Ages of Dwarfs in the Solar Neighborhood: Considering C and O Enhancements

Xunzhou, Chen; Zhishuai, Ge; Yuqin, Chen; Shaolan, Bi; Jie, Yu; Tanda, Li; Yaguang, Li; Ferguson, Ferguson J.W.; Jinghua, Zhang; Yaqian, Wu

doi:10.3847/1538-4357/ab66c7

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Ages of Dwarfs in the Solar Neighborhood: Considering C and O Enhancements

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Jie, Yu
Max Planck Institute for Solar System Research, Max Planck Society;

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Xunzhou, C., Zhishuai, G., Yuqin, C., Shaolan, B., Jie, Y., Tanda, L., et al. (2020). Ages of Dwarfs in the Solar Neighborhood: Considering C and O Enhancements. The Astrophysical Journal, 889(2): 157. doi:10.3847/1538-4357/ab66c7.

Cite as: https://hdl.handle.net/21.11116/0000-0006-F53A-5

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.