Dust formation in the winds of AGBs: the contribution at low metallicities

Criscienzo, M. Di; Dell’Agli, F.; Ventura, P.; Schneider, Raffaella; Valiante, Rosa; Franca, F. La; Rossi, C.; Gallerani, S.; Maiolino, R.

doi:10.1093/mnras/stt732

Cited by 53 publications

(59 citation statements)

References 50 publications

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“…All the relevant equations, with a detailed explanation of the physical assumptions adopted, can be found in Ferrarotti & Gail (2006) and in the series of papers on this argument published by our group (Ventura et al 2012a,b;Di Criscienzo et al 2013;Ventura et al 2014a). …”

Section: Dust Formation In the Winds Of Agb Starsmentioning

confidence: 99%

Planetary nebulae in the Small Magellanic Cloud

Ventura

Stanghellini

Criscienzo

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyse the planetary nebulae (PNe) population of the Small Magellanic Cloud (SMC), based on evolutionary models of stars with metallicities in the range 10 −3 ≤ Z ≤ 4 × 10 −3 and mass 0.9 M < M < 8 M , evolved through the asymptotic giant branch (AGB) phase. The models used account for dust formation in the circumstellar envelope. To characterise the PNe sample of the SMC, we compare the observed abundances of the various species with the final chemical composition of the AGB models: this study allows us to identify the progenitors of the PNe observed, in terms of mass and chemical composition. According to our interpretation, most of the PNe descend from low-mass (M < 2M ) stars, which become carbon rich, after experiencing repeated third dredge-up episodes, during the AGB phase. A fraction of the PNe showing the signature of advanced CNO processing are interpreted as the progeny of massive AGB stars, with mass above ∼ 6M , undergoing strong hot bottom burning. The differences with the chemical composition of the PNe population of the Large Magellanic Cloud (LMC) is explained on the basis of the diverse star formation history and age-metallicity relation of the two galaxies. The implications of the present study for some still highly debated points regarding the AGB evolution are also commented.

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Section: Dust Formation In the Winds Of Agb Starsmentioning

confidence: 99%

Planetary nebulae in the Small Magellanic Cloud

Ventura

Stanghellini

Criscienzo

et al. 2016

Mon. Not. R. Astron. Soc.

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“…One such fast mechanism is the condensation of dust grains in cooled SN ejecta (e.g., Matsuura et al 2011), where the contribution of SNe on dust production is dominant at early times (for time scales below ∼200 Myr, Gall et al 2011a). Asymptotic giant branch (AGB) stars start to recycle their metals into the ISM producing silicates grains after ∼40 Myr (Di Criscienzo et al 2013) and carbon-rich dust after a few hundreds Myr of main-sequence evolution (Galliano et al 2008). However, at low metallicities the contribution of AGB stars to dust production is unlikely to be significant in systems with young stellar populations (see below).…”

Section: At High Redshiftmentioning

confidence: 99%

Dust-to-metal ratios in damped Lyman-αabsorbers

De¹,

Ledoux²,

Savaglio³

et al. 2013

A&A

110

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Motivated by the anomalous dust-to-metal ratios derived in the literature for γ-ray burst (GRB) damped Lyman-α absorbers (DLAs), we measure these ratios using the dust-depletion pattern observed in UV/optical afterglow spectra associated with the interstellar medium (ISM) at the GRB host-galaxy redshifts. Our sample consists of 20 GRB absorbers and a comparison sample of 72 DLAs toward quasars (QSOs) with redshift 1.2 < z < 4.0 and down to Z = 0.002 Z metallicities. The dust-to-metal ratio in QSO-and GRB-DLAs increases both with metallicity and metal column density, spanning ∼10-110% of the Galactic value and pointing to a nonuniversal dust-to-metal ratio. The low values of dust-to-metal ratio suggest that low-metallicity systems have lower dust fractions than typical spiral galaxies and, perhaps, that the dust in these systems is produced inefficiently, i.e. by grain growth in the lowmetallicity regime with negligible contribution from supernovae (SNe) and asymptotic giant branch (AGB) stars. On the other hand, some GRB-and QSO-DLAs show high dust-to-metal ratio values out to z ∼ 4, requiring rapid dust production, such as in SN ejecta, but also in AGB winds and via grain growth for the highest metallicity systems. GRB-DLAs overall follow the dust-to-metal-ratio properties of QSO-DLAs, GRBs probing larger column and volume densities. For comparison, the dust-to-metal ratio that we derive for the SMC and LMC are ∼82-100% and ∼98% of the Galactic value, respectively. The literature dust-to-metal ratio of the lowmetallicity galaxy I Zw 18 (<37%) is consistent with the distribution that we find. The dust extinction A V increases steeply with the column density of iron in dust, N(Fe) dust , calculated from relative metal abundances, confirming that dust extinction is mostly occurring in the host galaxy ISM. Most GRB-DLAs display log N(Fe) dust > 14.7, above which several QSO-DLAs reveal molecular hydrogen, making GRB-DLAs promising candidates for molecular detection and study.

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“…The modelling of the AGB phase has made significant c 2017 RAS progresses in the recent years, with the description of the dust formation process in the winds, coupled to the evolution of the central star (Ferrarotti & Gail 2006;Nanni et al 2013Nanni et al , 2014Ventura et al 2012a,b;Di Criscienzo et al 2013;Ventura et al 2014a).…”

Section: Introductionmentioning

confidence: 99%

The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields

Ventura

Stanghellini

Dell’Agli

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the chemical abundances of a wide sample of 142 Galactic planetary nebulae (PNe) with good quality observations, for which the abundances have been derived more or less homogeneously, thus allowing a reasonable comparison with stellar models. The goal is the determination of mass, chemical composition and formation epoch of their progenitors, through comparison of the data with results from AGB evolution. The dust properties of PNe, when available, were also used to further support our interpretation.We find that the majority (∼ 60%) of the Galactic PNe studied has nearly solar chemical composition, while ∼ 40% of the sources investigated have sub-solar metallicities. About half of the PNe have carbon star progenitors, in the 1.5 M ⊙ < M < 3 M ⊙ mass range, which have formed between 300 Myr and 2 Gyr ago. The remaining PNe are almost equally distributed among PNe enriched in nitrogen, which we interpret as the progeny of M > 3.5 M ⊙ stars, younger than 250 Myr, and a group of oxygen-rich PNe, descending from old (> 2 Gyr) low-mass (M < 1.5 M ⊙ ) stars that never became C-stars.This analysis confirms the existence of an upper limit to the amount of carbon which can be accumulated at the surface of carbon stars, probably due to the acceleration of mass loss in the late AGB phases. The chemical composition of the present sample suggests that in massive AGB stars of solar (or slightly sub-solar) metallicity, the effects of third dredge up combine with hot bottom burning, resulting in nitrogenrich -but not severely carbon depleted -gaseous material to be ejected.

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Dust formation in the winds of AGBs: the contribution at low metallicities

Cited by 53 publications

References 50 publications

Planetary nebulae in the Small Magellanic Cloud

Planetary nebulae in the Small Magellanic Cloud

Dust-to-metal ratios in damped Lyman-αabsorbers

The evolution of Galactic planetary nebula progenitors through the comparison of their nebular abundances with AGB yields

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