How accurate are stellar ages based on stellar models?

Lebreton, Y.; Goupil, M. J.; Montalbán, J.

doi:10.1051/eas/1465005

Cited by 31 publications

(23 citation statements)

References 117 publications

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“…We focus on evolved stars, and refer to Lebreton et al (2014), and references therein, for the case of main-sequence stars.…”

Section: From Precise To Accurate Stellar Propertiesmentioning

confidence: 99%

“…With the advent of the Kepler (Borucki et al 2010) and CoRoT (Baglin et al 2006) space missions, time series measuring stellar variability of very-high quality have become widely available. Analysis of these time series can deliver precise estimates of stellar ages Lebreton et al 2014;Meibom et al 2015;Metcalfe et al 2015;Miglio et al 2013b;Silva Aguirre et al 2015) -a quantity critical for reconstructing the history of the Milky Way. With the re-purposed Kepler mission K2 (Howell et al 2014) currently capturing solar-like oscillations Stello et al 2015) in a number of different galactic directions, and the future missions of TESS (Ricker et al 2014) and PLATO (Rauer et al 2014) adding to this, ages for many thousands of stars in many different galactic distances and directions present an exciting possibility.…”

Section: Introductionmentioning

confidence: 99%

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Asteroseismology of red giants: From analysing light curves to estimating ages

Davies

Miglio

2016

Astron Nachr

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Asteroseismology has started to provide constraints on stellar properties that will be essential to accurately reconstruct the history of the Milky Way. Here we look at the information content in data sets representing current and future space missions (CoRoT, Kepler, K2, TESS, and PLATO) for red giant stars. We describe techniques for extracting the information in the frequency power spectrum and apply these techniques to Kepler data sets of different observing length to represent the different space missions. We demonstrate that for KIC 12008916, a low-luminosity red giant branch star, we can extract useful information from all data sets, and for all but the shortest data set we obtain good constraint on the g-mode period spacing and core rotation rates. We discuss how the high precision in these parameters will constrain the stellar properties of stellar radius, distance, mass and age. We show that high precision can be achieved in mass and hence age when values of the g-mode period spacing are available. We caution that tests to establish the accuracy of asteroseismic masses and ages are still "work in progress".

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“…We focus on evolved stars, and refer to Lebreton et al (2014), and references therein, for the case of main-sequence stars.…”

Section: From Precise To Accurate Stellar Propertiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Asteroseismology of red giants: From analysing light curves to estimating ages

Davies

Miglio

2016

Astron Nachr

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“…The ages determined with different stellar model can deviate by ∼10% for young stars and from 50% up to 100% for older stars (Lebreton et al 2014a). Only asteroseismology in combination with stellar evolution models can provide the age of main-sequence stars with an accuracy better than 10% (Lebreton et al 2014b). If the observed system is a cluster member, the age of the star can also be inferred from the age of the cluster.…”

Section: Introductionmentioning

confidence: 99%

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Eigmüller¹,

Eislöffel²,

Csizmadia³

et al. 2016

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Only a few well characterized very low-mass M dwarfs are known today. Our understanding of M dwarfs is vital as these are the most common stars in our solar neighborhood. We aim to characterize the properties of a rare F+dM stellar system for a better understanding of the low-mass end of the Hertzsprung-Russel diagram. We used photometric light curves and radial velocity follow-up measurements to study the binary. Spectroscopic analysis was used in combination with isochrone fitting to characterize the primary star. The primary star is an early F-type main-sequence star with a mass of (1.493 ± 0.073) M e and a radius of (1.474 ± 0.040) R e . The companion is an M dwarf with a mass of (0.188 ± 0.014) M e and a radius of (0.234 ± 0.009) R e . The orbital period is (1.35121±0.00001) days. The secondary star is among the lowest-mass M dwarfs known to date. The binary has not reached a 1:1 spin-orbit synchronization. This indicates a young main-sequence binary with an age below ∼250 Myr. The mass-radius relation of both components are in agreement with this finding.

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“…However, they undergo phases with rapid change and/or experience pulsating episodes. Figure 1 in Lebreton et al (2014b), in these series, illustrates a Hertzprung-Russell diagram with different types of pulsation (a review on asteroseismology can be found in Cunha et al 2007). As a matter of fact, helioseismology has been a terrific tool to understand the internal structure of the Sun.…”

Section: Asteroseismologymentioning

confidence: 99%

“…Eventually CHEOPS, TESS and PLATO will add new information. Lebreton et al (2014b) discussed in depth asteroseismology and its application to the age-dating. We would like to emphasize few issues here, related to exoplanetary studies (see also subsection 3.6.1).…”

Section: Asteroseismologymentioning

confidence: 99%

Clusters: Age Scales for Stellar Physics

Barrado

2016

EAS Publications Series

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Abstract. Ages are key to truly understand a large plethora of astrophysical phenomena. On the other hand, stellar clusters are open windows to understand stellar evolution, specifically, the change with time and mass of different stellar properties. As such, they are our laboratories where different theories can be tested, but without accurate ages, our knowledge would impaired. We revisit here a large number of age-dating techniques and discuss their advantages and draw-backs. In addition, a step-by step process is suggested in order to built a coherent age scale ladder, minimizing the error budget and the sources of uncertainty.

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How accurate are stellar ages based on stellar models?

Cited by 31 publications

References 117 publications

Asteroseismology of red giants: From analysing light curves to estimating ages

Asteroseismology of red giants: From analysing light curves to estimating ages

An M Dwarf Companion to an F-Type Star in a Young Main-Sequence Binary

Clusters: Age Scales for Stellar Physics

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