The mass-loss, expansion velocities, and dust production rates of carbon stars in the Magellanic Clouds

Nanni, Ambra; Groenewegen, M. A. T.; Aringer, B.; Rubele, Stefano; Bressan, A.; Loon, Jacco Th. van; Goldman, S. R.; Boyer, Martha L.

doi:10.1093/mnras/stz1255

Cited by 45 publications

(82 citation statements)

References 110 publications

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“…Compared with the LMC, the SMC is more deficient in C-AGB stars with thick dust shells. Also Nanni et al (2019) found a group of C-AGB stars with high mass-loss rates in the LMC that is not present in the SMC. This could be because the initial masses of C-AGB stars in the LMC are larger than those in the SMC (Ventura et al 2016).…”

Section: Discussion: Agb Stars In Our Galaxy and The Magellanic Cloudsmentioning

confidence: 93%

“…The gas-to-dust ratio (Ψ) is generally estimated to be 50 -200 in our Galaxy (the average Ψ is about 100) and Ψ tends to decrease for a higher metallicity (Draine et al 2007). Nanni et al (2019) found that Ψ is larger in the Magellanic Clouds (Ψ ∼ 700) probably due to the lower metallicity. Figure 12.…”

Section: Infrared Two-color Diagramsmentioning

confidence: 94%

“…Groenewegen & Sloan (2018) investigated mass loss and luminosity in a sample of AGB stars in our Galaxy, the Magellanic Clouds, and other nearby galaxies. Nanni et al (2019) investigated the mass-loss and dust production rates of C-AGB stars in the Magellanic Clouds and found a tail of extreme mass-losing C-AGB stars in the LMC with low gas-to-dust ratios that is not present in the SMC.…”

Section: Introductionmentioning

confidence: 99%

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Infrared Properties of Asymptotic Giant Branch Stars in Our Galaxy and the Magellanic Clouds

Suh

2020

ApJ

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We investigate infrared properties of asymptotic giant branch (AGB) stars in our Galaxy and the Magellanic Clouds using various infrared observational data and theoretical models. We use catalogs for the sample of 4996 AGB stars in our Galaxy and about 39,000 AGB stars in the Magellanic Clouds from the available literature. For each object in the sample, we cross-identify the 2MASS, WISE, and Spitzer counterparts. To compare the physical properties of O-rich and C-rich AGB stars in our Galaxy and the Magellanic Clouds, we present IR two color diagrams (2CDs) using various photometric data. We perform radiative transfer model calculations for AGB stars using various possible parameters of central stars and dust shells. Using dust opacity functions of amorphous silicate and amorphous carbon, the theoretical dust shell models can roughly reproduce the observations of AGB stars on various IR 2CDs. Compared with our Galaxy, we find that the Magellanic Clouds are deficient in AGB stars with thick dust shells. Compared with the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC) is more deficient in AGB stars with thick dust shells. This could be because the Magellanic Clouds are more metal poor than our Galaxy and the LMC is more metal rich than the SMC. We also present IR properties of known pulsating variable. Investigating the magnitude distributions at MIR bands for AGB stars in the Magellanic Clouds, we find that the SMC is more deficient in the bright AGB stars at MIR bands compared with the LMC. features. The spectral energy distributions (SEDs) of O-AGB stars show 10 µm and 18 µm features due to amorphous silicate dust. Low mass-loss rate O-AGB (LMOA; M ∼ 10 −8 − 10 −6 M /yr) stars with thin dust envelopes show the emission features and high mass-loss rate O-AGB (HMOA;Ṁ ∼ 10 −5 −10 −4 M /yr) stars with thick dust envelopes show the absorption features at the same wavelengths (e.g., Suh 1999). The detailed SEDs of LMOA stars can be reproduced by the silicate dust with a mixture of amorphous alumina (Al 2 O 3

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Section: Discussion: Agb Stars In Our Galaxy and The Magellanic Cloudsmentioning

confidence: 93%

Section: Infrared Two-color Diagramsmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

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Infrared Properties of Asymptotic Giant Branch Stars in Our Galaxy and the Magellanic Clouds

