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

Ferrarotti, A. S.; Gail, H. P.

doi:10.1051/0004-6361:20041198

Cited by 322 publications

(555 citation statements)

References 80 publications

(111 reference statements)

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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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“…We discuss this dependence in detail in the following. Ferrarotti & Gail (2006) performed extensive calculations of dust formation by low-and intermediate-mass stars during their AGB evolution for a wide range of initial stellar masses and metallicities, making these models the most suitable for use in evolutionary dust models. Their work is based on detailed theoretical models of non-equilibrium dust condensation in stellar winds, developed in a series of earlier papers (Gail & Sedlmayr 1987Ferrarotti & Gail 2001Gail 2003).…”

Section: Dust Formation By Low-and Intermediate-mass Starsmentioning

confidence: 99%

Dust input from AGB stars in the Large Magellanic Cloud

Zhukovska

Henning

2013

A&A

112

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Aims. The dust-forming population of AGB stars and their input to the interstellar dust budget of the Large Magellanic Cloud (LMC) are studied with evolutionary dust models with the main goals (1) to investigate how the amount and composition of dust from AGB stars vary over the galactic history; (2) to characterise the mass and metallicity distribution of the present population of AGB stars; (3) to quantify the contribution of AGB stars of different mass and metallicity to the present stardust population in the interstellar medium (ISM). Methods. We used models of the stardust lifecycle in the ISM developed and tested for the solar neighbourhood. The first global spatially resolved reconstruction of the star formation history of the LMC from the Magellanic Clouds Photometric Survey was employed to calculate the stellar populations in the LMC. Results. The dust input from AGB stars is dominated by carbon grains from stars with masses 4 M almost during the entire history of the LMC. The production of silicate, silicon carbide, and iron dust is delayed until the ISM is enriched to about half the present metallicity in the LMC. For the first time, theoretically calculated dust production rates of AGB stars are compared with those derived from infrared observations of AGB stars for the entire galaxy. We find good agreement within scatter of various observational estimates. We show that the majority of silicate and iron grains in the present stardust population originate from a small population of intermediate-mass stars consisting of only 4% of the total number of stars, whereas in the solar neighbourhood they originate from low-mass stars. With models of the lifecycle of stardust grains in the ISM we confirm the strong discrepancy between dust input from stars and the existing interstellar dust mass in the LMC reported previously.

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“…The dust mass after the wind depends on several assumptions (e.g. fate of the dust in the wind stage, wind mass loading, sputtering in the hot medium) and we are planning to improve upon the Calura et al (2008) In low and intermediate-mass stars, dust is produced during the Asymptotic Giant Branch (AGB) phase (Ferrarotti & Gail 2006, and references therein). We assume that dust formation depends mainly on the composition of the stellar envelopes.…”

Section: Stellar Dustmentioning

confidence: 99%

The chemical evolution of elliptical galaxies with stellar and QSO dust production

Pipino

Fan

Matteuccí

et al. 2010

A&A

145

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Context. The presence of dust strongly affects the way we see galaxies and also the chemical abundances we measure in gas. It is therefore important to study the chemical evolution of galaxies by taking into account dust evolution. Aims. We aim at performing a detailed study of abundance ratios of high redshift objects and their dust properties. We focus on Lyman-Break galaxies (LBGs) and Quasar (QSO) hosts as likely progenitors of low-and high-mass present-day elliptical galaxies, respectively. Methods. We have adopted a chemical evolution model for elliptical galaxies taking into account the dust production from low and intermediate mass stars, supernovae Ia, supernovae II, QSOs and both dust destruction and accretion processes. By means of such a model we have followed the chemical evolution of ellipticals of different baryonic masses. Our model complies with chemical downsizing.Results. We made predictions for the abundance ratios versus metallicity trends for models of differing masses that can be used to constrain the star formation rate, initial mass function and dust mass in observed galaxies. We predict the existence of a high redshift dust mass-stellar mass relationship. We have found a good agreement with the properties of LBGs if we assume that they formed at redshift z = 2-4. In particular, a non-negligible amount of dust is needed to explain the observed abundance pattern. We studied the QSO SDSS J114816, one of the most distant QSO ever observed (z = 6.4), and we have been able to reproduce the amount of dust measured in this object. The dust is clearly due to the production from supernovae and the most massive AGB stars as well as from the grain growth in the interstellar medium. The QSO dust is likely to dominate only in the very central regions of the galaxies and during the early development of the galactic wind.

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

Cited by 322 publications

References 80 publications

Planetary nebulae in the Small Magellanic Cloud

Planetary nebulae in the Small Magellanic Cloud

Dust input from AGB stars in the Large Magellanic Cloud

The chemical evolution of elliptical galaxies with stellar and QSO dust production

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