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Experimental Vapor Pressure Determination for C₂H₄, C₂H₆, CH₃OH, CH₄, CO, CO₂, H₂O, and N₂ Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

Experimental Vapor Pressure Determination for C₂H₄, C₂H₆, CH₃OH, CH₄, CO, CO₂, H₂O, and N₂ Molecules for Astrophysical Relevant Temperatures. Implications for the Presence of Volatiles in Kuiper Belt Objects and Trans-Neptunian Objects

JWST Reveals CO Ice, Concentrated CO₂ Deposits, and Evidence for Carbonates Potentially Sourced from Ariel’s Interior