Absolute Infrared Intensities of the Fundamental Absorption Bands in Solid CO2 and N2O

Yamada, Haruka; Person, Willis B.

doi:10.1063/1.1726291

Cited by 170 publications

(64 citation statements)

References 20 publications

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“…However, the ratio calculated using the second method depends on the band strengths provided by the literature. The band strength for the CO 2 asymmetric stretching band at 2340 cm −1 was measured to be 7.6 × 10 −17 cm molecule −1 for the pure solid (Yamada & Person 1964;Gerakines et al 1995), while in water ice a value of 1.4 × 10 −16 cm molecule −1 was found (Sandford & Allamandola 1990). The band strength for the wagging mode of NH 3 at 1070 cm −1 varies from 1.3 × 10 −17 to 1.7 ×10 −17 cm molecule −1 (Kerkhof et al 1999;d'Hendecourt et al 1986) in its pure solid form.…”

Section: Description Of Experimental Methodsmentioning

confidence: 99%

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Carbamic acid and carbamate formation in NH$_{\sf 3}$:CO$_{\sf 2}$ ices – UV irradiation versus thermal processes

Bossa¹,

Theulé²,

Duvernay³

et al. 2008

A&A

114

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ContextMethods. Infrared and mass spectroscopy are used to monitor NH 3 :CO 2 ice mixture evolution during both warming and VUV photon irradiation.Results. Carbamic acid and ammonium carbamate can be produced thermally in a 1:1 ratio from NH 3 and CO 2 above 80 K. They can be also formed in a 28:1 ratio by less efficient processes such as energetic photons. Our study and its results provide fresh insight into carbamic acid formation in interstellar ices. Conclusions. We demonstrate that care is required to separate irradiation-induced reactivity from purely thermal reactivity in ices in which ammonia and carbon dioxide are both present. From an interstellar chemistry point of view, carbamic acid and ammonium carbamate are readily produced from the ice mantle of a typical interstellar grain and should therefore be a detectable species in molecular clouds.

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Section: Description Of Experimental Methodsmentioning

confidence: 99%

“…The values of the band strengths for these two molecules depend on the nature, composition, and temperature of the ice in which they are found. We therefore used the values given by Yamada & Person (1964) for CO 2 (7.6×10…”

Section: Description Of Experimental Methodsmentioning

confidence: 99%

Carbamic acid and carbamate formation in NH$_{\sf 3}$:CO$_{\sf 2}$ ices – UV irradiation versus thermal processes

Bossa¹,

Theulé²,

Duvernay³

et al. 2008

A&A

114

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“…The ISAC set-up is an ultra-high vacuum (UHV) chamber with a pressure about 4 × 10 −11 mbar, which corresponds to a density of 10 6 cm −3 (Muñoz Caro et al 2010), similar to that found in dense cloud From Jiang et al (1975). (c) From Yamada & Person (1964). (d) From d 'Hendecourt & Allamandola (1986).…”

Section: Methodsmentioning

confidence: 99%

Thermal desorption of circumstellar and cometary ice analogs

Martín-Doménech

Muñoz

Bueno

et al. 2014

A&A

111

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Context. Thermal annealing of interstellar ices takes place in several stages of star formation. Knowledge of this process comes from a combination of astronomical observations and laboratory simulations under astrophysically relevant conditions. Aims. For the first time we present the results of temperature programmed desorption (TPD) experiments with pre-cometary ice analogs composed of up to five molecular components: H 2 O, CO, CO 2 , CH 3 OH, and NH 3 . Methods. The experiments were performed with an ultra-high vacuum chamber. A gas line with a novel design allows the controlled preparation of mixtures with up to five molecular components. Volatiles desorbing to the gas phase were monitored using a quadrupole mass spectrometer, while changes in the ice structure and composition were studied by means of infrared spectroscopy. Results. The TPD curves of water ice containing CO, CO 2 , CH 3 OH, and NH 3 present desorption peaks at temperatures near those observed in pure ice experiments, volcano desorption peaks after water ice crystallization, and co-desorption peaks with water. Desorption peaks of CH 3 OH and NH 3 at temperatures similar to the pure ices takes place when their abundance relative to water is above ∼3% in the ice matrix. We found that CO, CO 2 , and NH 3 also present co-desorption peaks with CH 3 OH, which cannot be reproduced in experiments with binary water-rich ice mixtures. These are extensively used in the study of thermal desorption of interstellar ices. Conclusions. These results reproduce the heating of circumstellar ices in hot cores and can be also applied to the late thermal evolution of comets. In particular, TPD curves represent a benchmark for the analysis of the measurements that mass spectrometers on board the ESA-Rosetta cometary mission will perform on the coma of comet 67P/Churyumov-Gerasimenko, which will be active before the arrival of Rosetta according to our predictions.

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“…Next, after fitting a straight baseline, we calculated the band area, divided by the band strength A, and corrected for 45 • incidence, to obtain the column density of the film. To quantify the optical depth we assumed that the band strengths of 13 CO and 13 CO 2 were the same as for 12 CO and 12 CO 2 , A = 7.6 × 10 −17 cm molecule −1 ( 13 CO 2 ) and A = 1.1 × 10 −17 cm molecule −1 ( 13 CO) (Yamada & Person 1964;Jiang et al 1975). Comparing the column density measured by infrared spectroscopy with the film thickness measured by laser interferometry (Baratta & Palumbo 1998), we derive that the density of the CO film in our experimental conditions is 0.81 g cm −3 .…”

Section: Experimental Methodsmentioning

confidence: 99%

CO$\mathsf{_{2}}$ synthesis in solid CO by Lyman-α photons and 200 keV protons

Loeffler

Baratta²,

Palumbo³

et al. 2005

A&A

139

150

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Abstract.We have studied the synthesis of carbon dioxide from solid carbon monoxide at 16 K induced by photolysis with Lyman-α photons and by irradiation with 200 keV protons to quantitatively compare the effects of photolysis and ion irradiation on CO ice and to determine the importance of these processes in interstellar ice grains. The CO and CO 2 concentrations during irradiation of an initially pure CO film evolve with fluence to a saturation value, a behaviour that is explained by a two-state model. Our results indicate that the initial CO 2 production rates for both radiation processes are similar when normalized to the absorbed energy and that the solid CO 2 abundance observed in the interstellar ices cannot be explained only by radiolysis and photolysis of pure solid CO.

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Absolute Infrared Intensities of the Fundamental Absorption Bands in Solid CO2 and N2O

Cited by 170 publications

References 20 publications

Carbamic acid and carbamate formation in NH$_{\sf 3}$:CO$_{\sf 2}$ ices – UV irradiation versus thermal processes

Carbamic acid and carbamate formation in NH$_{\sf 3}$:CO$_{\sf 2}$ ices – UV irradiation versus thermal processes

Thermal desorption of circumstellar and cometary ice analogs

CO$\mathsf{_{2}}$ synthesis in solid CO by Lyman-α photons and 200 keV protons

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