Other
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985msngr..41...12n&link_type=abstract
The Messenger, vol. 41, p. 12-13
Other
F Stars:Stellar Rotation, Stellar Rotation:F Stars
Scientific paper
The rotation is a general property of celestial objects, which is probably generated by the vorticity of the interstellar matter. Obviously, stars forming from turbulent vortices conserve some of the initial angular momentum, depending on the early formation history. It is weil known that there is a well-determined trend of the rotational velocity of main sequence and giant stars with the spectral type. This is shown by the continuous and dashed curves of Figure 1, which are from the paper of Bernacca and Perinotto (A A, 33, 443, 1974). Earlytype stars have high rotational velocities, while late-type stars are slow rotators. There is a sharp drop in the velocities from F0 to F5, particularly for main sequence stars: stars later than F5 have all very little angular momentum. This has been attributed to the presence of planets around late-type stars, which would contain most of the angular momentum of the system, as it happens in the case of the solar system. The angular momentum is probably transferred during the T Tauri pre-main-sequence phase. Another possibility suggested for the rotation velocity drop is the loss of angular momentum caused by stellar winds, which should occur for stars having convective layers close to the surface, i. e. late-type stars.
Noci Giancarlo
Ortolani Sergio
Pomilia A.
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