Dust from asymptotic giant branch stars: relevant factors and modelling uncertainties

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

doi:10.1093/mnras/stu028

Cited by 96 publications

(184 citation statements)

References 66 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%

“…The need for some extra-mixing was invoked by Herwig et al (2007), based on numerical simulations and, more recently, by Kamath et al (2012), on the basis of the comparison between the observed and expected transition luminosity from O-rich to C-rich stars in clusters in the MC. Extra-mixing from the bottom of the envelope has been used in almost the totality of the most recent works on AGB modelling (Cristallo et al 2009;Weiss & Ferguson 2009;Ventura et al 2014a;García-Hernández et al 2016).…”

Section: Pne In the Smc: A Further Test For Agb Modellingmentioning

confidence: 99%

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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%

Section: Pne In the Smc: A Further Test For Agb Modellingmentioning

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 consider that Fig. 4 but showing the predictions of stellar evolution models for Z = 0.001 (green squares) by Ventura et al (2013Ventura et al ( , 2014b and Z = 0.004 (red triangles) by Ventura et al (2014a, V14). See text for discussion.…”

Section: Testing Other Stellar Evolution Modelsmentioning

confidence: 99%

“…8 and 9 we explore the behaviour of 12 + log (N/H) vs. 12 + log (He/H) and log (N/O), and 12 + log (Ne/H) vs. 12 + log (O/H) with models by Ventura et al (2013Ventura et al ( , 2014b Ventura et al (2013Ventura et al ( , 2014b and Z = 0.004 (red triangles) by Ventura et al (2014a, V14). See text for discussion.…”

Section: Testing Other Stellar Evolution Modelsmentioning

confidence: 99%

The planetary nebulae and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis

García‐Rojas

Peña

Flores-Durán

et al. 2016

A&A

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Aims. The chemical behaviour of an ample sample of planetary nebulae (PNe) in NGC 6822 is analysed.Methods. Spectrophotometric data of 11 PNe and two H  regions were obtained with the OSIRIS spectrograph attached to the Gran Telescopio Canarias. Data for other 13 PNe and three H  regions were retrieved from the literature. Physical conditions and chemical abundances of O, N, Ne, Ar, and S were derived in a consistent way for 19 PNe and 4 H  regions.Results. Abundances in the PNe sample are widely distributed showing 12 + log (O/H) from 7.4 to 8.2 and 12 + log (Ar/H) from 4.97 to 5.80. Two groups of PNe can be differentiated: one old with low metallicity (12 + log (O/H) < 8.0 and 12 + log (Ar/H) < 5.7) and another younger one with metallicities similar to the values for H  regions. The old objects are distributed in a larger volume than the young ones. An important fraction of PNe (over 30%) was found to be highly N-rich (Peimbert Type I PNe). Such PNe occur at any metallicity. In addition, about 60% of the sample presents high ionization (He ++ /He ≥ 0.1), possessing a central star with effective temperature higher than 100 000 K. Possible biases in the sample are discussed. From comparison with stellar evolution models by Karakas (2010) and Fishlock et al. (2014) of the observed N/O abundance ratios, our PNe should have had initial masses that are lower than 4 M , although if the comparison is made with Ne vs. O abundances, the initial masses should have been lower than 2 M . It appears that these models of stars of 2−3 M are producing too much 22 Ne in the stellar surface at the end of the AGB. On the other hand, the comparison with another set of stellar evolution models with a different treatment of convection and on the assumptions about the overshoot of the convective core during the core H-burning phase, provided there is reasonable agreement between the observed and predicted N/O and Ne/H ratios if initial masses of more massive stars are about 4 M .

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“…these stars. Ventura et al [23][24], Di Criscienzo et al [25], and Ventura et al [26] have computed the composition and grain size distributions of dust produced by stars with masses 0.8 < M * < 8 M at different metallicities (3 × 10 −4 < Z < 8 × 10 −3 ). By starting from these results, to improve the presented analysis, it would be useful to compute the extinction curve of AGB and super AGB stars.…”

Section: Discussionmentioning

confidence: 99%

The extinction law at high redshift

Gallerani¹

2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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We analyze the optical-near infrared spectra of 33 quasars with redshifts 3.9 < z < 6.4 with the aim of investigating the properties of dust extinction at these cosmic epochs. The Small Magellanic Cloud (SMC) extinction curve has been used to reproduce the dust reddening of most quasars at z < 2.2; the main goal of this work is to investigate whether this curve provides a good prescription for describing dust extinction at higher redshifts or not. We fit the observed spectra with synthetic absorbed quasar templates obtained by varying the intrinsic slope (α), the absolute extinction (A 3000 ) and by using grid of empirical and theoretical extinction curves. We find that seven quasars in our sample require substantial extinction (A 3000 > 0.8), and are characterized by very steep intrinsic slopes (α < −2.3). All of the individual quasars require extinction curves deviating from the SMC, with a tendency to flatten at lambda < 2000 Å (rest frame). We obtain a mean extinction curve at z > 4 by averaging the extinction curves inferred for individual quasars. With a confidence level exceeding 95%, we can conclude that the extinction curve of BAL quasars deviates from that of the SMC. The different extinction curves in quasars at z > 4 relative to quasars at lower redshift suggest either a different dust production mechanism at high redshift, or a different mechanism of processing dust into the interstellar medium (ISM). We have applied the same method of analysis to the optical/near-infrared (IR) afterglow of GRB050904 at z = 6.3. In this case, we find that the SMC extinction curve and a supernova-type one provide equally good fit to the data at all epochs, with an average amount of dust absorption at λ rest = 3000 Å of A 3000 = 0.25 ± 0.07 mag. These results indicate both that the primeval galaxy at z = 6.3 hosting this GRB has already enriched its ISM with dust, and that it is not possible to characterize the nature of dust suppliers in this source. PoS(LCDU 2013)010The extinction law at high redshift Simona Gallerani Evolution of dust properties through cosmic timesExtensive measurements of the local interstellar extinction exist along hundreds of lines of sight in the Milky Way (MW) [1], and along tens of lines of sight in the Large Magellanic Cloud (LMC) and in the Small Magellanic Cloud (SMC) [2]. In particular, the extinction curve of the SMC is generally adopted also to describe the dust reddening of local QSOs [3][4] since the broad bump at 2175 Å, which is characteristic of the MW and LMC extinction curve, but absent in the SMC, has never been conclusively seen from quasar host galaxy dust. Recently, extinction curves have been also studied in several quasar and gamma ray bursts even at the highest redshifts probed so far [5][6][7][8][9][10][11][12]. These kind of studies allow to investigate whether the properties of dust evolve through cosmic times. Here, we briefly summarize the results obtained by Gallerani et al. [7] and Stratta et al.[9] and we discuss possible improvements for future investigations. ...

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Dust from asymptotic giant branch stars: relevant factors and modelling uncertainties

Cited by 96 publications

References 66 publications

Planetary nebulae in the Small Magellanic Cloud

Planetary nebulae in the Small Magellanic Cloud

The planetary nebulae and H II regions in NGC 6822 revisited. Clues to AGB nucleosynthesis

The extinction law at high redshift

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