Temperature Programmed Desorption of Water Ice from the Surface of Amorphous Carbon and Silicate Grains as Related to Planet-forming Disks

Потапов, А. В.; Jäger, Cornelia; Henning, Thomas

doi:10.3847/1538-4357/aad803

Cited by 29 publications

(42 citation statements)

References 76 publications

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“…The crystallisation can be accompanied by desorption of water ice following a desorption rate profile peaking around 180 K (cf. Potapov et al 2018). Similar desorption temperatures were observed by Collings et al (2004), who measured desorption temperatures around 160 K for a heating rate of 0.08 K s −1 .…”

Section: Warm-upsupporting

confidence: 83%

Spectroscopic measurements of CH₃OH in layered and mixed interstellar ice analogues

Müller

Giuliano

Goto

et al. 2021

A&A

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Context. The molecular composition of interstellar ice mantles is defined by gas-grain processes in molecular clouds, with the main components being H2O, CO, and CO2. Methanol (CH3OH) ice is detected towards the denser pre-stellar cores and star-forming regions, where large amounts of CO molecules freeze out and get hydrogenated on top of the icy grains. The thermal heating from nearby protostars can further change the ice structure and composition. Despite the several observations of icy features carried out towards molecular clouds and along the line of site of protostars, it is not yet clear if interstellar ices are mixed or if they have a layered structure. Aims. We aim to examine the effect of mixed and layered ice growth in dust grain mantle analogues, with specific focus on the position and shape of methanol infrared bands, so dedicated future observations could shed light on the structure of interstellar ices in different environments. Methods. Mixed and layered ice samples were deposited on a cold substrate kept at a temperature of 10 K using a closed-cycle cryostat placed in a vacuum chamber. The spectroscopic features were analysed by Fourier transform infrared spectroscopy. Different proportions of the most abundant four molecular species in ice mantles, namely H2O, CO, CO2, and CH3OH, were investigated, with a special attention placed on the analysis of the CH3OH bands. Results. We measure changes in the position and shape of the CH and CO stretching bands of CH3OH depending on the mixed or layered nature of the ice sample. Spectroscopic features of methanol are also found to change due to heating. Conclusions. A layered ice structure best reproduces the CH3OH band position recently observed towards a pre-stellar core and in star-forming regions. Based on our experimental results, we conclude that observations of CH3OH ice features in space can provide information about the structure of interstellar ices, and we expect the James Webb Space Telescope to put stringent constraints on the layered or mixed nature of ices in different interstellar environments, from molecular clouds to pre-stellar cores to protostars and protoplanetary discs.

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Section: Warm-upsupporting

confidence: 83%

Spectroscopic measurements of CH₃OH in layered and mixed interstellar ice analogues

Müller

Giuliano

Goto

et al. 2021

A&A

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“…Surveys at submillimeter (submm) wavelengths have 10 1 10 0 10 1 10 2 10 3 obs for crystalline ice (Fraser et al 2001;Brown et al 2006;Brown & Bolina 2007;Kobayashi et al 2011). In addition, the sublimation temperature does not change notably for the ice-dust mixture (Kobayashi et al 2011;Potapov et al 2018a). We therefore consider 100 K for amorphous ice dust aggregates and 105 K for crystalline ice dust aggregates.…”

