TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting an Extremely Eccentric Exoplanet

Jiang, Chen; Wu, Tao; Feinstein, Adina D.; Stassun, Keivan G.; Bedding, Timothy R.; Veras, Dimitri; Corsaro, E.; Buzasi, Derek L.; Stello, Dennis; Li, Yaguang; Mathur, S.; García, R. A.; Breton, Sylvain; Lundkvist, M.; Mikołajczyk, P.; Gehan, Charlotte; Campante, Tiago L.; Bossini, D.; Kane, Stephen R.; Ong, J. M. Joel; Yıldız, Mutlu; Kayhan, Cenk; Orhan, Zeynep Çelik; Örtel, Sibel; Zhang, Xinyi; Cunha, M. S.; Moura, Bruno Lustosa de; Jiang, Yu; Huber, Daniel; Ou, Jian-Wen; Wittenmyer, Robert A.; Gizon, Laurent; Chaplin, W. J.

doi:10.3847/1538-4357/acb8ac

Cited by 2 publications

(1 citation statement)

References 140 publications

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“…raising the yield of oscillating giants to a few hundreds of thousands (Hon et al 2021), an order of magnitude increase over the yield from Kepler and K2. This has enabled the systematic search for transiting planets around seismic giants (Campante et al 2016;Huber et al 2019;Pereira et al 2019;Grunblatt et al 2022Grunblatt et al , 2023Saunders et al 2022), as well as revisiting previously known (mostly from radial-velocity surveys) evolved hosts using asteroseismology (Campante et al 2019;Ball et al 2020;Jiang et al 2020Jiang et al , 2023Malla et al 2020;Nielsen et al 2020;Kane et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters

Campante

Ong

et al. 2023

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Asteroseismology is playing an increasingly important role in the characterization of red giant host stars and their planetary systems. Here, we conduct detailed asteroseismic modeling of the evolved red giant branch (RGB) hosts KOI-3886 and ι Draconis, making use of end-of-mission Kepler (KOI-3886) and multisector TESS (ι Draconis) time-series photometry. We also model the benchmark star KIC 8410637, a member of an eclipsing binary, thus providing a direct test to the seismic determination. We test the impact of adopting different sets of observed modes as seismic constraints. Inclusion of ℓ = 1 and 2 modes improves the precision of the stellar parameters, albeit marginally, compared to adopting radial modes alone, with 1.9%–3.0% (radius), 5%–9% (mass), and 19%–25% (age) reached when using all p-dominated modes as constraints. Given the very small spacing of adjacent dipole mixed modes in evolved RGB stars, the sparse set of observed g-dominated modes is not able to provide extra constraints, further leading to highly multimodal posteriors. Access to multiyear time-series photometry does not improve matters, with detailed modeling of evolved RGB stars based on (lower-resolution) TESS data sets attaining a precision commensurate with that based on end-of-mission Kepler data. Furthermore, we test the impact of varying the atmospheric boundary condition in our stellar models. We find the mass and radius estimates to be insensitive to the description of the near-surface layers, at the expense of substantially changing both the near-surface structure of the best-fitting models and the values of associated parameters like the initial helium abundance, Y i . Attempts to measure Y i from seismic modeling of red giants may thus be systematically dependent on the choice of atmospheric physics.

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Section: Introductionmentioning

confidence: 99%

Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters

Campante

Ong

et al. 2023

Self Cite

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Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay between Mixing Length, Metallicity, and ν max

Li 李,

Bedding,

Huber

et al. 2024

ApJ

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Asteroseismic modeling is a powerful way to derive stellar properties. However, the derived quantities are limited by built-in assumptions used in stellar models. This work presents a detailed characterization of stellar model uncertainties in asteroseismic red giants, focusing on the mixing-length parameter α MLT, the initial helium fraction Y init, the solar abundance scale, and the overshoot parameters. First, we estimate error floors due to model uncertainties to be ≈0.4% in mass, ≈0.2% in radius, and ≈17% in age, primarily due to the uncertain state of α MLT and Y init. The systematic uncertainties in age exceed typical statistical uncertainties, suggesting the importance of their evaluation in asteroseismic applications. Second, we demonstrate that the uncertainties from α MLT can be entirely mitigated by direct radius measurements or partially through ν max . Utilizing radii from Kepler eclipsing binaries, we determined the α MLT values and calibrated the α MLT–[M/H] relation. The correlation observed between the two variables is positive, consistent with previous studies using 1D stellar models, but in contrast with outcomes from 3D simulations. Third, we explore the implications of using asteroseismic modeling to test the ν max scaling relation. We found that a perceived dependency of ν max on [M/H] from individual frequency modeling can be largely removed by incorporating the calibrated α MLT–[M/H] relation. Variations in Y init can also affect ν max predictions. These findings suggest that ν max conveys information not fully captured by individual frequencies, and that it should be carefully considered as an important observable for asteroseismic modeling.

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TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting an Extremely Eccentric Exoplanet

Cited by 2 publications

References 140 publications

Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters

Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters

Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay between Mixing Length, Metallicity, and ν max

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