Ages of dwarfs in the solar neighborhood: considering C and O enhancements
Chen, Xunzhou Ge, Zhishuai Chen, Yuqin Bi, Shaolan Yu, Jie Li, Tanda Ferguson, Jason W. Zhang, Jinghua Wu, Yaqian
Chen, Xunzhou
Ge, Zhishuai
Chen, Yuqin
Bi, Shaolan
Yu, Jie
Li, Tanda
Ferguson, Jason W.
Zhang, Jinghua
Wu, Yaqian
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Authors
Chen, Xunzhou
Ge, Zhishuai
Chen, Yuqin
Bi, Shaolan
Yu, Jie
Li, Tanda
Ferguson, Jason W.
Zhang, Jinghua
Wu, Yaqian
Ge, Zhishuai
Chen, Yuqin
Bi, Shaolan
Yu, Jie
Li, Tanda
Ferguson, Jason W.
Zhang, Jinghua
Wu, Yaqian
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2020-02-04
Type
Article
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Keywords
Disks,Stars,Solar neighbourhood
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Citation
Chen, Xunzhou; Ge, Zhishuai; Chen, Yuqin; Bi, Shaolan; Yu, Jie; Li, Tanda; Ferguson, Jason W.; Zhang, Jinghua; Wu, Yaqian. 2020. Ages of dwarfs in the solar neighborhood: considering C and O enhancements. Astrophysical Journal, vol. 889:no. 2:art. no. 157
Abstract
Precise stellar ages of stars are necessary to study the evolution of the Milky Way. The age determination is significantly affected by C and O abundances of stars due to their contribution to the overall metallicity and opacity. On the basis of C and O abundances derived from high-resolution observations, we determine the ages of 148 FGK-type dwarfs in the solar neighborhood by considering C and O enhancements individually. Our results show that using C and O enhancements individually could affect the age determination of the high-α population, especially for stars with [O/α] > 0.2 dex, making them about 1 Gyr younger compared to the results using traditional α-enhanced models. This results in a steeper slope in the age-[α/Fe] relation for the high-α population (changes from 0.0339 ± 0.0075 to 0.0436 ± 0.0086), indicating a higher formation rate. We find no tight relation between age and [α/Fe] or [O/Fe] in the high-α populations. The distribution of space velocity for young α-rich stars shows that they are more likely characterized to the low-α populations.
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Institute of Physics Publishing
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Astrophysical Journal;vol.889:no.2:art. no.157
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0004-637X