Dust destruction in the ISM: a re-evaluation of dust lifetimes

Jones, A. P.; Nuth, Joseph A.

doi:10.1051/0004-6361/201014440

Cited by 206 publications

(236 citation statements)

References 126 publications

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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: 74%

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: 74%

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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“…Such a factor 2 variation is expected by considering inhomogeneity or multi-phase structures in the ISM (McKee 1989). Jones & Nuth (2011) pointed out that the estimate of τSN is uncertain; however, as shown later, our choice of βSN nicely explains the dust-to-metal ratio of the Milky Way (Section 4.2). For the destruction of small grains, we conservatively choose α = 1, but later we will also discuss the cases with α < 1.…”

Section: Choice Of Parameter Valuesmentioning

confidence: 62%

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Hirashita

2015

Monthly Notices of the Royal Astronomical Society

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Full calculations of the evolution of grain size distribution in galaxies are in general computationally heavy. In this paper, we propose a simple model of dust enrichment in a galaxy with a simplified treatment of grain size distribution by imposing a 'two-size approximation'; that is, all the grain population is represented by small (grain radius a < 0.03 µm) and large (a > 0.03 µm) grains. We include in the model dust supply from stellar ejecta, destruction in supernova shocks, dust growth by accretion, grain growth by coagulation and grain disruption by shattering, considering how these processes work on the small and large grains. We show that this simple framework reproduces the main features found in full calculations of grain size distributions as follows. The dust enrichment starts with the supply of large grains from stars. At a metallicity level referred to as the critical metallicity of accretion, the abundance of the small grains formed by shattering becomes large enough to rapidly increase the grain abundance by accretion. Associated with this epoch, the mass ratio of the small grains to the large grains reaches the maximum. After that, this ratio converges to the value determined by the balance between shattering and coagulation, and the dust-to-metal ratio is determined by the balance between accretion and shock destruction. With a Monte Carlo simulation, we demonstrate that the simplicity of our model has an advantage in predicting statistical properties. We also show some applications for predicting observational dust properties such as extinction curves.

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“…Besides AGB stars, other sources such as novae, supernovae type II (Wooden et al 1993;Rho et al 2008Rho et al , 2009), young stellar objects (Dwek & Scalo 1980), and red giant stars (Nittler et al 1997) can produce silicate dust. Even dust formation in the ISM may occur in interstellar clouds (Jones & Nuth 2011). Although the amounts of dust contributed by these sources is still debated (Meikle et al 2007;Jones & Nuth 2011), silicate dust is abundant in the ISM and can be found in many different stages of the life cycle of stars (Henning 2010).…”

Section: Introductionmentioning

confidence: 99%

Absorption and scattering by interstellar dust in the silicon K-edge of GX 5-1

Zeegers

Costantini

Vries

et al. 2017

A&A

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Context. We study the absorption and scattering of X-ray radiation by interstellar dust particles, which allows us to access the physical and chemical properties of dust. The interstellar dust composition is not well understood, especially on the densest sight lines of the Galactic Plane. X-rays provide a powerful tool in this study. Aims. We present newly acquired laboratory measurements of silicate compounds taken at the Soleil synchrotron facility in Paris using the Lucia beamline. The dust absorption profiles resulting from this campaign were used in this pilot study to model the absorption by interstellar dust along the line of sight of the low-mass X-ray binary (LMXB) GX 5-1. Methods. The measured laboratory cross-sections were adapted for astrophysical data analysis and the resulting extinction profiles of the Si K-edge were implemented in the SPEX spectral fitting program. We derive the properties of the interstellar dust along the line of sight by fitting the Si K-edge seen in absorption in the spectrum of GX 5-1. Results. We measured the hydrogen column density towards GX 5-1 to be 3.40 ± 0.1 × 10 22 cm −2 . The best fit of the silicon edge in the spectrum of GX 5-1 is obtained by a mixture of olivine and pyroxene. In this study, our modeling is limited to Si absorption by silicates with different Mg:Fe ratios. We obtained an abundance of silicon in dust of 4.0 ± 0.3 × 10 −5 per H atom and a lower limit for total abundance, considering both gas and dust, of > 4.4 × 10 −5 per H atom, which leads to a gas to dust ratio of > 0.22. Furthermore, an enhanced scattering feature in the Si K-edge may suggest the presence of large particles along the line of sight.

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Dust destruction in the ISM: a re-evaluation of dust lifetimes

Cited by 206 publications

References 126 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

Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies

Absorption and scattering by interstellar dust in the silicon K-edge of GX 5-1

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