Density of , and ices at different temperatures of deposition

Satorre, M. Á.; Domingo, M.; Millán, Carlos; Luna, R.; Vilaplana, R.; Santonja, C.

doi:10.1016/j.pss.2008.07.015

Cited by 123 publications

(104 citation statements)

References 14 publications

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“…For water ice grown at 14 K, the spectra were reproduced with the data of Hudgins et al (1993) at 10 K. A sticking coefficient of one and a density of 1.1 g cm −3 (Narten et al 1976) were assumed at this temperature. For CH 4 at 14 K, a sticking coefficient of 1 (Sandford & Allamandola 1990) and a density of 0.47 g cm −3 (Satorre et al 2008) were used. A mean value of the optical constants given by Hudgins et al (1993) for pure CH 4 at 10 K and 20 K was used to simulate the IR spectra, because the CH 4 spectrum undergoes considerable changes in this temperature interval.…”

Section: Methodsmentioning

confidence: 99%

SPECTROSCOPIC EFFECTS IN CH₄/H₂O ICES

Gálvez

Maté

Herrero

et al. 2009

ApJ

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Recent observations of CH 4 in different astrophysical objects encourage laboratory research on methane/water ice mixtures. An IR spectroscopy laboratory investigation is presented on these systems. Co-deposited samples are formed by vapor deposition of CH 4 and H 2 O on a cold substrate, in a wide range of stoichiometries, from very diluted mixtures to CH 4 /H 2 O = 2.5 values. Samples are prepared at 14 K and at 40 K, and their temperature behavior is studied when they are warmed up to 60 K. The spectroscopic analysis is centered on the methane features, and also on the water dangling bonds (DBs) that appear in the spectra of the mixtures. The IR forbidden ν 1 band shows up in the spectrum (3.44 μm), indicating some form of distorted methane. The combination bands ν 3 + ν 4 and ν 1 + ν 4 are seen at 2.32 and 2.38 μm, and the ν 2 + ν 3 band weakly at 2.21 μm. Whereas ν 3 is not shifted in spectra of mixed samples, the wavenumber peak of ν 4 and its combination bands vary in a 6 cm −1 range, providing a possible estimation for the relative methane concentration in the sample. Bands in the spectra of mixtures are always broader than their counterparts in pure CH 4 ice. The intensity of ν 4 appears to increase in mixed samples with respect to the pure solid. Raising the temperature of the ices up to 60 K liberates part of the methane, but a fraction is retained with a maximum value of ∼7% ± 2%. This limit may provide information on the temperature properties of astrophysical objects. The different spectral characteristics of water DBs with increasing methane proportion in mixed samples can also furnish information to estimate the stoichiometry of the mixture.

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Section: Methodsmentioning

confidence: 99%

SPECTROSCOPIC EFFECTS IN CH₄/H₂O ICES

Gálvez

Maté

Herrero

et al. 2009

ApJ

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“…The samples were irradiated until a total fluence of 1.0 × 10 13 , 3 × 10 13 , 3.4 × 10 12 , and 2.2 × 10 13 ions cm −2 , for samples a to d, respectively. The total dose deposited in the ices (given in Table 1) was calculated using the SRIM code (Ziegler et al 2010), assuming an ice density of 0.94 g cm −3 (Satorre et al 2008). …”

Section: Ice Samplesmentioning

confidence: 99%

“…Figure 6 exhibits a strong water ice contamination at the end of the experiment as shown by the broad water ice bands around 3280 cm −1 and 1600 cm −1 . For this particular sample (sample d), the beam was (Satorre et al 2008). ( f ) D = F × S e /ρ, where F is the ion fluence, S e its electronic stopping power, and ρ the target density.…”

