Cold condensation of dust in the ISM

Rouillé, Gaël; Jäger, Cornelia; Krasnokutski, Serge A.; Krebsz, Melinda; Henning, Thomas

doi:10.1039/c4fd00010b

Cited by 37 publications

(38 citation statements)

References 33 publications

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“…This study is therefore not able to solve this long-standing conundrum. Although recent experiments Rouillé et al 2014) show that it may be possible to form silicates under ISM conditions. However, it seems that the modelling of silicate sputtering together with hydrodynamical simulations of shock dynamics are absolutely critical to advance our understanding and will possibly give lower silicate sputtering resulting in a longer lifetime t SNR,s 6 × 10 8 yr.…”

Section: Discussionmentioning

confidence: 99%

“…However, as pointed out by Jones & Nuth (2011), silicate re-formation under the low density and temperature conditions of the ISM seems to be a rather problematic scenario. However, SiO and silicate grain formation at low temperatures (T 15 K) has been observed in the laboratory using idealised neon matrix and helium droplet isolation techniques Rouillé et al 2014). The oligomerisation of SiO molecules is barrierless and therefore could be an efficient mechanism for silicate formation in the low-temperature ISM .…”

Section: Consequences Of the Uncertaintiesmentioning

confidence: 99%

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A re-evaluation of dust processing in supernova shock waves

Bocchio

Jones

Slavin

2014

A&A

108

154

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Context. There is a long-standing and large discrepancy between the timescale for dust formation around evolved stars and the rapid dust destruction timescale in interstellar shocks. Aims. We use our latest estimates for dust processing to re-evaluate the dust destruction efficiency in supernova triggered shock waves, estimate the dust lifetime, and calculate the emission and extinction from shocked dust. Methods. We modelled the sputtering and fragmentation of grains in interstellar shocks for shock velocities between 50 km s −1 and 200 km s −1 . We constrained the dust destruction using our recent dust model. Finally, we coupled our code to the DustEM code in order to estimate the emission and extinction from the dust post-shock. Results. Carbonaceous grains are quickly destroyed, even in a 50 km s −1 shock, leading to a shorter lifetime than in previous studies. Silicate grains appear to be more resilient, but the new destruction lifetime that we find is similar to previous studies and short compared to the dust injection timescale. Conclusions. The calculated fraction of elements locked in grains is not compatible with the observed values and therefore implies the re-formation of dust in the dense regions of the interstellar medium. Better modelling of the silicate sputtering together with hydrodynamical simulations of interstellar shocks, appears to reduce the silicate destruction and may close the destruction-formation timescale gap.

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Section: Discussionmentioning

confidence: 99%

Section: Consequences Of the Uncertaintiesmentioning

confidence: 99%

A re-evaluation of dust processing in supernova shock waves

Bocchio

Jones

Slavin

2014

A&A

108

154

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“…Dwek et al 2007;Michałowski et al 2010aMichałowski et al , 2010bHirashita & Kuo 2011;Valiante et al 2011;Kuo & Hirashita 2012;Mancini et al 2015;Michałowski 2015). Recent experiments by Rouillé et al (2014) showed that accretion actually occurs in cold environments.…”

Section: Constraint On the Parametersmentioning

confidence: 99%

Dust evolution processes constrained by extinction curves in nearby galaxies

Hou

Hirashita

Michałowski

2016

Publications of the Astronomical Society of Japan

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Extinction curves, especially those in the Milky Way (MW), the Large Magellanic Cloud (LMC), and the Small Magellanic Cloud (SMC), have provided us with a clue to the dust properties in the nearby Universe. We examine whether or not these extinction curves can be explained by well known dust evolution processes. We treat the dust production in stellar ejecta, destruction in supernova shocks, dust growth by accretion and coagulation, and dust disruption by shattering. To make a survey of the large parameter space possible, we simplify the treatment of the grain size distribution evolution by adopting the 'two-size approximation', in which we divide the grain population into small ( < ∼ 0.03 µm) and large ( > ∼ 0.03 µm) grains. It is confirmed that the MW extinction curve can be reproduced in reasonable ranges for the time-scale of the above processes with a silicate-graphite mixture. This indicates that the MW extinction curve is a natural consequence of the dust evolution through the above processes. We also find that the same models fail to reproduce the SMC/LMC extinction curves. Nevertheless, this failure can be remedied by giving higher supernova destruction rates for small carbonaceous dust and considering amorphous carbon for carbonaceous dust; these modification fall in fact in line with previous studies. Therefore, we conclude that the current dust evolution scenario composed of the aforementioned processes is successful in explaining the extinction curves. All the extinction curves favor efficient interstellar processing of dust, especially, strong grain growth by accretion and coagulation.

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“…b á ñ a 3 derived from Equation (9) for the enhancement factor D(a) for silicate grains in the CNM. recent experiments in Jena thatdemonstrate that adsorbed species can form chemical bonds characteristic ofsilica and silicates at substrate temperatures of 10K without an activation barrier Rouillé et al 2014).…”

Section: Sticking Coefficientmentioning

confidence: 99%

Modeling Dust Evolution in Galaxies With a Multiphase, Inhomogeneous Ism

Zhukovska

Dobbs

Jenkins

et al. 2016

ApJ

151

160

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We develop a model of dust evolution in a multiphase, inhomogeneous interstellar medium (ISM) using hydrodynamical simulations of giant molecular clouds in a Milky Way-like spiral galaxy. We improve the treatment of dust growth by accretion in the ISM to investigate the role of the temperature-dependent sticking coefficient and ion-grain interactions. From detailed observational data on the gas-phase Si abundances Si H ] and the local gas density n H ( )thatwe use as a critical constraint for the models. This relation requires a sticking coefficient that decreases with the gas temperature. The relation predicted by the models reproduces the slope of −0.5 forthe observed relation in cold clouds, which is steeper than that for the warm medium and is explained by dust growth. We find that growth occurs in the cold medium for all adopted values of the minimum grain size a min from 1 to 5nm. ] -n H ( ) relation, and provide a better match to observations. The rates of dust re-formation in the ISM by far exceed the rates of dust production by stellar sources. After the initial 140Myr, the cycle of matter in and out of dust reaches a steady state, in which the dust growth balances the destruction on a similar timescale of 350Myr.

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Cold condensation of dust in the ISM

Cited by 37 publications

References 33 publications

A re-evaluation of dust processing in supernova shock waves

A re-evaluation of dust processing in supernova shock waves

Dust evolution processes constrained by extinction curves in nearby galaxies

Modeling Dust Evolution in Galaxies With a Multiphase, Inhomogeneous Ism

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