Asteroseismic determination of fundamental parameters for exoplanet host stars with deep learning

Guo, Zhao; Jiang, Chen

doi:10.1016/j.ascom.2023.100686

Cited by 2 publications

(1 citation statement)

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“…By constructing stellar evolution models that seek to reproduce a star's observed oscillation frequencies and surface properties (for example, luminosity, effective temperature, and metallicity), asteroseismology can be used to study a broad range of physics, including atomic diffusion, rotation, magnetic fields, and convection (for an overview, see, e.g., Chaplin & Miglio 2013;García & Ballot 2019). These asteroseismic models can be found using a variety of techniques, including Bayesian inference (e.g., Silva Aguirre et al 2015Aguirre Børsen-Koch et al 2022), Markov Chain Monte Carlo (e.g., Bazot et al 2008;Gruberbauer et al 2012Gruberbauer et al , 2013Bellinger & Christensen-Dalsgaard 2019;Rendle et al 2019;Jiang & Gizon 2021), machine learning (e.g., Bellinger et al 2016Bellinger et al , 2019bBellinger et al , 2020bAngelou et al 2020;Hon et al 2020;Guo & Jiang 2023), genetic algorithms (e.g., Metcalfe & Charbonneau 2003;Charpinet et al 2005;Metcalfe et al 2009Metcalfe et al , 2014Metcalfe et al , 2023, and Levenberg-Marquardt algorithms (e.g., Frandsen et al 2002;Teixeira et al 2003;Miglio & Montalbán 2005).…”

Section: Introductionmentioning

confidence: 99%

Asteroseismic Inversions for Internal Sound Speed Profiles of Main-sequence Stars with Radiative Cores

Buchele,

Bellinger,

Hekker

et al. 2024

ApJ

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The theoretical oscillation frequencies of even the best asteroseismic models of solar-like oscillators show significant differences from observed oscillation frequencies. Structure inversions seek to use these frequency differences to infer the underlying differences in stellar structure. While used extensively to study the Sun, structure inversion results for other stars have so far been limited. Applying sound speed inversions to more stars allows us to probe stellar theory over a larger range of conditions, as well as look for overall patterns that may hint at deficits in our current understanding. To that end, we present structure inversion results for 12 main-sequence solar-type stars with masses between 1 and 1.15 M ⊙. Our inversions are able to infer differences in the isothermal sound speed in the innermost 30% by radius of our target stars. In half of our target stars, the structure of our best-fit model fully agrees with the observations. In the remainder, the inversions reveal significant differences between the sound speed profile of the star and that of the model. We find five stars where the sound speed in the core of our stellar models is too low and one star showing the opposite behavior. For the two stars in which our inversions reveal the most significant differences, we examine whether changing the microphysics of our models improves them and find that changes to nuclear reaction rates or core opacities can reduce, but do not fully resolve, the differences.

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