Volatiles retained in icy surfaces dominated by CO2 after energy inputs

Satorre, M. Á.; Luna, R.; Millán, Carlos; Santonja, C.; Cantó, J.

doi:10.1016/j.pss.2008.05.017

Cited by 5 publications

(9 citation statements)

References 27 publications

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“…They also studied the desorption rate as function of temperature and found that CO 2 released some CO near 𝑇 = 40 K (corresponding to the CO sublimation temperature and likely representing desorption of CO deposited on the surface of the CO 2 ice rather than authentic segregation). They found that low-level emission of CO took place at 45-70 K, and that most CO was released during CO 2 sublimation that peaked at 80 K. It is interesting to compare these results with similar experiments for CH 4 (Luna et al 2008) and N 2 (Satorre et al 2009) entrapped in CO 2 . Both species have a first desorption peak near 𝑇 = 50 K (corresponding to CH 4 and N 2 sublimation), a second broad desorption peak at 𝑇 = 80-90 K (attributed to the removal of porosity in the CO 2 host), and a third peak centred at 𝑇 = 95-100 K during CO 2 sublimation.…”

Section: Release Of Co From Comentioning

confidence: 82%

“…However, the conditions within icy minor Solar System bodies are different from the interstellar conditions studied by Cooke et al (2018). Firstly, the relevant temperatures are higher and the porosity of CO 2 ice decreases drastically with increasing temperature (Satorre et al 2009). The smaller presence of pores at higher temperatures may strongly reduce the diffusivity and result in a much higher 𝐸 seg -value.…”

Section: Release Of Co From Comentioning

confidence: 88%

“…Considering that the ESA Rosetta mission demonstrated that a fraction of ices in Comet 67P/Churyumov-Gerasimenko appear to have presolar origin (Calmonte et al 2016;Marty et al 2017), icy minor Solar System bodies could have inherited CO : CO 2 mixtures from the interstellar medium. Laboratory experiments show that CO 2 readily traps hypervolatiles such as CH 4 (Luna et al 2008), N 2 (Satorre et al 2009), and CO (Simon et al 2019). Such substances are released from the CO 2 ice above their individual sublimation temperatures (the process is called segregation or distillation), primarily at a temperature interval of 70-90 K. As pointed out by Jewitt et al (2017), the activity of Comet C/2017 K2 took place at a heliocentric distance where a nucleus temperature of 60-70 K is expected.…”

Section: Introductionmentioning

confidence: 99%

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Thermophysical evolution of planetesimals in the primordial disc

Davidsson

2021

Monthly Notices of the Royal Astronomical Society

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The Primordial Disk of small icy planetesimals, once located at 15–30 AU from the Sun, was disrupted by giant planet migration in the early Solar System. The Primordial Disk thereby became the source region of objects in the current–day Kuiper Belt, Scattered Disk, and Oort Cloud. I present the thermophysics code ‘Numerical Icy Minor Body evolUtion Simulator’, or NIMBUS, and use it to study the thermophysical evolution of planetesimals in the Primordial Disk prior to its disruption. Such modelling is mandatory in order to understand the behaviour of dynamically new comets from the Oort Cloud, as well as the activity of Centaurs and short–period comets from the Scattered Disk, that return pre–processed to the vicinity of the Sun. I find that bodies in the midst of the Primordial Disk with diameters ranging 4–200 km lost all their CO ice on time-scales of order 0.1–10 Myr depending on size, through a combination of protosolar and long–lived radionuclide heating. CO and other hypervolatiles therefore require a less volatile host for their storage. I consider two possible hosts: amorphous water ice and CO2 ice. Because of the high luminosity of the protosun, some Primordial Disk bodies may have sustained significant crystallisation, CO: CO2 segregation, and CO2 sublimation in the uppermost few tens of meters. I discuss how this may affect coma abundance ratios and distant activity in dynamically new comets.

