Density and index of refraction of water ice films vapor deposited at low temperatures

Westley, M. S.; Baratta, G. A.; Baragiola, R. A.

doi:10.1063/1.475730

Cited by 178 publications

(149 citation statements)

References 55 publications

(75 reference statements)

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“…This amplitude change can have different reasons; a loss of coherence of the reflected light because of surface roughness, cracks, and/or wide boundaries (Baragiola 2003;Howett et al 2007;Romanescu et al 2010). The distance A82, page 2 of 5 between subsequent minima and maxima is constant within 1% indicating that the density of the porous ASW does not change significantly during deposition (Westley et al 1998).…”

Section: Experimental Methodsmentioning

confidence: 99%

“…For layered structures (Fig. 6), the reflection coefficient R can be written as a function of the Fresnel reflection coefficients according to the relation (Westley et al 1998;Dohnalek et al 2003):…”

Section: Discussionmentioning

confidence: 99%

“…To exclude the influence of the gas deposited on the backside of the substrate, we use the Si substrate that is opaque to the laser wavelength. We use n 0 = 1 for vacuum, n 1 = 1.19 for porous ASW at 15 K (extrapolated from the data reported in Dohnalek et al 2003), and n 1 = 1.29 for less-porous ASW (Westley et al 1998). A quantitative characterization of the ice thickness during deposition is possible by correlating the interference fringe pattern of subsequent minima and maxima (m) and the corresponding deposition time.…”

Section: Experimental Methodsmentioning

confidence: 99%

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Thermal collapse of porous interstellar ice

Bossa

Isokoski

Valois

et al. 2012

A&A

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Aims. This article aims at a quantitative characterization of the phase transition of porous amorphous solid water (ASW) to a nonporous, i.e., more compact structure over an astronomically relevant temperature regime. Methods. A new laboratory based method is described that monitors the ice thickness decrease by combining optical interference with Fourier transform infrared spectroscopy. Three different water ice morphologies are studied; porous ASW as primary target, and less-porous ASW as well as crystalline solid water for comparison. Results. The thickness of the porous ASW sample is found to decrease by 12 ± 1% upon heating from 20 to 120 K. The thickness decrease of less-porous ASW is smaller, and negligible for crystalline solid water. Conclusions. Porous ASW, if formed under interstellar conditions, is expected to become less porous with increasing temperature. The thermally induced structural collapse affects the diffusion of the interstellar ice components, and therefore the catalytic properties of the ice.

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Section: Experimental Methodsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Experimental Methodsmentioning

confidence: 99%

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Thermal collapse of porous interstellar ice

Bossa

Isokoski

Valois

et al. 2012

A&A

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“…Water-ice morphology/structure strongly depends on deposition conditions such as temperature, deposition rate, and growth angle (e.g., Hagen et al 1983;Jenniskens & Blake 1994;Westley et al 1998;Kimmel et al 2001a,b;Dohnálek et al 2003).…”

Section: Resultsmentioning

confidence: 99%

Near-infrared laboratory spectra of H₂O trapped in N₂, CH₄, and CO: hints for trans-Neptunian objects' observations

Fulvio¹,

Guglielmino²,

Favone³

et al. 2010

A&A

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Context. Recent mid-infrared spectroscopic observations of Pluto and Triton suggest a wide distribution of H 2 O ice into surface regions containing more volatile species such as N 2 , CH 4 , and CO. This disagrees with the common idea that because of their typical surface temperature, water should not be involved in volatile transport processes, standing easily segregated from the more volatile species. Aims. We analyse infrared H 2 O band profiles when water is diluted in solid matrices dominated by methane, carbon monoxide, and/or molecular nitrogen. We also show the results of temperature-related diffusion processes of solid N 2 into H 2 O ice deposited at different temperatures. Finally, we analyse ion irradiation effects for some of the mixtures considered. Methods. Solid samples were analysed by infrared (1.0-16.0 µm) transmission and reflectance spectroscopy at different temperatures (15-150 K), before and after ion irradiation with 200 keV protons. Results. When water is highly diluted in solid matrices, the profile of its near-infrared bands is strongly modified. Two narrow bands appear around 1.89 µm and 1.39 µm instead of the well known pure water ice bands at 2 µm and 1.5 µm, respectively. Furthermore, the peak position and width of the 1.89 and 1.39 µm bands depend on the initial mixture water is embedded in. The intensity of these bands decreases after ion irradiation. Conclusions. Since the mixtures considered closely resemble the surface composition of trans-Neptunian objects, experiments here discussed show that the bands around 1.89 µm and 1.39 µm are appropriate to investigating the presence of diluted water regions on their surface. In fact, the irradiation dose required for a significant decrease in their intensity would be accumulated on a timescale larger than the timescale for resurfacing processes on the surfaces of trans-Neptunian objects. Results shown here will contribute in a strong way to the interpretation of New Horizons near-infrared observations.

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“…for crystalline H 2 O-ice (Hale and Querry, 1973), 1.29 for amorphous H 2 O-ice (Westley et al, 1998;Dohnálek et al, 2003)], and h ice is the angle of reflection in the ice (taken to be 45°). After the ice was fully deposited, its spectrum was obtained and ratioed to the background spectrum.…”

Section: Methodsmentioning

confidence: 99%

Laboratory spectra of CO2 vibrational modes in planetary ice analogs

White

Mastrapa

Sandford

2012

Icarus

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a b s t r a c tLaboratory spectra have shown that CO 2 is a powerful diagnostic tool for analyzing infrared data from remote observations, as it has been detected on icy moons in the outer Solar System as well as dust grain surfaces in the interstellar medium (ISM). IR absorption band profiles of CO 2 within ice mixtures containing H 2 O and CH 3 OH change with respect to temperature and mixture ratios. In this particular study, the m 3 CO 2 asymmetric stretch mode near 4.3 lm (2350 cm À1 ), overtone mode near 1.97 lm (5080 cm À1 ), and the combination bands near 2.7 lm (3700 cm À1 ), 2.8 lm (3600 cm À1 ), and 2.02 lm (4960 cm À1 ), are systematically observed in different mixtures with H 2 O and CH 3 OH in temperature ranges from 15 K to 150 K. Additionally, some high-temperature deposits (T > 50 K) of H 2 O, CH 3 OH, and CO 2 ice mixtures were performed and it was discovered that CO 2 may deposit out at higher temperatures than previously recorded. These data may then be used to interpret infrared observational data obtained from icy surfaces in the outer Solar System and beyond.

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Density and index of refraction of water ice films vapor deposited at low temperatures

Cited by 178 publications

References 55 publications

Thermal collapse of porous interstellar ice

Thermal collapse of porous interstellar ice

Near-infrared laboratory spectra of H₂O trapped in N₂, CH₄, and CO: hints for trans-Neptunian objects' observations

Laboratory spectra of CO2 vibrational modes in planetary ice analogs

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Density and index of refraction of water ice films vapor deposited at low temperatures

Cited by 178 publications

References 55 publications

Thermal collapse of porous interstellar ice

Thermal collapse of porous interstellar ice

Near-infrared laboratory spectra of H2O trapped in N2, CH4, and CO: hints for trans-Neptunian objects' observations

Laboratory spectra of CO2 vibrational modes in planetary ice analogs

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Resources

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Near-infrared laboratory spectra of H₂O trapped in N₂, CH₄, and CO: hints for trans-Neptunian objects' observations