Suh

2020

ApJ

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“…A different and complementary approach was followed by Dell'Agli et al (2014a, 2015a, who used stellar evolutionary tracks to characterize the individual sources, in terms of mass, chemical composition and formation epoch of the progenitors, and of the amount and mineralogy of the dust in the circumstellar envelope. Nanni et al (2019) used a similar analysis to derive an estimate of the overall dust production rate by evolved stars in the Magellanic Clouds (hereinafter MC).…”

Section: Introductionmentioning

confidence: 99%

Characterization of M-stars in the LMC in the JWST era

Marini

Dell’Agli

Criscienzo

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the M-type asymptotic giant branch (AGB) population of the Large Magellanic Cloud (LMC) by characterizing the individual sources in terms of the main properties of the progenitors and of the dust present in the circumstellar envelope. To this aim we compare the combination of the spectroscopic and photometric data collected by Spitzer, complemented by additional photometric results available in the literature, with results from AGB modelling that include the description of dust formation in the wind. To allow the interpretation of a paucity stars likely evolving through the post-AGB phase, we extended the available evolutionary sequences to reach the PN phase. The main motivation of the present analysis is to prepare the future observations of the evolved stellar populations of Local Group galaxies that will be done by the James Webb Space Telescope (JWST), by identifying the combination of filters that will maximize the possibilities of characterizing the observed sources. The present results show that for the M-star case the best planes to be used for this purpose are the colour magnitude ([F770W]-[F2550W], [F770W]) and (K S -[F770W], [F770W]) planes. In these observational diagrams the sequences of low-mass stars evolving in the AGB phases before the achievement of the C-star stage and of massive AGBs experiencing hot bottom burning are clearly separated and peculiar sources, such as post-AGB, dual-dust chemistry and iron-dust stars can be easily identified.

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“…A fundamental problem in astrophysics is understanding how stars in the late stages of their evolution enrich galaxies with dust and freshly fused elements. It is currently uncertain what the relative contributions are from the most massive stars, which will explode as supernovae, creating new elements but likely destroying dust, compared to lower-mass stars (e.g., Micelotta et al 2018;Dell'Agli et al 2019;Nanni et al 2019). Low-and intermediate-mass stars create dust grains in the cool outer layers of their atmospheres, and the radiation pressure on these grains then helps drive the mass-loss process (e.g., Höfner & Olofsson 2018; Groenewegen & Sloan 2018, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Stellar Pulsation and the Production of Dust and Molecules in Galactic Carbon Stars

Kraemer

Sloan

Keller

et al. 2019

ApJ

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New infrared spectra of 33 Galactic carbon stars from FORCAST on SOFIA reveal strong connections between stellar pulsations and the dust and molecular chemistry in their circumstellar shells. A sharp boundary in overall dust content, which predominantly measures the amount of amorphous carbon, separates the semi-regular and Mira variables, with the semi-regulars showing little dust in their spectra and the Miras showing more. In semi-regulars, the contribution from SiC dust increases rapidly as the overall dust content grows, but in Miras, the SiC dust feature grows weaker as more dust is added. A similar dichotomy is found with the absorption band from CS at ∼7.3 µm, which is generally limited to semi-regular variables. Observationally, these differences make it straightforward to distinguish semiregular and Mira variables spectroscopically without the need for long-term photometric observations or knowledge of their distances. The rapid onset of strong SiC emission in Galactic carbon stars in semi-regulars variables points to a different dust-condensation process before strong pulsations take over. The break in the production of amorphous carbon between semi-regulars and Miras seen in the Galactic sample is also evident in Magellanic carbon stars, linking strong pulsations in carbon stars to the strong mass-loss rates which will end their lives as stars across a wide range of metallicities.

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The mass-loss, expansion velocities, and dust production rates of carbon stars in the Magellanic Clouds

Cited by 45 publications

References 110 publications

Infrared Properties of Asymptotic Giant Branch Stars in Our Galaxy and the Magellanic Clouds

Infrared Properties of Asymptotic Giant Branch Stars in Our Galaxy and the Magellanic Clouds

Characterization of M-stars in the LMC in the JWST era

Stellar Pulsation and the Production of Dust and Molecules in Galactic Carbon Stars

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