The evolution of lithium in FGK dwarf stars

Andrés, F. Llorente de; Chavero, C.; Reza, R. de la; Roca-Fàbrega, S.; Cifuentes, C.

doi:10.1051/0004-6361/202141339

Cited by 11 publications

(3 citation statements)

References 86 publications

(100 reference statements)

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“…Bouma et al (2021) recently used Li and rotation period (Prot) measurements of NGC 2516 members to confirm the existence of the 500 pclong tidal tails discovered by Meingast et al (2021), finding that the Li-rotation connection is enduring, even in the extended structures. Llorente de Andrés et al (2021) recently compiled Li and v sin i measurements for FGK-type members of dozens of clusters and associations and computed a v sin i threshold, separating Li-rich and Li-poor stars, which decreases with age.…”

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confidence: 99%

The Gaia-ESO survey: Constraining evolutionary models and ages for young low mass stars with measurements of lithium depletion and rotation

Binks

Jeffries

Sacco

et al. 2022

Monthly Notices of the Royal Astronomical Society

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A growing disquiet has emerged in recent years that standard stellar models are at odds with observations of the colour-magnitude diagrams (CMDs) and lithium depletion patterns of pre main sequence (PMS) stars in clusters. In this work we select 1,246 high probability K/M-type constituent members of 5 young open clusters (5–125 Myr) in the Gaia-ESO Survey to test a series of models that use standard input physics and others that incorporate surface magnetic fields or cool starspots. We find that: standard models provide systematically under-luminous isochrones for low-mass stars in the CMD and fail to predict Li-depletion of the right strength at the right colour; magnetic models provide better CMD fits with isochrones that are ∼1.5 − 2 times older, and provide better matches to Li depletion patterns. We investigate how rotation periods, most of which are determined here for the first time from Transiting Exoplanet Survey Satellite data, correlate with CMD position and Li. Among the K-stars in the older clusters we find the brightest and least Li-depleted are the fastest rotators, demonstrating the classic ‘Li-rotation connection’ for the first time at ∼35 Myr in NGC 2547, and finding some evidence that it exists in the early M-stars of NGC 2264 at <10 Myr. However, the wide dispersion in Li depletion observed in fully-convective M-dwarfs in the γ Vel cluster at ∼20 Myr appears not to be correlated with rotation and is challenging to explain without a very large (>10 Myr) age spread.

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confidence: 99%

The Gaia-ESO survey: Constraining evolutionary models and ages for young low mass stars with measurements of lithium depletion and rotation

Binks

Jeffries

Sacco

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…A full description of our sample was given in our previous works (Chavero et al 2019;Llorente de Andrés et al 2021;Roca-Fàbrega et al 2021, hereafter, CH19, LA21, and RF21, respectively). Table A.1 is complementary to the table published in our previous catalogue (see LA21).…”

Section: Stellar Samplementioning

confidence: 99%

The evolution of lithium in FGK dwarf stars

de Andrés,

de la Reza,

Cruz

et al. 2024

A&A

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This work aims to investigate the behaviour of the lithium abundance in stars with and without detected planets. Our study is based on a sample of 1332 FGK main-sequence stars with measured lithium abundances, for 257 of which planets were detected. Our method reviews the sample statistics and is addressed specifically to the influence of tides and orbital decay, with special attention to planets on close orbits, whose stellar rotational velocity is higher than the orbital period of the planet. In this case, tidal effects are much more pronounced. The analysis also covers the orbital decay on a short timescale, with planets spiralling into their parent star. Furthermore, the sample allows us to study the relation between the presence of planets and the physical properties of their host stars, such as the chromospheric activity, metallicity, and lithium abundance. In the case of a strong tidal influence, we cannot infer from any of the studies described that the behaviour of Li differs between stars that host planets and those that do not. Our sample includes stars with super-solar metallicity ( Fe/H >0.15\,dex) and a low lithium abundance (A(Li) <1.0\,dex). This enabled us to analyse scenarios of the origin and existence of these stars. Considering the possible explanation of the F dip, we show that it is not a plausible scenario. Our analysis is based on a kinematic study and concludes that the possible time that elapsed in the travel from their birth places in the central regions of the Galaxy to their current positions in the solar neighbourhood is not enough to explain the high lithium depletion. It is remarkable that those of our high-metallicity low-lithium stars with the greatest eccentricity (e>0.2) are closest to the Galactic centre. A dedicated study of a set of high-metallicity low-Li stars is needed to test the migration-depletion scenario.

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“…On the other hand, CCs such as Li (Llorente de Andrés et al 2021) or the ratio [C/N] (Casali et al 2019;Jofré 2021) are known in the literature. These CCs are based on stellar evolution and they are not considered for this work.…”

Section: Introductionmentioning

confidence: 99%

Stellar dating using chemical clocks and Bayesian inference

Moya

Sarro

Delgado-Mena

et al. 2022

A&A

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Context. Dating stars is a major challenge with a deep impact on many astrophysical fields. One of the most promising techniques for this is using chemical abundances. Recent space- and ground-based facilities have improved the quantity of stars with accurate observations. This has opened the door for using Bayesian inference tools to maximise the information we can extract from them. Aims. Our aim is to present accurate and reliable stellar age estimates of FGK stars using chemical abundances and stellar parameters. Methods. We used one of the most flexible Bayesian inference techniques (hierarchical Bayesian models) to exceed current possibilities in the use of chemical abundances for stellar dating. Our model is a data-driven model. We used a training set that has been presented in the literature with ages estimated with isochrones and accurate stellar abundances and general characteristics. The core of the model is a prescription of certain abundance ratios as linear combinations of stellar properties including age. We gathered four different testing sets to assess the accuracy, precision, and limits of our model. We also trained a model using chemical abundances alone. Results. We found that our age estimates and those coming from asteroseismology, other accurate sources, and also with ten Gaia benchmark stars agree well. The mean absolute difference of our estimates compared with those used as reference is 0.9 Ga, with a mean difference of 0.01 Ga. When using open clusters, we reached a very good agreement for Hyades, NGC 2632, Ruprecht 147, and IC 4651. We also found outliers that are a reflection of chemical peculiarities and/or stars at the limit of the validity ranges of the training set. The model that only uses chemical abundances shows slightly worse mean absolute difference (1.18 Ga) and mean difference (−0.12 Ga).

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The evolution of lithium in FGK dwarf stars

Cited by 11 publications

References 86 publications

The Gaia-ESO survey: Constraining evolutionary models and ages for young low mass stars with measurements of lithium depletion and rotation

The Gaia-ESO survey: Constraining evolutionary models and ages for young low mass stars with measurements of lithium depletion and rotation

The evolution of lithium in FGK dwarf stars

Stellar dating using chemical clocks and Bayesian inference

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