Cosmic dust formation at cryogenic temperatures

Rouillé, Gaël; Krasnokutski, Serge A.; Krebsz, Melinda; Jäger, C.; Huisken, F.; Henning, Thomas

doi:10.22323/1.207.0047

Cited by 3 publications

(9 citation statements)

References 13 publications

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“…The experiments also suggest that the formation process of carbonaceous solids is barrierless: neither additional energy nor long time scales are necessary to produce the solid carbonaceous materials. Interestingly, these results coincide with the finding of a barrierless condensation of silicates at temperatures of about 10 K (Krasnokutski et al 2014, Rouillé et al 2014a.…”

Section: Astrophysical Implication and Conclusionsupporting

confidence: 89%

“…The final condensates are fluffy aggregates consisting of nanometer-sized primary grains, amorphous and homogeneous in structure and composition. Looking at the mid-infrared (MIR) spectral properties of the condensates, a significant coincidence was pointed out between the 10 µm band of interstellar silicates (Chiar & Tielens 2006) and the 10 µm band of the low temperature siliceous condensates (Rouillé et al, 2014a).…”

Section: Introductionmentioning

confidence: 99%

“…Condensation of interstellar grains may be fueled by atoms and molecules which are the product, on the one hand, of stellar and interstellar chemistry and, on the other hand, of the erosion and destruction of pre-existing grains. Condensation of SiO molecules at low temperature has been recently studied in the laboratory (Krasnokutski et al 2014;Rouillé et al 2014a). Reactions between SiO molecules were found to be barrierless and the experiments have clearly revealed the efficient formation of SiO x condensates at temperatures of about 10 K. In another experimental study, low temperature condensation of more complex silicates with pyroxene and olivine composition has been studied (Rouillé et al, 2014b).…”

Section: Introductionmentioning

confidence: 99%

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Laboratory Experiments on the Low-temperature Formation of Carbonaceous Grains in the ISM

Fulvio

Góbi

Jäger

et al. 2017

ApJS

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The life-cycle of cosmic dust grains is far from being understood and the origin and evolution of interstellar medium (ISM) grains is still under debate. In the ISM, the cosmic dust destruction rate is faster than the production rate by stellar sources. However, observations of ISM refractory matter suggest that to maintain a steady amount of cosmic grains, some supplementary production mechanism takes place. In this context, we aimed to study possible re-formation mechanisms of cosmic grains taking place at low temperature directly in the ISM. The low temperature condensation of carbonaceous materials has been investigated in experiments mimicking the ISM conditions. Gasphase carbonaceous precursors created by laser ablation of graphite were forced to accrete on cold substrates (T ≈ 10 K) representing surviving dust grains. The growing and evolution of the condensing carbonaceous precursors have been monitored by MIR and UV spectroscopy under a number of experimental scenarios. It is demonstrated, for the first time, the possibility to form ISM carbonaceous grains "in situ". The condensation process is governed by carbon chains that first condense into small carbon clusters and finally into more stable carbonaceous materials, which structural characteristics are comparable to the material formed in gas-phase condensation experiments at very high temperature. We also show that the so-formed fullerene-like carbonaceous material is transformed into a more ordered material under VUV processing. The cold condensation mechanisms here discussed can give fundamental clues to fully understand the balance between the timescale for dust injection, destruction and re-formation in the ISM.

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Section: Astrophysical Implication and Conclusionsupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Laboratory Experiments on the Low-temperature Formation of Carbonaceous Grains in the ISM

Fulvio

Góbi

Jäger

et al. 2017

ApJS

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“…This finding is certainly caused by small problems with the reference measurements of pure KBr during the cooling and warming up phase. Previous temperature-dependent IR measurements of low-temperature SiO x condensates revealed the formation of the solid phase already at about 10 K. 19 Similarly, the magnesium silicate condensate shown in Fig. 5 has either been formed at low temperature (13 K).…”

Section: Analysis Of the Low-temperature Condensatesmentioning

confidence: 54%

Cold condensation of dust in the ISM

et al. 2014

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The condensation of complex silicates with pyroxene and olivine composition at conditions prevailing in molecular clouds has been experimentally studied. For this purpose, molecular species comprising refractory elements were forced to accrete on cold substrates representing the cold surfaces of surviving dust grains in the interstellar medium. The efficient formation of amorphous and homogeneous magnesium iron silicates at temperatures of about 12 K has been monitored by IR spectroscopy. The gaseous precursors of such condensation processes in the interstellar medium are formed by erosion of dust grains in supernova shock waves. In the laboratory, we have evaporated glassy silicate dust analogs and embedded the released species in neon ice matrices that have been studied spectroscopically to identify the molecular precursors of the condensing solid silicates. A sound coincidence between the 10 µm band of the interstellar silicates and the 10 µm band of the low-temperature siliceous condensates can be noted.

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“…Table A1 contains information on the wavelength positions of the features used for identification. Not included in Table A1 are complex absorption features attributed to Si x O x (x > 1) oligomers (Rouillé et al 2014b;Krasnokutski et al 2014).…”

Section: Methodsmentioning

confidence: 99%

Separate Silicate and Carbonaceous Solids Formed from Mixed Atomic and Molecular Species Diffusing in Neon Ice

Rouillé

Jäger

Henning

2020

ApJ

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The formation and growth of refractory matter on pre-existing interstellar dust grain surfaces was studied experimentally by annealing neon-ice matrices in which potential precursors of silicate grains (Mg and Fe atoms, SiO and SiO 2 molecules) and of solid carbon (C n molecules, n = 2-10) were initially isolated. Other molecules, mainly O 3 , CO, CO 2 , C 3 O, and H 2 O, were embedded at the same time in the matrices. The annealing procedure caused the cold dopants to diffuse and interact in the neon ice. Monitoring the procedure in situ with infrared spectroscopy revealed the disappearance of the silicon oxide and carbon molecules at temperatures lower than 13 K, and the rise of the Si O stretching band of silicates. Ex situ electron microscopy confirmed the formation of silicate grains and showed that their structure was amorphous. It also showed that amorphous carbon matter was formed simultaneously next to the silicate grains, the two materials being chemically separated. The results of the experiments support the hypothesis that grains of complex silicates and of carbonaceous materials are re-formed in the cold ISM, as suggested by astronomical observations and evolution models of cosmic dust masses. Moreover, they show that the potential precursors of one material do not combine with those of the other at cryogenic temperatures, providing us with a clue as to the separation of silicates and carbon in interstellar grains.

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Cosmic dust formation at cryogenic temperatures

Cited by 3 publications

References 13 publications

Laboratory Experiments on the Low-temperature Formation of Carbonaceous Grains in the ISM

Laboratory Experiments on the Low-temperature Formation of Carbonaceous Grains in the ISM

Cold condensation of dust in the ISM

Separate Silicate and Carbonaceous Solids Formed from Mixed Atomic and Molecular Species Diffusing in Neon Ice

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