INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT

By T. Rogers, D. Lin, Jim N. McElwaine, H. Lau. 2013

150 citations recorded by the source corpus.

We present numerical simulations of internal gravity waves (IGW) in a star with a convective core and extended radiative envelope. We report on amplitudes, spectra, dissipation, and consequent angular momentum transport by such waves. We find that these waves are generated efficiently and transport angular momentum on short timescales over large distances. We show that, as in Earth's atmosphere, IGW drive equatorial flows which change magnitude and direction on short timescales. These results have profound consequences for the observational inferences of massive stars, as well as their long term angular momentum evolution. We suggest IGW angular momentum transport may explain many observational mysteries, such as: the misalignment of hot Jupiters around hot stars, the Be class of stars, Ni enrichment anomalies in massive stars, and the non-synchronous orbits of interacting binaries.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fbaf884c6fdddd19566596236b47cabc91206cb2

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In Astronomy and Astrophysics

1. J. Fuller
2. A. Piro
3. B. Paxton
4. Matteo Cantiello
5. R. Townsend
6. L. Bildsten
7. Adam S. Jermyn
8. C. Mankovich

Citations in the corpus

• Classical Be stars (2013, background): “Rogers et al. (2013) have modeled such modes as internal gravity waves, transporting angular momentum upwards.”
• Angular momentum transport by heat-driven g-modes in slowly pulsating B stars (2017, background): “Rogers et al. (2013) and Rogers (2015) use two-dimensional anelastic hydrodynamical simulations to investigate the impact of internal gravity waves (IGWs), excited stochastically at the convective core boundary, on the internal rotation profile of massive stars.”
• Pre-supernova outbursts via wave heating in massive stars – I. Red supergiants (2017, background): “…is not well understood, as Goldreich & Kumar (1990) and Lecoanet & Quataert (2013) argue for excitation at ωwave ∼ ωcon due to bulk Reynolds stresses, while Rogers et al. (2013) argue for excitation via plume incursion that adds a substantial high-frequency (ωwave > ωcon) tail to the spectrum.”
• ANGULAR MOMENTUM TRANSPORT WITHIN EVOLVED LOW-MASS STARS (2014, background): “…needs to be done to understand the details of the excitation and propagation of gravity waves (See e.g. Lecoanet & Quataert 2013; Shiode et al. 2013; Rogers et al. 2013) Another possibility is that some large scale magnetic field is present in and above the stellar core at the end of the main…”
• Slowing the spins of stellar cores (2019, background): “For rotation rates of about 100 d, equation (47) predicts tAM ∼ 106 yr, which may be longer than the time-scale for shear to develop due to other effects such as internal gravity waves (Rogers et al. 2013; Fuller et al. 2014; Townsend, Goldstein & Zweibel 2018).”