Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...199..183v&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 199, no. 1-2, June 1988, p. 183-190.
Astronomy and Astrophysics
Astrophysics
26
Angular Momentum, Binary Stars, G Stars, Late Stars, Main Sequence Stars, Stellar Rotation, Angular Velocity, Star Formation, Stellar Activity, Stellar Evolution, Stellar Mass
Scientific paper
Magnetic activity generated in the convective zone is at the origin of angular momentum loss of late type stars, and is generally accepted as the explanation for the decay of rotation observed in these stars. The angular momentum loss can be expressed as a power law of the angular velocity whose validity is established for equatorial velocities up to 40 km/s. Synchronized late-type binaries losing angular momentum will evolve toward smaller orbits and, hence, toward increasing angular velocities of the components, by virtue of the coupling between spin and orbital momentum. This effect is used to explain the bimodal character of the period distribution of close G type binaries. It is also possible to derive a new power law for the loss of angular momentum of these very rapidly rotating (up to 200 km/s) tidally coupled binary components.
Maceroni Carla
van't Veer Frans
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