Section: Irradiation Of the Ice Mixturesmentioning

confidence: 99%

Irradiation of nitrogen-rich ices by swift heavy ions

Augé

Dartois

Engrand

et al. 2016

A&A

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Context. Extraterrestrial materials, such as meteorites and interplanetary dust particles, provide constraints on the formation and evolution of organic matter in the young solar system. Micrometeorites represent the dominant source of extraterrestrial matter at the Earth's surface, some of them originating from large heliocentric distances. Recent analyses of ultracarbonaceous micrometeorites recovered from Antarctica (UCAMMs) reveal an unusually nitrogen-rich organic matter. Such nitrogen-rich carbonaceous material could be formed in a N 2 -rich environment, at very low temperature, triggered by energetic processes. Aims. Several formation scenarios have been proposed for the formation of the N-rich organic matter observed in UCAMMs. We experimentally evaluate the scenario involving high energy irradiation of icy bodies subsurface orbiting at large heliocentric distances. Methods. The effect of Galactic cosmic ray (GCR) irradiation of ices containing N 2 and CH 4 was studied in the laboratory. The N 2 -CH 4 (90:10 and 98:2) ice mixtures were irradiated at 14 K by 44 MeV Ni 11+ and 160 MeV Ar 15+ swift heavy ion beams. The evolution of the samples was monitored using in-situ Fourier transform infrared spectroscopy. The evolution of the initial ice molecules and new species formed were followed as a function of projectile fluence. After irradiation, the target was annealed to room temperature. The solid residue of the whole process left after ice sublimation was characterized in-situ by infrared spectroscopy, and the elemental composition was measured ex-situ. Results. The infrared bands that appear during irradiation allow us to identify molecules and radicals (HCN, CN − , NH 3 , ...). The infrared spectra of the solid residues measured at room temperature show similarities with that of UCAMMs. The results point towards the efficient production of a poly-HCN-like residue from the irradiation of N 2 -CH 4 rich surfaces of icy bodies. The room temperature residue provides a viable precursor for the N-rich organic matter found in UCAMMs.

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“…Así, por ejemplo, si se realizan cálculos que involucren a la densidad, se debería de tener en cuenta que un hecho confirmado experimentalmente es que tanto la densidad del H2O (Jenniskens y Blake, 1996), como la del CO2 (Satorre et al, 2008) varía con la temperatura de depósito: de hecho para el caso del agua (principal molécula detectada), se suele tomar como referencia 1 g/cm 3 , es decir, su densidad en condiciones atmosféricas; sin embargo, la densidad del agua en condiciones astrofísicas no tiene este valor, sino que puede ser incluso un 40 % menor según varía la temperatura de depósito (0,62 < ρ(H2O) < 0,94 g/cm 3 , de 10 a 140 K de temperatura de depósito).…”

Section: Manto De Hielounclassified

“…El estudio del CO2 ha sido abordado desde varios puntos de vista por muchos autores en distintos trabajos (Wood and Roux, 1982;Warren, 1986;Hudgins et al, 1993;Ehrenfreund et al, 1997;Baratta y Palumbo, 1998, Satorre et al, 2008) obteniéndose valiosa información: constantes ópticas; coeficiente de absorción (A); propiedades espectroscópicas antes y después de su procesado energético (fotónico o iónico) mediante espectroscopia infrarroja; densidad, etc. Junto a estos estudios, es también importante conocer la relación existente entre su estructura y la capacidad de retención de otras especies químicas a bajas temperaturas, debido a que estas propiedades pueden influir en el cálculo de las abundancias de moléculas hipervolátiles (como el CH4 o el N2) en ambientes en que se den junto al hielo de CO2.…”

Section: Gasunclassified

Estudio experimental de la retención de volátiles por hielo de CO2: relevancia astrofísica

Domenech¹,

Rafael²

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Density of , and ices at different temperatures of deposition

Cited by 123 publications

References 14 publications

SPECTROSCOPIC EFFECTS IN CH₄/H₂O ICES

SPECTROSCOPIC EFFECTS IN CH₄/H₂O ICES

Irradiation of nitrogen-rich ices by swift heavy ions

Estudio experimental de la retención de volátiles por hielo de CO2: relevancia astrofísica

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Density of , and ices at different temperatures of deposition

Cited by 123 publications

References 14 publications

SPECTROSCOPIC EFFECTS IN CH4/H2O ICES

SPECTROSCOPIC EFFECTS IN CH4/H2O ICES

Irradiation of nitrogen-rich ices by swift heavy ions

Estudio experimental de la retención de volátiles por hielo de CO2: relevancia astrofísica

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SPECTROSCOPIC EFFECTS IN CH₄/H₂O ICES

SPECTROSCOPIC EFFECTS IN CH₄/H₂O ICES