Internal Gravity Waves in Massive Stars II: Frequency Analysis Across Stellar Mass

Abstract

Stars with masses above 1.6 solar masses generally possess convective cores and radiative envelopes, which allows the propagation of outward-travelling internal gravity waves. We have studied the generation and propagation of IGWs in such stars using two-dimensional, fully nonlinear hydrodynamical simulations with realistic stellar reference states from the one-dimensional stellar evolution code, Modules for Stellar Astrophysics. Compared to previous similar works, this study utilises radius-dependent thermal diffusivity profiles for 5 different stellar masses at the middle of main sequence: 3 - 13 solar masses. From the simulations, we find that the surface perturbations are larger for higher masses, but no noticeable trends are observed for the frequency slopes with different stellar masses. The slopes are also similar to the results from previous works. We compare our simulation results with stellar photometric data from a recent survey and find that for frequency intervals above 8 microHz, there is a good agreement between the temperature frequency slopes from the simulations and the surface brightness variations of these observed stars, indicating that the brightness variations are caused by core-generated IGWs.

arXiv comment17 pages, 30 figures, 5 tables

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• Multidimensional Simulations of Core Convection
• Effect of Rotation on Wave Mixing in Intermediate Mass Stars
• The ESO UVES/FEROS Large Programs of TESS OB pulsators. II. On the physical origin of macroturbulence
• Asteroseismology of the young open cluster NGC 2516 II. Constraining cluster age using gravity-mode pulsators
• Calibrating chemical mixing induced by internal gravity waves based on hydrodynamical simulations; The chemical evolution of OB-type stars
• Effects of stratification on overshooting and waves atop the convective core of $5M_{\odot }$ main-sequence stars
• Variability of Galactic blue supergiants observed with TESS
• Fast optical variability in Supergiant X-ray binaries