Towards a self-consistent model of the convective core boundary in upper main sequence stars

Abstract:

There is strong observational evidence that the convective cores of intermediate-mass and massive main sequence stars are substantially larger than those predicted by standard stellar-evolution models. However, it is unclear what physical processes cause this phenomenon or how to predict the extent and stratification of stellar convective boundary layers. Convective penetration is a thermal-timescale process that is likely to be particularly relevant during the slow evolution on the main sequence. We use our low-Mach-number SEVEN-LEAGUE HYDRO code to study this process in 2.5D and 3D geometries. Starting with a chemically homogeneous model of a 15  M⊙ zero-age main sequence star, we construct a series of simulations with the luminosity increased and opacity decreased by the same factor, ranging from 10^3 to 10^6. After reaching thermal equilibrium, all of our models show a clear penetration layer; its thickness becomes statistically constant in time and it is shown to converge upon grid refinement. The penetration layer becomes nearly adiabatic with a steep transition to a radiative stratification in simulations at the lower end of our luminosity range. This structure corresponds to the adiabatic ‘step overshoot’ model often employed in stellar-evolution calculations. The simulations with the highest and lowest luminosity differ by less than a factor of two in the penetration distance. The high computational cost of 3D simulations makes our current 3D data set rather sparse. Depending on how we extrapolate the 3D data to the actual luminosity of the initial stellar model, we obtain penetration distances ranging from 0.09 to 0.44 pressure scale heights, which is broadly compatible with observations.

SEEK ID: https://publications.h-its.org/publications/1823

DOI: 10.1051/0004-6361/202347407

Research Groups: Physics of Stellar Objects

Publication type: Journal

Journal: Astronomy & Astrophysics

Citation: A&A 683:A97

Date Published: 1st Mar 2024

Registered Mode: by DOI

Authors: R. Andrassy, G. Leidi, J. Higl, P. V. F. Edelmann, F. R. N. Schneider, F. K. Röpke

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Citation
Andrassy, R., Leidi, G., Higl, J., Edelmann, P. V. F., Schneider, F. R. N., & Röpke, F. K. (2024). Towards a self-consistent model of the convective core boundary in upper main sequence stars. In Astronomy & Astrophysics (Vol. 683, p. A97). EDP Sciences. https://doi.org/10.1051/0004-6361/202347407
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Created: 14th Mar 2024 at 14:49

Last updated: 14th Mar 2024 at 14:53

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