Deep inside low-mass stars
arXiv:0805.4697 · doi:10.1017/S1743921308022710
Abstract
Low-mass stars exhibit, at all stages of their evolution, the signatures of complex physical processes that require challenging modeling beyond standard stellar theory. In this review, we recall the most striking observational evidences that probe the interaction and interdependence of various transport processes of chemicals and angular momentum in these objects. We then focus on the impact of atomic diffusion, large scale mixing due to rotation, and internal gravity waves on stellar properties on the main sequence and slightly beyond.
Invited Review to be published in the proceedings of the IAU Symposium 252 "The Art of Modelling stars in the 21st Century" - Sanya - China - April 2008
References in corpus (7)
- White dwarf spins from low mass stellar evolution models
- Magnetic confinement of the solar tachocline
- The effect of rotation on the abundances of the chemical elements of the A-type stars in the Praesepe cluster
- Spectrum and amplitudes of internal gravity waves excited by penetrative convection in solar-type stars
- Confinement of the Sun's interior magnetic field: some exact boundary-layer solutions
- Abundances determination of A, Am and F stars in the Pleiades and Coma Berenices clusters
- Angular momentum transport by internal gravity waves. IV - Wave generation by surface convection zone, from the pre-main sequence to the early-AGB in intermediate mass stars