AGB stars in the SMC: evolution and dust properties based on Spitzer observations

被引:49
作者
Dell'Agli, F. [1 ,2 ]
Garcia-Hernandez, D. A. [3 ,4 ]
Ventura, P. [2 ]
Schneider, R. [2 ]
Di Criscienzo, M. [2 ]
Rossi, C. [1 ]
机构
[1] Univ Roma La Sapienza, Dipartimento Fis, I-00143 Rome, Italy
[2] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy
[3] Inst Astrofis Canarias, E-38205 Tenerife, Spain
[4] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
基金
欧洲研究理事会;
关键词
stars: abundances; stars: AGB and post-AGB; ISM: abundances; ASYMPTOTIC GIANT BRANCH; SMALL-MAGELLANIC-CLOUD; MASS-LOSS; LOW-METALLICITY; STELLAR WINDS; MINERAL FORMATION; GALAXY EVOLUTION; MOLECULAR OPACITIES; OPTICAL-PROPERTIES; FORMATION HISTORY;
D O I
10.1093/mnras/stv2298
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We study the population of asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC) by means of full evolutionary models of stars of mass 1 M-circle dot <= M <= 8 M-circle dot, evolved through the thermally pulsing phase. The models also account for dust production in the circumstellar envelope. We compare Spitzer infrared colours with results from theoretical modelling. We show that similar to 75 per cent of the AGB population of the SMC is composed by scarcely obscured objects, mainly stars of mass M <= 2 M-circle dot at various metallicity, formed between 700 Myr and 5 Gyr ago; similar to 70 per cent of these sources are oxygen-rich stars, while similar to 30 per cent are C-stars. The sample of the most obscured AGB stars, accounting for similar to 25 per cent of the total sample, is composed almost entirely by carbon stars. The distribution in the colour-colour ([3.6] - [4.5], [5.8] - [8.0]) and colour-magnitude ([3.6] - [8.0], [8.0]) diagrams of these C-rich objects, with a large infrared emission, traces an obscuration sequence, according to the amount of carbonaceous dust in their surroundings. The overall population of C-rich AGB stars descends from 1.5-2 M-circle dot stars of metallicity Z = 4 x 10(-3), formed between 700 Myr and 2 Gyr ago, and from lower metallicity objects, of mass below 1.5 M-circle dot, 2-5 Gyr old. We also identify obscured oxygen-rich stars (M similar to 4-6 M-circle dot) experiencing hot bottom burning. The differences between the AGB populations of the SMC and LMC are also commented.
引用
收藏
页码:4235 / 4249
页数:15
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