Mixing by internal gravity waves in stars: assessing numerical simulations against theory

Morton, J.; Guillet, T.; Baraffe, I.; Morison, A.; Le Saux, A.; Vlaykov, D. G.; Goffrey, T.; Pratt, J.

doi:10.1093/mnras/staf010

Mixing by internal gravity waves in stars: assessing numerical simulations against theory

Journal Article · Mon Jan 06 00:00:00 EST 2025 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/staf010· OSTI ID:2500931

; ; Baraffe, I.; ; ; ; Goffrey, T.; Pratt, J.

ABSTRACT

Here we present a study of radial chemical mixing in non-rotating massive main-sequence stars driven by internal gravity waves (IGWs), based on multidimensional hydrodynamical simulations with the fully compressible code MUSIC. We examine two proposed mechanisms of material mixing in stars by IGWs that are commonly quoted, relating to thermal diffusion and sub-wavelength shearing. Thermal diffusion provides a non-restorative effect to the waves, leaving material displaced from its previous equilibrium, while shearing arising within the waves drives weak localized flows, mixing the fluid there. Using IGW spectra from the simulations, we evaluate theoretical predictions of mixing rates due to these mechanisms. We show, for $$20\, \mathrm{M}_\odot$$ main-sequence stars, that neither of these mechanisms are likely to create mixing sufficient to correct inaccuracies in current stellar evolution models. Furthermore, we compare these predictions to results obtained from Lagrangian tracer particles, following a method recently used for global simulations of stellar interiors to measure mixing by IGWs in their radiative zones. We demonstrate that tracer particle methods face significant numerical challenges in measuring the small diffusion coefficients predicted by the aforementioned theories, for which they are prone to yielding artificially enhanced coefficients. Diffusion coefficients based on such methods are currently used with stellar evolution codes for asteroseismic studies, but should be viewed with caution. Finally, in a case where tracer particles do not suffer from numerical artefacts, we suggest that a diffusion model is not suitable for time-scales typically considered by 2D numerical simulations.

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Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Organization:: European Research Council (ERC); Science and Technology Facilities Council (STFC); USDOE; USDOE National Nuclear Security Administration (NNSA)

Grant/Contract Number:: AC52-07NA27344

OSTI ID:: 2500931

Alternate ID(s):: OSTI ID: 2511360

Report Number(s):: LLNL--JRNL-867493

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 1 Vol. 537; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United Kingdom

Language:: English

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