Section: Model Descriptionmentioning

confidence: 99%

Constraining the detectability of water ice in debris disks

Kim

Wolf

Потапов

et al. 2019

A&A

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Context. Water ice is important for the evolution and preservation of life. Identifying the distribution of water ice in debris disks is therefore of great interest in the field of astrobiology. Furthermore, icy dust grains are expected to play important roles throughout the entire planet formation process. However, currently available observations only allow deriving weak conclusions about the existence of water ice in debris disks. Aims. We investigate whether it is feasible to detect water ice in typical debris disk systems. We take the following ice destruction mechanisms into account: sublimation of ice, dust production through planetesimal collisions, and photosputtering by UV-bright central stars. We consider icy dust mixture particles with various shapes consisting of amorphous ice, crystalline ice, astrosilicate, and vacuum inclusions (i.e., porous ice grains). Methods. We calculated optical properties of inhomogeneous icy dust mixtures using effective medium theories, that is, Maxwell-Garnett rules. Subsequently, we generated synthetic debris disk observables, such as spectral energy distributions and spatially resolved thermal reemission and scattered light intensity and polarization maps with our code DMS. Results. We find that the prominent ∼ 3 µm and 44 µm water ice features can be potentially detected in future observations of debris disks with the James Webb Space Telescope (JWST) and the Space Infrared telescope for Cosmology and Astrophysics (SPICA). We show that the sublimation of ice, collisions between planetesimals, and photosputtering caused by UV sources clearly affect the observational appearance of debris disk systems. In addition, highly porous ice (or ice-rich aggregates) tends to produce highly polarized radiation at around 3 µm. Finally, the location of the ice survival line is determined by various dust properties such as a fractional ratio of ice versus dust, physical states of ice (amorphous or crystalline), and the porosity of icy grains.

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“…The total experimental uncertainty estimated from the uncertainty of the photon flux, linear fit, and repeated experiments is ∼40% for the total photodesorption rate. An empirical dependence of the photodesorption yield on the temperature (T) and ice thickness (x) Ypd (T, x) = 10 -3 (1.3 + 0.032 × T)(1e -x/l(T) ), where l is a temperature-dependent ice diffusion parameter, was determined previously (Öberg, et al 2009a (Potapov, et al 2018a). Therefore, we probably have a sub-monolayer ice coverage of the dust instead of "nominal" 3 ML.…”

Section: Carbonaceous Grains Produced By Laser Ablation Show a Very Smentioning

confidence: 99%

Photodesorption of Water Ice from Dust Grains and Thermal Desorption of Cometary Ices Studied by the INSIDE Experiment

Потапов

Jäger

Henning

2019

ApJ

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A new experimental set-up INterStellar Ice-Dust Experiment (INSIDE), was designed for studying cosmic grain analogues represented by ice-coated carbon-and silicate-based dust grains. In the new instrument, we can simulate physical and chemical conditions prevailing in interstellar and circumstellar environments. The set-up combines ultrahigh vacuum and low temperature conditions with infrared spectroscopy and mass spectrometry. Using INSIDE, we plan to investigate physical and chemical processes, such as adsorption, desorption, and formation of molecules, on the surface of dust/ice samples. First experiments on the photodesorption of water ice molecules from the surface of silicate and carbon grains by UV photons revealed a strong influence of the surface properties on the desorption yield, in particular in the monolayer regime. In the second experiment, the thermal desorption of cometary ice analogues composed of six molecular components was studied for the first time.Co-desorption of CO2 and CH3OH with O2 indicates that at high O2 concentrations in cometary or interstellar ices "heavy" ice molecules can be partly trapped in O2 and release to the gas phase much earlier than expected. This effect could explain astronomical detections of complex organic molecules in cold dense interstellar clouds.

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Temperature Programmed Desorption of Water Ice from the Surface of Amorphous Carbon and Silicate Grains as Related to Planet-forming Disks

Cited by 29 publications

References 76 publications

Spectroscopic measurements of CH₃OH in layered and mixed interstellar ice analogues

Spectroscopic measurements of CH₃OH in layered and mixed interstellar ice analogues

Constraining the detectability of water ice in debris disks

Photodesorption of Water Ice from Dust Grains and Thermal Desorption of Cometary Ices Studied by the INSIDE Experiment

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Temperature Programmed Desorption of Water Ice from the Surface of Amorphous Carbon and Silicate Grains as Related to Planet-forming Disks

Cited by 29 publications

References 76 publications

Spectroscopic measurements of CH3OH in layered and mixed interstellar ice analogues

Spectroscopic measurements of CH3OH in layered and mixed interstellar ice analogues

Constraining the detectability of water ice in debris disks

Photodesorption of Water Ice from Dust Grains and Thermal Desorption of Cometary Ices Studied by the INSIDE Experiment

Contact Info

Product

Resources

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Spectroscopic measurements of CH₃OH in layered and mixed interstellar ice analogues

Spectroscopic measurements of CH₃OH in layered and mixed interstellar ice analogues