Chemical Evolution in the Milky Way: Rotation-based Ages for APOGEE-Kepler Cool Dwarf Stars
We use models of stellar angular momentum evolution to determine ages for ∼500 stars in the APOGEE-Kepler Cool Dwarfs sample. We focus on lower-main-sequence stars, where other age-dating tools become ineffective. Our age distributions are compared to those derived from asteroseismic and giant sampl...
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Published in: | The Astrophysical journal Vol. 888; no. 1; pp. 43 - 59 |
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Main Authors: | , , , , , , , |
Format: | Journal Article |
Language: | English |
Published: |
Philadelphia
The American Astronomical Society
01-01-2020
IOP Publishing |
Subjects: | |
Online Access: | Get full text |
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Summary: | We use models of stellar angular momentum evolution to determine ages for ∼500 stars in the APOGEE-Kepler Cool Dwarfs sample. We focus on lower-main-sequence stars, where other age-dating tools become ineffective. Our age distributions are compared to those derived from asteroseismic and giant samples and solar analogs. We are able to recover gyrochronological ages for old, lower-main-sequence stars, a remarkable improvement over prior work in hotter stars. Under our model assumptions, our ages have a median relative uncertainty of 14%, comparable to the age precision inferred for more massive stars using traditional methods. We investigate trends of Galactic -enhancement with age, finding evidence of a detection threshold between the age of the oldest -poor stars and that of the bulk -rich population. We argue that gyrochronology is an effective tool reaching ages of 10-12 Gyr in K and early M dwarfs. Finally, we present the first effort to quantify the impact of detailed abundance patterns on rotational evolution. We estimate a ∼15% bias in age for cool, -enhanced (+0.4 dex) stars when standard solar-abundance-pattern rotational models are used for age inference, rather than models that appropriately account for -enrichment. |
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Bibliography: | AAS19525 Stars and Stellar Physics |
ISSN: | 0004-637X 1538-4357 |
DOI: | 10.3847/1538-4357/ab5c24 |