Star Formation Timescales of the Halo Populations from Asteroseismology and Chemical Abundances

We combine asteroseismology, optical high-resolution spectroscopy, and kinematic analysis for 26 halo red giant branch stars in the Kepler field in the range of −2.5 < [Fe/H] < −0.6. After applying theoretically motivated corrections to the seismic scaling relations, we obtain an average mass...

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Bibliographic Details
Published in:The Astrophysical journal 2021-05, Vol.912 (1), p.72
Main Authors: Matsuno, Tadafumi, Aoki, Wako, Casagrande, Luca, Ishigaki, Miho N., Shi, Jianrong, Takata, Masao, Xiang, Maosheng, Yong, David, Li, Haining, Suda, Takuma, Xing, Qianfan, Zhao, Jingkun
Format: Article
Language:English
Subjects:
Abundance
Astrophysics
Asymptotic giant branch stars
Chemical evolution
Dispersion
Iron
Magnesium
Milky Way
Red giant stars
Spectroscopy
Star & galaxy formation
Star formation
Stars
Stars & galaxies
Stellar age
Stellar evolution
Stellar mass
Stellar seismology
Supernovae
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Summary:We combine asteroseismology, optical high-resolution spectroscopy, and kinematic analysis for 26 halo red giant branch stars in the Kepler field in the range of −2.5 < [Fe/H] < −0.6. After applying theoretically motivated corrections to the seismic scaling relations, we obtain an average mass of 0.97 ± 0.03 M ⊙ for our sample of halo stars. Although this maps into an age of ∼7 Gyr, significantly younger than independent age estimates of the Milky Way stellar halo, we considered this apparently young age to be due to the overestimation of stellar mass in the scaling relations. There is no significant mass dispersion among lower red giant branch stars (log g > 2), which constrains the relative age dispersion to
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abeab2