Asteroseismology of 3642 Kepler Red Giants: Correcting the Scaling Relations Based on Detailed Modeling

Li, Tanda; Li, Yaguang; Bi, Shaolan; Bedding, Timothy R.; Davies, G. R.; Du, Minghao

doi:10.3847/1538-4357/ac4fbf

Cited by 24 publications

(22 citation statements)

References 74 publications

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“…While the ν max correction does constitute an improvement, more stars with similar quality data are needed to know whether this is something that should be implemented and whether it has the right dependence on stellar parameters. The empirical calibration by Li et al (2022a) suggests a stronger variation of f ν max with metallicity than Viani et al (2017), but that could be dependent on the source and analysis of the spectroscopic data. From Eqn.…”

Section: Asteroseismic Comparisons For the Oscillating Giantmentioning

confidence: 94%

“…but no empirical tests have been conducted yet. Li et al (2022a) attempted to carry out a calibration of the scaling relations based on direct asteroseismic frequency modelling, suggesting a metallicity dependence in the relation between ν max and the surface gravity, which could relate to the theoretical work of Viani et al (2017). Unfortunately, their attempt to calibrate the scaling relations is model dependent and also changes when adopting another source of spectroscopic information.…”

Section: Introductionmentioning

confidence: 99%

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Establishing the accuracy of asteroseismic mass and radius estimates of giant stars

Brogaard

Arentoft

Slumstrup

et al. 2022

A&A

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Context. Eclipsing binary stars with an oscillating giant component allow accurate stellar parameters to be derived and asteroseismic methods to be tested and calibrated. To this aim, suitable systems need to be firstly identified and secondly measured precisely and accurately. KIC 4054905 is one such system, which has been identified, but with measurements of a relatively low precision and with some confusion regarding its parameters and evolutionary state. Aims. Our aim is to provide a detailed and precise characterisation of the system and to test asteroseismic scaling relations. Methods. Dynamical and asteroseismic parameters of KIC4054905 were determined from Kepler time-series photometry and multiepoch high-resolution spectra from FIES at the Nordic Optical Telescope. Results. KIC 4054905 was found to belong to the thick disk and consist of two lower red giant branch (RGB) components with nearly identical masses of 0.95M and an age of 9.9 ± 0.6 Gyr. The most evolved star with R 8.4R displays solar-like oscillations. These oscillations suggest that the star belongs to the RGB, supported also by the radius, which is significantly smaller than the red clump phase for this mass and metallicity. Masses and radii from corrected asteroseismic scaling relations can be brought into full agreement with the dynamical values if the RGB phase is assumed, but a best scaling method could not be identified. Conclusions. The dynamical masses and radii were measured with a precision better than 1.0%. We firmly establish the evolutionary nature of the system to be that of two early RGB stars with an age close to 10 Gyr, unlike previous findings. The metallicity and Galactic velocity suggest that the system belongs to the thick disk of the Milky Way. We investigate the agreement between dynamical and asteroseismic parameters for KIC 4054905 measured in various ways. This suggests that consistent solutions exist, but the need to analyse more of these systems continues in order to establish the accuracy of asteroseismic methods.

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Section: Asteroseismic Comparisons For the Oscillating Giantmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Establishing the accuracy of asteroseismic mass and radius estimates of giant stars

Brogaard

Arentoft

Slumstrup

et al. 2022

A&A

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“…Similar to Zinn et al (2020), the purpose of reporting such a representation is to provide the user with the choice of using their own atmospheric parameters to estimate masses and radii. Not only do the scaling relations have an explicit temperature dependence, but the correction term f Δν is also often computed with reference to stellar models as a function of mass, temperature, metallicity, and evolutionary phase of the star (Sharma et al 2016;Rodrigues et al 2017;Serenelli et al 2017;Li et al 2022). To obtain cursory estimates of masses and radii in Section 4.2, we adopt the Sharma et al…”

Section: Seismic Measurementsmentioning

confidence: 99%

HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones

Hon¹,

Kuszlewicz²,

Huber³

et al. 2022

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We present HD-TESS, a catalog of 1709 bright (V ∼ 3–10) red giants from the Henry Draper (HD) Catalog with asteroseismic measurements based on photometry from NASA’s Transiting Exoplanet Survey Satellite (TESS). Using light curves spanning at least 6 months across a single TESS observing cycle, we provide measurements of global asteroseismic parameters ( ν max and Δν) and the evolutionary state for each star in the catalog. We adopt literature values of atmospheric stellar parameters to estimate the masses and radii of the giants in our catalog using asteroseismic scaling relations, and observe that HD-TESS giants on average have larger masses compared to Kepler red giants. Additionally, we present the discovery of oscillations in 99 red giants in astrometric binary systems, including those with subdwarf or white dwarf companions. Finally, we benchmark radii from asteroseismic scaling relations against those measured using long-baseline interferometry for 18 red giants and find that correction factors to the scaling relations improve the agreement between asteroseismic and interferometric radii to approximately 3%.

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“…Our sample (see Fig. 1) consists of stars with measured individual frequencies: the Sun (Broomhall et al 2009), the SONG subgiant µ Herculis (Grundahl et al 2017), Kepler main-sequence dwarfs (Lund et al 2017), Kepler subgiants (Li et al 2020a) and Kepler red-giant-branch (RGB) stars with ∆ν > 2 µHz (Li et al 2022).…”

Section: Observational Samplementioning

confidence: 99%

A prescription for the asteroseismic surface correction

Li¹,

Bedding²,

Stello³

et al. 2022

Preprint

Self Cite

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In asteroseismology, the surface effect is a disparity between the observed and the modelled oscillation frequencies. It originates from improper modelling of the surface layers in stars with solar-like oscillations. Correcting the surface effect usually requires using functions with free parameters, which are conventionally fitted to the observed frequencies. On the basis that the correction should vary smoothly across the H-R diagram, we parameterize it as a simple function of three stellar surface properties: surface gravity, effective temperature, and metallicity. We determine this function by fitting stars ranging from main-sequence dwarfs to red-giant-branch stars. The absolute amount of the surface correction increases with surface gravity, but the ratio between it and ν max decreases. Applying the prescription has an advantage of eliminating unrealistic surface correction, which improves parameter estimations with stellar modelling. Using two open clusters, we found that adopting the prescription can help reduce the scatter of the modelderived ages for each star in the same cluster. For an application, we provide a new revision for the ∆ν scaling relation, using our prescription to account for the surface effect in models. The values of the correction factor, f ∆ν , are up to 2% smaller than those determined without the surface effect considered, suggesting decreases of up to 4% in asteroseismic scaling radii and up to 8% in asteroseismic scaling masses. This revision brings the asteroseismic properties into agreement with those determined from eclipsing binaries. Finally, the new correction factor and the stellar models with the corrected frequencies are made publicly available.

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Asteroseismology of 3642 Kepler Red Giants: Correcting the Scaling Relations Based on Detailed Modeling

Cited by 24 publications

References 74 publications

Establishing the accuracy of asteroseismic mass and radius estimates of giant stars

Establishing the accuracy of asteroseismic mass and radius estimates of giant stars

HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones

A prescription for the asteroseismic surface correction

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