Coupling 1D stellar evolution with 3D-hydrodynamical simulations on-the-fly II: Stellar Evolution and Asteroseismic Applications

Abstract

Models of stellar structure and evolution are an indispensable tool in astrophysics, yet they are known to incorrectly reproduce the outer convective layers of stars. In the first paper of this series, we presented a novel procedure to include the mean structure of 3D hydrodynamical simulations on-the-fly in stellar models, and found it to significantly improve the outer stratification and oscillation frequencies of a standard solar model. In the present work, we extend the analysis of the method; specifically how the transition point between envelope and interior affects the models. We confirm the versatility of our method by successfully repeating the entire procedure for a different grid of 3D hydro-simulations. Furthermore, the applicability of the procedure was investigated across the HR diagram and an accuracy comparable to the solar case was found. Moreover, we explored the implications on stellar evolution and find that the red-giant branch is shifted about 40 K to higher effective temperatures. Finally, we present for the first time an asteroseismic analysis based on stellar models fully utilising the stratification of 3D simulations on-the-fly. These new models significantly reduce the asteroseismic surface term for the two selected stars in the Kepler field. We extend the analysis to red giants and characterise the shape of the surface effect in this regime. Lastly, we stress that the interpolation required by our method would benefit from new 3D simulations, resulting in a finer sampling of the grid.

14 pages, 13 figures, 4 tables. Accepted for publication in MNRAS

References in corpus (13)

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• On the surface physics affecting solar oscillation frequencies
• Stellar models with mixing length and T(tau) relations calibrated on 3D convection simulations
• Stellar models with the ML2 theory of convection
• The asteroseismic surface effect from a grid of 3D convection simulations. I. Frequency shifts from convective expansion of stellar atmospheres
• Theoretical oscillation frequencies for solar-type dwarfs from stellar models with $⟨3\mathrm{D}⟩$-atmospheres
• Mending the structural surface effect of 1D stellar structure models with non-solar metallicities based on interpolated 3D envelopes

Cited by in corpus (21)

• Probing the interior physics of stars through asteroseismology
• Solar structure and evolution
• Numerical Simulations of Convective 3-Dimensional Red Supergiant Envelopes
• The BAyesian STellar Algorithm (BASTA): a fitting tool for stellar studies, asteroseismology, exoplanets, and Galactic archaeology
• A prescription for the asteroseismic surface correction
• Calibrating Core Overshooting Parameters With Two-dimensional Hydrodynamical Simulations
• Investigating surface correction relations for RGB stars
• The Status and Future of Direct Nuclear Reaction Measurements for Stellar Burning
• On the impact of the structural surface effect on global stellar properties and asteroseismic analyses
• Differential Modelling Systematics across the HR Diagram from Asteroseismic Surface Corrections
• An asteroseismic age estimate of the open cluster NGC 6866 using Kepler and Gaia
• The effect of the adiabatic assumption on asteroseismic scaling relations for luminous red giants
• Stellar evolution models with entropy-calibrated mixing-length parameter: application to red giants
• Properties of the ionisation glitch: I. Modelling the ionisation region
• Does the ${\nu }_{\max }$ scaling relation depend on metallicity? Insights from 3D convection simulations
• Estimating the nonstructural component of the helioseismic surface term using hydrodynamic simulations
• Surface effects and turbulent pressure. Assessing the Gas-${\Gamma }_1$ and Reduced-${\Gamma }_1$ empirical models
• Glitch analysis and asteroseismic modelling of subgiant $\mu$ Herculis: confirming and interpreting the ${\Gamma }_1$ peak as the helium glitch
• Third order correlations and skewness in convection. I. A new approach suitable for three-equation non-local models
• Advanced asteroseismic modelling: breaking the degeneracy between stellar mass and initial helium abundance
• PLATO Hare-and-Hounds exercise: Asteroseismic model fitting of main-sequence solar-like pulsators