Angular Momentum Transport via Internal Gravity Waves in Evolving Stars
arXiv:1409.6835 · doi:10.1088/0004-637X/796/1/17
Abstract
Recent asteroseismic advances have allowed for direct measurements of the internal rotation rates of many sub-giant and red giant stars. Unlike the nearly rigidly rotating Sun, these evolved stars contain radiative cores that spin faster than their overlying convective envelopes, but slower than they would in the absence of internal angular momentum transport. We investigate the role of internal gravity waves in angular momentum transport in evolving low mass stars. In agreement with previous results, we find that convectively excited gravity waves can prevent the development of strong differential rotation in the radiative cores of Sun-like stars. As stars evolve into sub-giants, however, low frequency gravity waves become strongly attenuated and cannot propagate below the hydrogen burning shell, allowing the spin of the core to decouple from the convective envelope. This decoupling occurs at the base of the sub-giant branch when stars have surface temperatures of roughly 5500 K. However, gravity waves can still spin down the upper radiative region, implying that the observed differential rotation is likely confined to the deep core near the hydrogen burning shell. The torque on the upper radiative region may also prevent the core from accreting high-angular momentum material and slow the rate of core spin-up. The observed spin-down of cores on the red giant branch cannot be totally attributed to gravity waves, but the waves may enhance shear within the radiative region and thus increase the efficacy of viscous/magnetic torques.
13 pages, 5 figures, accepted to ApJ
References in corpus (11)
- Modules for Experiments in Stellar Astrophysics (MESA)
- Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
- Asteroseismic measurement of surface-to-core rotation in a main sequence A star, KIC 11145123
- Stochastic excitation of nonradial modes II. Are solar asymptotic gravity modes detectable?
- On the tidal origin of hot Jupiter stellar obliquity trends
- Theoretical seismology in 3D : nonlinear simulations of internal gravity waves in solar-like stars
- A Revised Prescription for the Tayler-Spruit Dynamo: Magnetic Angular Momentum Transport in Stars
- Impact of rotation on stochastic excitation of gravity and gravito-inertial waves in stars
- Nonlinear Dynamics of Gravity Wave Driven Flows in the Solar Radiative Interior
- Angular momentum transport by internal gravity waves III - Wave excitation by core convection and the Coriolis effect
- What Prevents Internal Gravity Waves From Disturbing the Solar Uniform Rotation?
Cited by in corpus (3)
- Asteroseismic measurement of slow, nearly-uniform surface-to-core rotation in the main sequence F star KIC 9244992
- Angular momentum redistribution by mixed modes in evolved low-mass stars. II. Spin-down of the core of red giants induced by mixed modes
- Angular momentum redistribution by mixed modes in evolved low-mass stars. I. Theoretical formalism