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Section: Release Of Co From Comentioning

confidence: 82%

Section: Release Of Co From Comentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

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Thermophysical evolution of planetesimals in the primordial disc

Davidsson

2021

Monthly Notices of the Royal Astronomical Society

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“…It has been argued that the production rates of CO and C 2 H 2 (Luspay- Kuti et al 2015), in addition to CH 4 , HCN, and H 2 S (Gasc et al 2017), are all correlated with that of CO 2 . Laboratory experiments likewise confirm that CO 2 is capable of trapping hyper-volatiles (Luna et al 2008;Satorre et al 2009;Simon et al 2019). This could be consistent with CO 2 being the source of these molecules.…”

Section: Modifications By Occluded Super-volatilesmentioning

confidence: 76%

Are there any pristine comets? Constraints from pebble structure

Malamud,

Landeck,

Bischoff

et al. 2022

Preprint

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We show that if comets (or any small icy planetesimals such as Kuiper belt objects) are composed of pebble piles, their internal radiogenic as well as geochemical heating results in considerably different evolutionary outcomes compared to similar past studies. We utilize a 1D thermo-physical evolution code, modified to include state-of-the-art empirical measurements of pebble thermal conductivity and compression, the latter obtained through a new laboratory experiment presented here for the first time. Results indicate that due to the low pebble thermal conductivity, the peak temperatures attained during evolution are much higher than in any previous study given the same formation time. Assuming meteoritic radiogenic abundances, we find that only extremely small, sub-kilometre comets have the potential to retain the primordial, uniform and thermally unprocessed composition from which they formed. Comets with radii in excess of about 20 km are typically swept by rapid and energetically powerful aqueous hydration reactions. Across the full range of comet sizes and formation times, evolutions result in the processing and differentiation of various volatile species, and a radially heterogeneous nucleus stucture. Our computations however also indicate that the assumed fraction of radionuclides is a pivotal free parameter, because isotopic analyses of the only available cometary samples suggest that no 26 Al was ever present in comet 81P/Wild 2. We show that if comets formed early in the protoplanetary disc (within 1-3 Myr), the radionuclide abundances indeed must be much smaller than those typically assumed based on meteoritic samples. We discuss the importance of our findings for the formation, present-day attributes and future research of comets.

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“…However, the study of mixtures where water is the main component has been addressed by several authors and typically all these molecules behave in a similar way, presenting two main desorption peaks: a first peak corresponding to its own desorption energy and an additional peak when this molecule desorbs simultaneously with water (Collings et al 2004;Martín-Doménech et al 2014). This retaining behavior is not exclusive of a polar molecule like water but is also observed for other nonpolar molecules, e.g., carbon dioxide (Satorre et al 2009). Calculations of desorption energy are necessary to interpret desorption processes occurring in many astrophysical scenarios.…”

Section: Discussionmentioning

confidence: 99%

A Fast, Direct Procedure to Estimate the Desorption Energy for Various Molecular Ices of Astrophysical Interest

Luna

Luna-Ferrándiz

Millán

et al. 2017

ApJ

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Desorption energy is a relevant parameter when studying the desorption kinetics of an ice under astrophysical conditions. Values reported are generally calculated using at least a desorption experiment and a further data analysis at present. In this work the establishment of a simple rule that relates the desorption energy of a species to the temperature of its desorption peak is explored. The paper presents the results obtained from zeroth-order desorption experiments, based on the use of a quartz crystal microbalance to monitor the loss of weight during desorption of the accreted ice sample under high-vacuum conditions, of nine different molecules covering a wide range of desorption energies. During these experiments, the ice desorption rate reaches a maximum at a certain temperature depending on the molecule. The formula obtained in this study facilitates the estimation of the desorption energy and is valid for all the investigated molecules. Based on these experimental results and simulations, the theoretical expression obtained is valid to calculate desorption energy for zeroth-and first-order desorption experiments under high-or ultrahigh-vacuum conditions using different ice thickness films.

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Volatiles retained in icy surfaces dominated by CO2 after energy inputs

Cited by 5 publications

References 27 publications

Thermophysical evolution of planetesimals in the primordial disc

Thermophysical evolution of planetesimals in the primordial disc

Are there any pristine comets? Constraints from pebble structure

A Fast, Direct Procedure to Estimate the Desorption Energy for Various Molecular Ices of Astrophysical Interest

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