The K2 M67 Study: Precise Mass for a Turnoff Star in the Old Open Cluster M67

Sandquist, Eric L.; Latham, David W.; Leiner, Emily; Vanderburg, Andrew; Stello, Dennis; Orosz, Jerome A.; Bedin, L. R.; Libralato, Mattia; Malavolta, L.; Nardiello, D.

doi:10.3847/1538-3881/abca8d

Cited by 15 publications

(8 citation statements)

References 107 publications

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“…about 8σ lower). We confirm that we also get the same result with the new version of parsec and leave this problem to a more exhaustive investigation using new parsec models with varying initial metallicity and He content (see also Sandquist et al 2021).…”

supporting

confidence: 80%

“…Recently, it has been shown that M67 harbours an interesting spectroscopic binary system located near the turnoff region, WOCS 11028, that challenges theoretical models (see Sandquist et al 2021, for a thorough discussion). Briefly, the mass of the primary component is estimated to be M WOCSa = 1.222 ± 0.006 M , while current predictions using different stellar evolution codes (including parsec V1.2S) give values that are lower by δ m = 0.05 M (i.e.…”

mentioning

confidence: 99%

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PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

Nguyen

Costa

Girardi

et al. 2022

A&A

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We present a new comprehensive collection of stellar evolutionary tracks and isochrones for rotating low-and intermediate-mass stars assembled with the updated version of parsec V2.0. This version includes our recent calibration of the extra mixing from overshooting and rotation, as well as several improvements regarding the nuclear reaction network, treatment of convective zones, mass loss, and other physical input parameters. The initial mass of the stellar models covers the range 0.09 M to 14 M for six sets of initial metallicity, from Z=0.004 to Z=0.017. Rotation is considered for stars above ∼ 1 M with a smooth transition between non-rotating and extremely fast-rotating models, based on the initial mass. For stars more massive than ∼ 1.3 M , the full rotation range, from low to critical, is considered. We adopt the solar-scaled chemical mixtures with Z = 0.01524. All the evolutionary phases from the pre-main-sequence to the first few thermal pulses on the asymptotic giant branch or central C exhaustion are considered. The corresponding theoretical isochrones are further derived with trilegal code and are converted into several photometric systems, taking different inclination angles into account. Besides magnitudes, they also offer many other stellar observables in line with the data being provided by current large surveys. The new collection is fully integrated in a user-friendly web-interface for the benefit of easily performing stellar population studies.

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supporting

confidence: 80%

mentioning

confidence: 99%

PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

Nguyen

Costa

Girardi

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…about 8σ lower. We confirm that we get the same result also with the new version of parsec and leave this problem to a more exhaustive investigation using new parsec models at varying initial metallicity and He content (see also Sandquist et al 2021).…”

supporting

confidence: 80%

PARSEC V2.0: Stellar tracks and isochrones of low and intermediate mass stars with rotation

Nguyen¹,

Costa²,

L.³

et al. 2022

Preprint

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We present a new comprehensive collection of stellar evolutionary tracks and isochrones for rotating low-and intermediate-mass stars assembled with the updated version of parsec V2.0. This version includes our recent calibration of the extra mixing from overshooting and rotation, as well as several improvements in nuclear reaction network, treatment of convective zones, mass loss and other physical input parameters. The initial mass of the stellar models covers the range from 0.09 M to 14 M , for six sets of initial metallicity, from Z=0.004 to Z=0.017. Rotation is considered for stars above ∼ 1 M with a smooth transition between non-rotating and extremely fast-rotating models, based on the initial mass. For stars more massive than ∼ 1.3 M the full rotation range, from low to the critical one, is considered. We adopt the solar-scaled chemical mixtures with Z = 0.01524. All the evolutionary phases from the pre-main-sequence to the first few thermal-pulses on the asymptotic-giant-branch or central C exhaustion, are considered. The corresponding theoretical isochrones are further derived with trilegal code and are converted in several photometric systems, taking into account different inclination angles. Besides magnitudes, they also offer many other stellar observables in line with the data that are being provided by current large surveys. The new collection is fully integrated in a user friendly WEB interface for the benefit of easily performing stellar population studies.

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“…3. The ages of the clusters used to calibrate the gyrochronology themselves have significant standard errors and systematics; full consideration of these is beyond the scope of this work but should be included when considering rotation-based ages in an absolute sense (Sandquist et al 2021).…”

Section: Gyrochrone Errormentioning

confidence: 99%

The TIME Table: Rotation and Ages of Cool Exoplanet Host Stars

Gaidos¹,

Claytor²,

Dungee³

et al. 2023

Preprint

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Age is a stellar parameter that is both fundamental and difficult to determine. Among middleaged M dwarfs, the most prolific hosts of close-in and detectable exoplanets, gyrochronology is the most promising method to assign ages, but requires calibration by rotation-temperature sequences (gyrochrones) in clusters of known ages. We curated a catalog of 249 late Kand M-type (𝑇 eff =3200-4200K) exoplanet host stars with established rotation periods, and applied empirical, temperature-dependent rotation-age relations based on relevant published gyrochrones, including one derived from observations of the 4 Gyr-old open cluster M67. We estimated ages for 227 of these stars, and upper limits for 8 others, excluding 14 which are too rapidly rotating or are otherwise outside the valid parameter range of our gyrochronology. We estimated uncertainties based on observed scatter in rotation periods in young clusters, error in the gyrochrones, and uncertainties in temperature and non-solar metallicity. For those stars with measured metallicities, we provide but do not incorporate a correction for the effects of deviation from solar-metallicity. The age distribution of our sample declines to near zero at 10 Gyr, the age of the Galactic disk, with the handful of outliers explainable by large uncertainties. Continued addition or extension of cluster rotation sequences to more thoroughly calibrate the gyrochronology in time and temperature space, more precise and robust measurement of rotation periods, and more accurate stellar parameter measurements will enable continued improvements in the age estimates of these important exoplanet host stars.

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The K2 M67 Study: Precise Mass for a Turnoff Star in the Old Open Cluster M67

Cited by 15 publications

References 107 publications

PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

PARSEC V2.0: Stellar tracks and isochrones of low and intermediate mass stars with rotation

The TIME Table: Rotation and Ages of Cool Exoplanet Host Stars

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