Two-dimensional simulations of internal gravity waves in a $\mathrm{5M_⊙}$ zero-age-main-sequence model

Le Saux, Arthur; Baraffe, I.; Guillet, Thomas; Vlaykov, Dimitar Georgiev; Morison, A.; Pratt, J.; Constantino, T.; Goffrey, T.

doi:10.1093/mnras/stad1067

Two-dimensional simulations of internal gravity waves in a $$\mathrm{5M_⊙}$$ zero-age-main-sequence model

Journal Article · Fri Apr 14 00:00:00 EDT 2023 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stad1067· OSTI ID:1975608

^[1]; Baraffe, I. ^[1]; ^[2]; ^[2]; Morison, A. ^[2]; Pratt, J. ^[3]; Constantino, T. ^[2]; Goffrey, T. ^[4]

Univ. of Exeter (United Kingdom); Univ. of Lyon (France); Centre National de la Recherche Scientifique (CNRS) (France)
Univ. of Exeter (United Kingdom)
Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)
Univ. of Warwick, Coventry (United Kingdom)

Main-sequence intermediate-mass stars present a radiative envelope that supports internal gravity waves (IGWs). Excited at the boundary with the convective core, IGWs propagate towards the stellar surface and are suspected to impact physical processes such as rotation and chemical mixing. Using the fully compressible time-implicit code MUSIC, we study IGWs in two-dimensional simulations of a zero-age-main-sequence 5 solar mass star model up to 91 percent of the stellar radius with different luminosity and radiative diffusivity enhancements. Our results show that low-frequency waves excited by core convection are strongly impacted by radiative effects as they propagate. This impact depends on the radial profile of radiative diffusivity which increases by almost 5 orders of magnitude between the centre of the star and the top of the simulation domain. In the upper layers of the simulation domain, we observe an increase of the temperature. Our study suggests that this is due to heat added in these layers by IGWs damped by radiative diffusion. We show that non-linear effects linked to large amplitude IGWs may be relevant just above the convective core. Both these effects are intensified by the artificial enhancement of the luminosity and radiative diffusivity, with enhancement factors up to 10⁴ times the realistic values. Our results also highlight that direct comparison between numerical simulations with enhanced luminosity and observations must be made with caution. Finally, our work suggests that thermal effects linked to the damping of IGWs could have a non-negligible impact on stellar structure.

View Accepted Manuscript (DOE)

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

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

Grant/Contract Number:: AC52-07NA27344

OSTI ID:: 1975608

Report Number(s):: LLNL-JRNL-842731; 1065215

Journal Information:: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 2 Vol. 522; ISSN 0035-8711

Publisher:: Oxford University PressCopyright Statement

Country of Publication:: United States

Language:: English

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