The rotation of very low-mass stars and brown dwarfs
arXiv:0708.1479 · doi:10.1017/S174392130700960X
Abstract
The evolution of angular momentum is a key to our understanding of star formation and stellar evolution. The rotational evolution of solar-mass stars is mostly controlled by magnetic interaction with the circumstellar disc and angular momentum loss through stellar winds. Major differences in the internal structure of very low-mass stars and brown dwarfs -- they are believed to be fully convective throughout their lives, and thus should not operate a solar-type dynamo -- may lead to major differences in the rotation and activity of these objects. Here, we report on observational studies to understand the rotational evolution of the very low-mass stars and brown dwarfs.
arXiv comment8 pages, 5 figures, Proceedings for IAU Symposium No. 243, 2007, 'Star-disk interaction in young stars'
References in corpus (11)
- On the rotational evolution of solar- and late-type stars, its magnetic origins, and the possibility of stellar gyrochronology
- Accretion-powered Stellar Winds as a Solution to the Stellar Angular Momentum Problem
- The Angular Momentum Evolution of Very Low Mass Stars
- The Monitor project: Rotation of low-mass stars in the open cluster NGC 2516
- Stellar Models with Microscopic Diffusion and Rotational Mixing II: Application to Open Clusters
- The Mass Dependence of Stellar Rotation in the Orion Nebula Cluster
- Rotational velocities of low-mass stars in the Pleiades and Hyades
- The Monitor project: Rotation of low-mass stars in the open cluster M34
- A Search for Photometric Rotation Periods in Low-Mass Stars and Brown Dwarfs in the Pleiades
- Periodic photometric variability of the brown dwarf Kelu-1
- Angular Momentum Evolution of Young Stars: Toward a Synthesis of Observations, Theory, and Modeling