Grain Shattering in Shocks: The Interstellar Grain Size Distribution

Jones, A. P.; Tielens, A. G. G. M.; Hollenbach, D. J.

doi:10.1086/177823

Cited by 668 publications

(1,033 citation statements)

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“…PAH destruction in the ISM is apparently so effective (Micelotta, Jones & Tielens 2010a) that they do not survive the travel from parent stars to H ii complexes where they are observed. The misbalance between the dust formation and destruction has also been noted for our Galaxy by Jones et al (1994) and Jones, Tielens & Hollenbach (1996) (see however Jones & Nuth 2011). A conventional explanation is that some dust formation in molecular clouds is possible.…”

Section: Introductionsupporting

confidence: 72%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of optical spectroscopy and infrared aperture photometry of more than 100 H ii complexes in nine galaxies. Spectra obtained with the 6-m telescope of SAO RAS are used along with archival data from Spitzer and several ground-based telescopes to infer a strength of polycyclic aromatic hydrocarbon (PAH) emission, age, properties of the UV radiation field, and metallicity of studied H ii complexes. Physical properties (age, radiation field parameters, metallicity) are related to the F 8 /F 24 ratio used as a proxy for the PAH abundance in order to reveal factors that may influence the PAH evolution in H ii complexes. The well-known correlation between the F 8 /F 24 ratio and metallicity is confirmed in the studied complexes. The infrared flux ratio also correlates with the [O iii]λ5007/Hβ ratio which is often considered as an indicator of the radiation field hardness, but this correlation seems to be a mere reflection of a correlation between [O iii]λ5007/Hβ and metallicity. In separate metallicity bins, the F 8 /F 24 ratio is found to correlate with an age of an H ii complex, which is estimated from the equivalent width of Hβ line. The correlation is positive for low metallicity complexes and negative for high metallicity complexes. Analysing various mechanisms of PAH formation and destruction in the context of found correlations, we suggest that PAH abundance is likely altered by the UV radiation within H ii complexes, but this is not necessarily due to their destruction. If PAHs can also form in H ii complexes due to some processes like aromatisation, photodestruction, shattering and sputtering of very small grains, the net F 8 /F 24 ratio is determined by a balance between all these processes that can be different at different metallicities.

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Section: Introductionsupporting

confidence: 72%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…During their time in the warm medium, grains are altered and partially or completely destroyed by a number of processes such as vaporisation in grain-grain collisions and erosion by ion sputtering in interstellar shocks, and by UV irradiation by the interstellar radiation field (McKee 1989;Tielens et al 1994;Jones et al 1994Jones et al , 1996Jones et al , 2013Slavin et al 2015). In clouds, grains are protected from UV irradiation and sputtering in shocks, and the dust mass can grow by accretion of gas-phase species (Greenberg 1982;Draine 2009).…”

Section: Introductionmentioning

confidence: 99%

The turbulent life of dust grains in the supernova-driven, multiphase interstellar medium

Peters

Zhukovska

Naab

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Dust grains are an important component of the interstellar medium (ISM) of galaxies. We present the first direct measurement of the residence times of interstellar dust in the different ISM phases, and of the transition rates between these phases, in realistic hydrodynamical simulations of the multi-phase ISM. Our simulations include a timedependent chemical network that follows the abundances of H + , H, H 2 , C + and CO and take into account self-shielding by gas and dust using a tree-based radiation transfer method. Supernova explosions are injected either at random locations, at density peaks, or as a mixture of the two. For each simulation, we investigate how matter circulates between the ISM phases and find more sizeable transitions than considered in simple mass exchange schemes in the literature. The derived residence times in the ISM phases are characterised by broad distributions, in particular for the molecular, warm and hot medium. The most realistic simulations with random and mixed driving have median residence times in the molecular, cold, warm and hot phase around 17, 7, 44 and 1 Myr, respectively. The transition rates measured in the random driving run are in good agreement with observations of Ti gas-phase depletion in the warm and cold phases in a simple depletion model, although the depletion in the molecular phase is under-predicted. ISM phase definitions based on chemical abundance rather than temperature cuts are physically more meaningful, but lead to significantly different transition rates and residence times because there is no direct correspondence between the two definitions.

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“…Interstellar shocks destroy interstellar dust (Jones et al 1994, Jones et al 1996 mainly through sputtering by impinging energetic ions. Supernova explosions drive strong shock waves into the surrounding interstellar medium.…”

Section: Shock Destructionmentioning

confidence: 99%

Chemical and physical properties of interstellar dust

Tielens¹

2011

Proc. IAU

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Abstract. The characteristics of interstellar dust reflect a complex interplay between stellar injection of stardust, destruction in the ISM, and regrowth in clouds. Astronomical observations and analysis of stardust isolated from meteorites have revealed a highly diverse interstellar and circumstellar grain inventory, including both amorphous materials and highly crystalline compounds (silicates and carbon). This review summarizes this dust budget and inventory. Interstellar dust is highly processed during its sojourn from its birthsite (stellar ejecta) to its incorporation into protoplanetary systems. Processing by strong shocks due to supernova explosions is particularly important. Sputtering by impacting gas ions in shocks in the intercloud medium of the ISM is counteracted by accretion in cloud phases and their balance sets the observed, interstellar, elemental depletion patterns. Astronomical and meteoritical-stardust evidence for these processes is reviewed and it is concluded that dust formation in the ISM is very rapid. Not surprisingly, the characteristics of interstellar dust are expected to vary widely reflecting local stellar sources, the effects of SNe processing, and the interstellar accretion process.

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Grain Shattering in Shocks: The Interstellar Grain Size Distribution

Cited by 668 publications

References 0 publications

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

The turbulent life of dust grains in the supernova-driven, multiphase interstellar medium

Chemical and physical properties of interstellar dust

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