Damping rates and frequency corrections of Kepler LEGACY stars

Houdek, G.; Lund, Mikkel N.; Trampedach, Regner; Christensen‐Dalsgaard, J.; Handberg, R.; Appourchaux, T.

doi:10.1093/mnras/stz1211

Cited by 20 publications

(25 citation statements)

References 78 publications

(149 reference statements)

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“…Asteroseismology of a variety of stars permits one to do better. Indeed, the shift between the measured oscillation frequencies and those predicted by 3D hydrodynamical simulations of convection relevant for the outer envelopes of low-mass stars is informative when evaluating such simulations (Zhou, Asplund, and Collet, 2019), assessing nonadiabatic stability analyses (Houdek et al, 2019), and finding out how to "patch" 3D atmosphere models to 1D models of stellar interiors.…”

Section: Improving the Physics Of Cool-star Surface Convectionmentioning

confidence: 99%

Probing the interior physics of stars through asteroseismology

2021

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Section: Improving the Physics Of Cool-star Surface Convectionmentioning

confidence: 99%

Probing the interior physics of stars through asteroseismology

2021

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“…This requirement builds on the assumption that the combined surface effect is negative as in the case of the present-day Sun and other main-sequence stars (e.g. Brown 1984;Christensen-Dalsgaard et al 1988;Houdek et al 2017;Houdek et al 2019).…”

Section: Choosing Surface Correction Relation Parametersmentioning

confidence: 99%

“…the pressure stemming from the bulk motion of a convective fluid, is often not correctly accounted for, further contributing to the aforementioned frequency shift (cf. Houdek et al 2017;Houdek et al 2019;Schou & Birch 2020, for a detailed discussion of this issue).…”

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confidence: 99%

Investigating surface correction relations for RGB stars

Jørgensen

Montalbán

Miglio

et al. 2020

Monthly Notices of the Royal Astronomical Society

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State-of-the-art stellar structure and evolution codes fail to adequately describe turbulent convection. For stars with convective envelopes such as red giants, this leads to an incomplete depiction of the surface layers. As a result, the predicted stellar oscillation frequencies are haunted by systematic errors, the so-called surface effect. Different empirically and theoretically motivated correction relations have been proposed to deal with this issue. In this paper, we compare the performance of these surface correction relations for red giant branch stars. For this purpose, we apply the different surface correction relations in asteroseismic analyses of eclipsing binaries and open clusters. In accordance with previous studies of main-sequence stars, we find that the use of different surface correction relations biases the derived global stellar properties, including stellar age, mass, and distance estimates. We, furthermore, demonstrate that the different relations lead to the same systematic errors for two different open clusters. Our results overall discourage from the use of surface correction relations that rely on reference stars to calibrate free parameters. Due to the demonstrated systematic biasing of the results, the use of appropriate surface correction relations is imperative to any asteroseismic analysis of red giants. Accurate mass, age, and distance estimates for red giants are fundamental when addressing questions that deal with the chemo-dynamical evolution of the Milky Way galaxy. In this way, our results also have implications for fields such as galactic archaeology that draw on findings from stellar physics.

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“…To this end, Rosenthal et al (1999) used 3D hydrodynamical simulations, which allowed them to account for the mean turbulent pressure (as well as convective backwarming; see Trampedach et al 2017) in the equilibrium structure. Their work was followed by Piau et al (2014), Magic & Weiss (2016), Houdek et al (2017), , Schou & Birch (2020) for the Sun and Sonoi et al (2015Sonoi et al ( , 2017, Ball et al (2016), Trampedach et al (2017), Jørgensen et al (2017Jørgensen et al ( , 2018Jørgensen et al ( , 2021, Manchon et al (2018), , Houdek et al (2019), Mosumgaard et al (2020) for solar-like stars. A drawback of this approach is the need to compute adiabatic eigenfrequencies using empirical models to describe the Lagrangian perturbation of turbulent pressure.…”

Section: Introductionmentioning

confidence: 99%

Surface effects and turbulent pressure

Belkacem

Kupka

Philidet

et al. 2021

A&A

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The application of the full potential of stellar seismology is made difficult by the improper modelling of the upper-most layers of solar-like stars and their influence on the modelled frequencies. Our knowledge of these so-called ‘surface effects’ has improved thanks to the use of 3D hydrodynamical simulations, however, the calculation of eigenfrequencies relies on empirical models for the description of the Lagrangian perturbation of turbulent pressure, namely: the reduced-Γ1 model (RGM) and the gas-Γ1 model (GGM). Starting from the fully compressible turbulence equations, we derived both the GGM and RGM models by using a closure to model the flux of turbulent kinetic energy. We find that both models originate from two terms: the source of turbulent pressure due to compression produced by the oscillations and the divergence of the flux of turbulent pressure. We also demonstrate that they are both compatible with the adiabatic approximation and, additionally, that they imply a number of questionable assumptions, mainly with respect to mode physics. Among other hypotheses, it is necessary to neglect the Lagrangian perturbation of the dissipation of turbulent kinetic energy into heat and the Lagrangian perturbation of buoyancy work.

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Damping rates and frequency corrections of Kepler LEGACY stars

Cited by 20 publications

References 78 publications

Probing the interior physics of stars through asteroseismology

Probing the interior physics of stars through asteroseismology

Investigating surface correction relations for RGB stars

Surface effects and turbulent pressure

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