Composition and quantities of dust produced by AGB-stars and returned to the interstellar medium

By A. Ferrarotti, H. Gail. 2006

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In Astronomy and Astrophysics

Citations in the corpus

Evolution of asymptotic giant branch stars. II. Optical to far-infrared isochrones with improved TP- (2007, methodology): “In our calculations the con- 7 Following Ferrarotti & Gail (2006), with seed or key elementwe denote the least abundant element among those required to form the dust species under consideration; e.g. Si is the seed element of the silicate compounds in O-rich stars. densation degrees are estimated as”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, background): “Dust is thought to be produced by both low–intermediate mass asymptotic giant branch (AGB) stars (Gehrz 1989; Ferrarotti & Gail 2006; Sargent et al. 2010) and massive stars when they explode as supernovae (SNe) at the end of their short lives (Rho et al. 2008; Dunne et al. 2009; Barlow et al. 2010).”
Mass loss of stars on the asymptotic giant branch (2018, background): “4.3 and 5.1) and in studies of dust yields from AGB stars (e.g., Ferrarotti and Gail 2006; Zhukovska and Henning 2013; Nanni et al. 2013, 2014; Schneider et al. 2014).”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, methodology): “In the model calculation of Ferrarotti & Gail (2006), olivine-and pyroxene-type dust are treated as separate species, but their production rates are added for the reasons mentioned above 4 .”
Too little radiation pressure on dust in the winds of oxygen-rich AGB stars (2006, methodology): “The gas is cold here (Tg≈700−900 K) which is not revealed by models using grey radiative transfer (Jeong et al. 2003, Ferrarotti & Gail 2006).”
Production of dust by massive stars at high redshift (2011, methodology): “The amount of dustMd(m,Z) is obtained from total dust yields of Ferrarotti and Gail (2006).”
The dust content of galaxies from z = 0 to z = 9 (2016, methodology): “This number is in decent agreement with the dust-condensation efficiencies calculated in Ferrarotti & Gail (2006) for the majority of combinations of initial stellar mass and metallicity.”
THE ACS NEARBY GALAXY SURVEY TREASURY. IX. CONSTRAINING ASYMPTOTIC GIANT BRANCH EVOLUTION WITH OLD METAL-POOR GALAXIES (2010, background): “This prediction is in agreement with the results of detailed models of dust formation (Ferrarotti & Gail 2006).”
The ATLAS3D Project – XXVIII. Dynamically driven star formation suppression in early-type galaxies (2014, background): “The formation of dust is a controversial subject, but it is thought that stellar winds from AGB/pAGB stars are likely tobe important (e.g. Ferrarotti & Gail 2006).”
simba: Cosmological simulations with black hole growth and feedback (2019, methodology): “We take a fixed dust condensation efficiency δAGB i,dust = 0.2 based on the theoretical models of Ferrarotti & Gail (2006).”
A far-infrared survey of bow shocks and detached shells around AGB stars and red supergiants (Corrigendum) (2011, background): “…material returned to the ISM can be altered by several processes, such as mixing of nucleosynthesis products into the envelope, dust formation (Ferrarotti & Gail 2006), shock-induced chemistry in the inner wind envelope (Duari et al. 1999), as well as photo-dissociation due to interstellar…”
Stellar sources of dust in the high-redshift Universe (2009, background): “Ferrarotti & Gail (2006) provide models which consistently describe the dependence of dust producti n by AGB stars on stellar initial mass and metallicity.”
Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, background): “…chemistry of these stars is crucial for a number of topics, such as the role played by AGBs and SAGBs as dust producers (Gail & Sedlmayr 1999; Ferrarotti & Gail 2006), that was shown to depend critically on the abundances of the various chemical species in the surface layers of the star…”