Journal
ASTROPHYSICAL JOURNAL
Volume 772, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/772/1/21
Keywords
hydrodynamics; stars: interiors; stars: rotation; waves
Categories
Funding
- NASA [NNG06GD44G]
- NSF [AST09-08807]
- UC/LAB
- Templeton Foundation
- NSF ATM Faculty Position in Solar physics [0457631]
- Direct For Mathematical & Physical Scien [0908807] Funding Source: National Science Foundation
- Directorate For Geosciences
- Div Atmospheric & Geospace Sciences [0457631] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [0908807] Funding Source: National Science Foundation
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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.
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