Densities and refractive indices of ethane and ethylene at astrophysically relevant temperatures

Satorre, M. Á.; Millán, Carlos; Molpeceres, Germán; Luna, R.; Maté, Belén; Domingo, M.; Escribano, Rafael; Santonja, C.

doi:10.1016/j.icarus.2017.05.005

Cited by 16 publications

(17 citation statements)

References 19 publications

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“…This overall behaviour is similar to that of other molecules studied before: CO 2 (Satorre et al 2008), NH 3 (Satorre et al 2013), and C 2 H 4 and C 2 H 6 (Satorre et al 2017). An amorphous structure is formed at low temperature that increases its order with increasing deposition temperature until a maximum density (or refractive index) is achieved, corresponding to a crystalline structure.…”

Section: Densities and Refractive Indicessupporting

confidence: 86%

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Densities, infrared band strengths, and optical constants of solid methanol

Luna

Molpeceres

Ortigoso

et al. 2018

A&A

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Contact. The increasing capabilities of space missions like the James Webb Space Telescope or ground-based observatories like the European Extremely Large Telescope demand high quality laboratory data of species in astrophysical conditions for the interpretation of their findings. Aims. We provide new physical and spectroscopic data of solid methanol that will help to identify this species in astronomical environments. Methods. Ices were grown by vapour deposition in high vacuum chambers. Densities were measured via a cryogenic quartz crystal microbalance and laser interferometry. Absorbance infrared spectra of methanol ices of different thickness were recorded to obtain optical constants using an iterative minimization procedure. Infrared band strengths were determined from infrared spectra and ice densities. Results. Solid methanol densities measured at eight temperatures vary between 0.64 g cm−3 at 20 K and 0.84 g cm−3 at 130 K. The visible refractive index at 633 nm grows from 1.26 to 1.35 in that temperature range. New infrared optical constants and band strengths are given from 650 to 5000 cm−1 (15.4–2.0 μm) at the same eight temperatures. The study was made on ices directly grown at the indicated temperatures, and amorphous and crystalline phases have been recognized. Our optical constants differ from those previously reported in the literature for an ice grown at 10 K and subsequently warmed. The disagreement is due to different ice morphologies. The new infrared band strengths agree with previous literature data when the correct densities are considered.

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Section: Densities and Refractive Indicessupporting

confidence: 86%

“…Our experiments were performed using two different experimental set-ups, one at the UPV-Alcoy and the other at IEM-CSIC-Madrid. Both have been described in detail in previous publications (Satorre et al 2017;Molpeceres et al 2016;Zanchet et al 2013).…”

Section: Experiments and Data Analysismentioning

confidence: 99%

Densities, infrared band strengths, and optical constants of solid methanol

Luna

Molpeceres

Ortigoso

et al. 2018

A&A

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“…As the temperature drops rapidly in Pluto’s lower atmosphere from >100 K at 25–50 km to ~40 K near the surface 17 , organic ice is expected to form 23 , which may influence the scattering cross section at visible wavelengths. Laboratory measurements of CH 4 and C 2 H 4 ices at 633 nm 58 , which is similar to the wavelength of LORRI (608 nm), suggest that organic ices have typical real refractive indices near 1.5 at temperatures between 40–65 K. In comparison, the real refractive index of Titan “tholins”, the haze material assumed in this work, is around 1.7. Also, due to the slightly higher CO mixing ratio in Pluto’s atmosphere compared to Titan, Pluto’s haze may contain more oxygen atoms than “tholins”.…”

Section: Methodssupporting

confidence: 61%

A bimodal distribution of haze in Pluto’s atmosphere

et al. 2022

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Pluto, Titan, and Triton make up a unique class of solar system bodies, with icy surfaces and chemically reducing atmospheres rich in organic photochemistry and haze formation. Hazes play important roles in these atmospheres, with physical and chemical processes highly dependent on particle sizes, but the haze size distribution in reducing atmospheres is currently poorly understood. Here we report observational evidence that Pluto’s haze particles are bimodally distributed, which successfully reproduces the full phase scattering observations from New Horizons. Combined with previous simulations of Titan’s haze, this result suggests that haze particles in reducing atmospheres undergo rapid shape change near pressure levels ~0.5 Pa and favors a photochemical rather than a dynamical origin for the formation of Titan’s detached haze. It also demonstrates that both oxidizing and reducing atmospheres can produce multi-modal hazes, and encourages reanalysis of observations of hazes on Titan and Triton.

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“…Investigations of the structural changes for the icy C 2 H 4 have been reported at different temperatures previously (Hudson et al, 2014;Satorre et al, 2017 amorphous, metastable, and crystalline structures; which are dominate at 12-20 K, 20-40 K and 50-60 K, respectively. Figure 5 supports their conclusion that there are three structures for icy C 2 H 4 at low temperature.…”

Section: Resultsmentioning

confidence: 99%

Vacuum-Ultraviolet Absorption Spectra of Icy C2H4 at 13–60 K

Lo¹,

Ghosh²,

Lu³

et al. 2021

Front. Astron. Space Sci.

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The thermal variation of absorption spectra of icy ethene in wavelength range 105–220 nm was measured from 13 to 100 K using a synchrotron as light source. Sublimation of icy ethene began above 62 K, resulting in decreasing absorption. The absorption of icy ethene increased at wavelengths less than about 150 nm with increasing temperature from 13 to 60 K, but decreased beyond above 150 nm. According to detailed examination, the absorption spectra of icy ethene intersected at isosbestic point 147.0 nm from 13 to 17 K, whereas those varied absorption profiles crossed at another point, 150.6 nm, from 23 to 60 K. These results indicate that ethene ices might exhibit three structures within temperature range 13–60 K. This work enhances our understanding of the spectra of icy ethene at low temperatures and our knowledge of its astrochemistry and astrophysics in cold astro-environments.

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Densities and refractive indices of ethane and ethylene at astrophysically relevant temperatures

Cited by 16 publications

References 19 publications

Densities, infrared band strengths, and optical constants of solid methanol

Densities, infrared band strengths, and optical constants of solid methanol

A bimodal distribution of haze in Pluto’s atmosphere

Vacuum-Ultraviolet Absorption Spectra of Icy C2H4 at 13–60 K

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