Evolution of interstellar dust and stardust in the solar neighbourhood
By S. Zhukovska, H. Gail, M. Trieloff. 2007
279 citations recorded by the source corpus.
Aims. We studied the evolution of the abundance in interstellar dust species that originate in stellar sources and from condensation in molecular clouds in the local interstellar medium of the Milky Way. We determined from this the input of dust material to the Solar System. Methods. A one-zone chemical evolution model of the Milky Way for the elemental composition of the disk combined with an evolution model for its interstellar dust component similar to that of Dwek (1998) is developed. The dust model considers dust-mass return from AGB stars as calculated from synthetic AGB models combined with models for dust condensation in stellar outflows. Supernova dust formation is included in a simple parametrised form that is gauged by observed abundances of presolar dust grains with a supernova origin. For dust growth in the ISM, a simple method is developed for coupling this with disk and dust evolution models. Results. A chemical evolution model of the solar neighbourhood in the Milky Way is calculated, which forms the basis for calculating a model of the evolution of the interstellar dust population at the galactocentric radius of the Milky Way. The model successfully passes all standard tests for the reliability of such models. In particular the abundance evolution of the important dust-forming elements is compared with observational results for the metallicity-dependent evolution of the abundances for G-type stars from the solar neighbourhood. It is found that the new tables of Nomoto et al. (2006) for the heavy element production give much better results for the abundance evolution of these important elements than the widely used tables of Woosley & Weaver (1995). The time evolution for the abundance of the following dust species is followed in the model: silicate, carbon, silicon carbide, and iron dust from AGB stars and from supernovae, as well as silicate, carbon, and iron dust grown in molecular clouds. It is shown that the interstellar dust population is dominated by dust accreted in molecular clouds; stardust only forms a minor fraction. Most of the dust material entering the Solar System at its formation does not show isotopic abundance anomalies of the refractory elements, i.e., inconspicuous isotopic abundances do not point to a Solar System origin for dust grains. The observed abundance ratios of presolar dust grains formed in supernova ejecta and in AGB star outflows requires that, for the ejecta from supernovae, the fraction of refractory elements condensed into dust is 0.15 for carbon dust and is quite small (∼10 −4 ) for other dust species.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/4b52b7cbc4f3a351f93314ab634386b6d00ceac7
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Citations in the corpus
- Physical Processes in the Interstellar Medium (2014, background): “A plausible explanation of this fact is that dust growth in the ISM is an ongoing process that occurs more rapidly in cold, dense gas than in warm, diffuse gas (see e.g. Zhukovska et al., 2008).”
- Astrophysics with Extraterrestrial Materials (2016, background): “…from stars of different masses, coupled with GCE models, indicate that massive AGB stars should have contributed at least as many O-rich grains to the ISM at the time of Solar System birth as did lowmass stars (Zhukovska et al. 2008, Gail et al. 2009), yet none have been observed (Nittler 2009).”
- The dust scaling relations of the Herschel Reference Survey (2012, unknown): “Here we assumeχ1 =0.2 (Morgan & Edmunds 2003),χ2 =0.5 (Zhukovska et al. 2008),p = 0.012 andα =0.80 (i.e., consistent with a Chabrier 2003 IMF),δ =0.3 (Edmunds 2001) andǫ =0.5.”
- THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP (2011, background): “Meanwhile, accounting for the observed dust abundance appears to require buildup of dust in molecular clouds (Dwek 1998; Zhukovska et al. 2008; Draine 2009).”
- Dust formation history of galaxies: A critical role of metallicity* for the dust mass growth by accreting materials in the interstellar medium (2012, background): “Dust grains not only originate from stars, but are also destroyed by SNe blast waves (e.g., Jones et al., 1994, 1996; Nozawa et al., 2003; Zhukovska et al., 2008).”
- Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, methodology): “Morgan & Edmunds (2003) used observations of dust in LIMSs to show that χ 2 ∼ 0.16 yet theoretical models following grain growth in stellar atmospheres (e.g. Zhukovska et al. 2008) suggest higher values of χ 2 ∼ 0.5.”
- Stellar sources of dust in the high-redshift Universe (2009, methodology): “On the basis of this model calculations, Zhukovska et al. (2008) propose refined grids of the ejected mass of different dust species, for different star masses in the range (1− 7)M⊙ and at various (sub-solar and solar) metallicities.”
- Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range (2013, methodology): “These models were originally introduced to study the lifecycle of dust species from different origins in the Solar neighbourhood (Zhukovska et al. 2008).”
- Production of dust by massive stars at high redshift (2011, background): “…grain growth in the ISM (e.g., Draine, 2009; Michałowski et al, 2010a; Dwek and Cherchneff, 2011), which is the preferred scenario in the Milky Way (e.g., Zhukovska et al, 2008; Draine, 2009), and (ii) dust formation in QSO outflows (e.g., Elvis etal, 2002; Pipino et al, 2011; Gall et al, 2011a).”
- The global dust SED: tracing the nature and evolution of dust with DustEM (2010, background): “Carbonaceous dust is formed in the ejecta of evolved stars but, seemingly, must also form directly in theISM (Zhukovska et al. 2008; Draine 2009a; Jones 2009).”