Asymptotic giant branch and super-asymptotic giant branch stars: modelling dust production at solar metallicity

Dell’Agli, F.; García-Hernández, D. A.; Schneider, Raffaella; Ventura, P.; Franca, F. La; Valiante, Rosa; Marini, E.; Criscienzo, M. Di

doi:10.1093/mnras/stx387

Cited by 49 publications

(34 citation statements)

References 52 publications

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“…In the dust production process, stellar mass and metallicity play a key role in determining the dust species formed: this happens because m and Z are crucial to set the number of thermal pulses occurring, which define the surface composition of the star (e.g. Ferrarotti & Gail 2006;Dell'Agli et al 2017).…”

Section: Dust Productionmentioning

confidence: 99%

Galactic Archaeology at High Redshift: Inferring the Nature of GRB Host Galaxies from Abundances

Palla

Matteuccí

Calura

et al. 2020

ApJ

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We identify the nature of high redshift long Gamma-Ray Bursts (LGRBs) host galaxies by comparing the observed abundance ratios in the interstellar medium with detailed chemical evolution models accounting for the presence of dust. We compare abundance data from long Gamma-Ray Bursts afterglow spectra to abundance patterns as predicted by our models for different galaxy types. We analyse [X/F e] abundance ratios (where X is C, N , O, M g, Si, S, N i, Zn) as functions of [F e/H]. Different galaxies (irregulars, spirals, spheroids) are, in fact, characterised by different star formation histories, which produce different [X/F e] vs. [F e/H] relations ("time-delay model"). This allows us to identify the star formation history of the host galaxies and to infer their age (i.e. the time elapsed from the beginning of star formation) at the time of the GRB events. Unlike previous works, we use newer models in which we adopt updated stellar yields and prescriptions for dust production, accretion and destruction. We consider a sample of seven LGRB host galaxies. Our results suggest that two of them (GRB 050820, GRB 120815A) are star forming spheroids, two (GRB 081008, GRB 161023A) are spirals and three (GRB 090926A, GRB 050730, GRB 120327A) are irregulars. The inferred ages of the considered host galaxies span from 10 M yr to slightly more than 1 Gyr.

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Section: Dust Productionmentioning

confidence: 99%

Galactic Archaeology at High Redshift: Inferring the Nature of GRB Host Galaxies from Abundances

Palla

Matteuccí

Calura

et al. 2020

ApJ

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“…In particular, the dust abundance is dominated by large grains when the stellar dust production is the major dust source, since dust grains ejected from stars are considered to be biased to large (a 0.1 µm, where a is the grain radius) grains (e.g. Nozawa et al 2007;Yasuda & Kozasa 2012;Dell'Agli et al 2017). Observations of the optical properties of dust formed in stellar environments (mainly in stellar winds) also show that dust condensed in the ejecta is dominated by large (sub-micron) grains (Groenewegen 1997;Winters et al 1997;Scicluna et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Expected dust grain-size distributions in galaxies detected by ALMA at z > 7

Liu

Hirashita

2019

Monthly Notices of the Royal Astronomical Society

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The dust properties in high-redshift galaxies provide clues to the origin of dust in the Universe. Although dust has been detected in galaxies at redshift z > 7, it is difficult to constrain the dominant dust sources only from the total dust amount. Thus, we calculate the evolution of grain size distribution, expecting that different dust sources predict different grain size distributions. Using the star formation time-scale and the total baryonic mass constrained by the data in the literature, we calculate the evolution of grain size distribution. To explain the total dust masses in ALMA-detected z > 7 galaxies, the following two solutions are possible: (i) high dust condensation efficiency in stellar ejecta, and (ii) efficient accretion (dust growth by accreting the gas-phase metals in the interstellar medium). We find that these two scenarios predict significantly different grain size distributions: in (i), the dust is dominated by large grains (a 0.1 µm, where a is the grain radius), while in (ii), the small-grain (a 0.01 µm) abundance is significantly enhanced by accretion. Accordingly, extinction curves are expected to be much steeper in (ii) than in (i). Thus, we conclude that extinction curves provide a viable way to distinguish the dominant dust sources in the early phase of galaxy evolution.

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“…Nanni et al 2013;Dell'Agli et al 2017). It has been believed for a long time that post-AGB stars and PNe belong to only one of the two chemical branches (C-rich or O-rich) mentioned above.…”

Section: Introductionmentioning

confidence: 99%

C/O ratios in planetary nebulae with dual-dust chemistry from faint optical recombination lines

García‐Rojas

Delgado-Inglada

García–Hernández

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present deep high-resolution (R∼15,000) and high-quality UVES optical spectrophotometry of nine planetary nebulae with dual-dust chemistry. We compute physical conditions from several diagnostics. Ionic abundances for a large number of ions of N, O, Ne, S, Cl, Ar, K, Fe and Kr are derived from collisionally excited lines. Elemental abundances are computed using state-of-the-art ionization correction factors. We derive accurate C/O ratios from optical recombination lines. We have re-analyzed additional high-quality spectra of 14 PNe from the literature following the same methodology. Comparison with asymptotic giant branch models reveal that about half of the total sample objects are consistent with being descendants of low-mass progenitor stars (M < 1.5 M ). Given the observed N/O, C/O, and He/H ratios, we cannot discard that some of the objects come from more massive progenitor stars (M > 3-4 M ) that have suffered a mild HBB. None of the objects seem to be descendant of very massive progenitors. We propose that in most of the planetary nebulae studied here, the PAHs have been formed through the dissociation of the CO molecule. The hypothesis of a last thermal pulse that turns O-rich PNe into C-rich PNe is discarded, except in three objects, that show C/O>1. We also discuss the possibility of a He pre-enrichment to explain the most Heenriched objects. We cannot discard another scenarios like extra mixing, stellar rotation or binary interactions to explain the chemical abundances behaviour observed in our sample.

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Asymptotic giant branch and super-asymptotic giant branch stars: modelling dust production at solar metallicity

Cited by 49 publications

References 52 publications

Galactic Archaeology at High Redshift: Inferring the Nature of GRB Host Galaxies from Abundances

Galactic Archaeology at High Redshift: Inferring the Nature of GRB Host Galaxies from Abundances

Expected dust grain-size distributions in galaxies detected by ALMA at z > 7

C/O ratios in planetary nebulae with dual-dust chemistry from faint optical recombination lines

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