Trapping and release of gases by water ice and implications for icy bodies

Bar‐Nun, A.; Herman, G.; Laufer, D.; Rappaport, M.

doi:10.1016/0019-1035(85)90048-x

Cited by 253 publications

(161 citation statements)

References 27 publications

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“…This indicates that these molecules are retained in the water ice structure (Bar-Nun et al 1985;Collings et al 2004;Fayolle et al 2011). A fraction of the trapped molecules is released in the "volcano" desorption (Smith et al 1997) when the change from amorphous to cubic crystalline water ice occurs at T ∼ 160 K. Volcano desorption of NH 3 molecules in co-deposited mixtures with water was not reported in Collings et al (2004) , while volcano desorption of CH 3 OH had already been detected by Brown et al (2006).…”

Section: Resultsmentioning

confidence: 98%

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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Section: Resultsmentioning

confidence: 98%

Thermal desorption of circumstellar and cometary ice analogs

Martín-Doménech

Muñoz

Bueno

et al. 2014

A&A

111

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“…This, however, leads to a systematic error which affects the pre-exponential factor, D 0 , but not the energy barrier E D . A related aspect is the structural change in the water ice during the experiment, which leads to compaction of the film due to the collapse of macropores (Bossa et al 2012) and subsequently to trapping or release of CO (Bar-Nun et al 1985;Collings et al 2003b). In a pure ice, this transition is observed between 38 and 68 K (Jenniskens & Blake 1994).…”

Section: Experimental Results and Analysismentioning

confidence: 99%

Dynamics of Co in Amorphous Water-Ice Environments

Karssemeijer

Ioppolo

Hemert

et al. 2013

ApJ

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The long-timescale behavior of adsorbed carbon monoxide on the surface of amorphous water ice is studied under dense cloud conditions by means of off-lattice, on-the-fly, kinetic Monte Carlo simulations. It is found that the CO mobility is strongly influenced by the morphology of the ice substrate. Nanopores on the surface provide strong binding sites, which can effectively immobilize the adsorbates at low coverage. As the coverage increases, these strong binding sites are gradually occupied leaving a number of admolecules with the ability to diffuse over the surface. Binding energies and the energy barrier for diffusion are extracted for various coverages. Additionally, the mobility of CO is determined from isothermal desorption experiments. Reasonable agreement on the diffusivity of CO is found with the simulations. Analysis of the 2152 cm −1 polar CO band supports the computational findings that the pores in the water ice provide the strongest binding sites and dominate diffusion at low temperatures.

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“…The second reason that the building blocks could preferentially trap CH 4 and NH 3 in the Saturnian subnebula is that the temperature could have been too high to trap CO and N 2 , which are trapped at much lower temperatures than CH 4 and NH 3 (Bar-Nun et al, 1985. This possibility would still be valid in a gas-starved disc and is further supported by the measured 36 Ar abundance relative to N 2 of 1.1 × 10 −7 (Niemann et al 2010).…”

Section: Titanmentioning

confidence: 99%

“…Like Triton, Pluto's nitrogen originated either as N 2 or NH 3 in the PSN. The abundance of N 2 is believed to have been greater in the PSN than NH 3 (Lewis and Prinn 1980), but would only have been accreted by Pluto if it formed at temperatures less than 38 K (Bar-Nun et al 1985.…”

Section: Pluto and Kuiper Belt Objectsmentioning

confidence: 99%

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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Trapping and release of gases by water ice and implications for icy bodies

Cited by 253 publications

References 27 publications

Thermal desorption of circumstellar and cometary ice analogs

Thermal desorption of circumstellar and cometary ice analogs

Dynamics of Co in Amorphous Water-Ice Environments

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

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