Dust Production and Mass Loss in the Galactic Globular Cluster 47 Tucanae

McDonald, Iain; Boyer, Martha L.; Loon, Jacco Th. van; Zijlstra, A. A.

doi:10.1088/0004-637x/730/2/71

Cited by 53 publications

(76 citation statements)

References 80 publications

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“…Iron is expected to efficiently condense in metallic iron dust in C-and S-stars from theoretical considerations (Gail & Sedlmayr 1999), but it has long remained undetected due to its featureless spectra. There is recent observational evidence that iron grains may be an important opacity source at low metallicities (McDonald et al 2010(McDonald et al , 2011. Since carbon is synthesized in AGB stars, while the abundances of other elements (O, Mg, Si, Fe) available for dust formation are determined by initial stellar abundances, there is a strong dependence of the dust mixture from AGB stars on their initial metallicity (e.g., Zijlstra et al 2006;Leisenring et al 2008).…”

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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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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“…Mass-loss rates acquired by method (3) make many assumptions, and represent instantaneous snapshots of very dynamic systems [7]. Method (1) is not widely used, due to the complexity in data collection and analysis.…”

Section: Is Dust-production Efficiency Constant?mentioning

confidence: 99%

“…Mass-loss rates for AGB stars may be significantly over-estimated. While a number of factors affect mass-loss rates derived from infrared spectra, the most important is likely to be the stellar outflow velocity [7]. If we are to understand the role of stellar mass loss in galactic ecology, it is vital we measure gas mass-loss rates and wind velocities of metal-poor stars.…”

Section: Future Workmentioning

confidence: 99%

Dust production by metal-poor stars

McDonald¹

2014

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

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I summarise work carried out on the differences in dust production by metal-poor stars, compared to canonical expectations from the Galaxy. Our conclusions are as follows. Dust may be more efficiently produced by low-mass, metal-poor stars due to their faster RGB evolution. The onset of dust production appears correlated with pulsation, which begins at slightly higher luminosities for metal-poor stars. The dust condensation sequence appears little changed for metal-poor carbon stars. Metal-poor oxygen-rich stars show marked changes in dust condensation products, with a dramatic shift occurring for globular cluster stars below [Fe/H] = -1. A lack of oxygen-rich AGB stars in globular clusters much below this metallicity currently prevents further analysis. We consider the mass-loss rate to be set by magneto-acoustic or pulsation processes on the stellar surface. Dust-driving may only become important at the highest dust-production rates where its primary role is to set the wind velocity. Future work should concentrate on obtaining gas massloss rates and wind velocities for AGB stars across a variety of dust-production rates, chemistries and metallicities to conclusively determine the role of dust in driving stellar winds.

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“…While a carbon star in the metal-poor Local Group galaxy Sculptor was found to still be rather dusty (Sloan et al 2009), little more has been revealed to settle the issue whether metalpoor carbon stars produce more or less dust than metal-rich counterparts. Much has been learnt about mass loss from RGB stars in globular clusters, though, with Origlia et al (2010) finding dust production low on the RGB whereas Boyer et al (2009Boyer et al ( , 2010 and McDonald et al (2009McDonald et al ( , 2011a find dust production to be confined to the tip of the RGB where RGB stars develop cool extended atmospheres and start to pulsate more vigorously. Momany et al (2011), in an independent study, cast their verdict in favour of the latter.…”

Section: Mass Loss From Red Giant Stars (J Van Loon)mentioning

confidence: 99%

Commission 35: Stellar Constitution

Charbonnel¹,

Limongi²,

D’Antona³

et al. 2011

Proc. IAU

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Commission 35 consists of members of the International Astronomical Union whose research is concerned with the structure and evolution of stars in all parts of the H-R diagram. Their interests range from various aspects of stellar interior physics, such as convection, diffusion, rotation, magnetic fields, to asteroseismology and the prediction of the evolutionary and nucleosynthetic histories of stars that are of vital importance for our understanding of stellar populations and galactic chemical evolution.

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Dust Production and Mass Loss in the Galactic Globular Cluster 47 Tucanae

Cited by 53 publications

References 80 publications

Dust input from AGB stars in the Large Magellanic Cloud

Dust input from AGB stars in the Large Magellanic Cloud

Dust production by metal-poor stars

Commission 35: Stellar Constitution

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