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2007MNRAS.382..356K - Mon. Not. R. Astron. Soc., 382, 356-366 (2007/November-3)
Determination of the axial rotation rate using apsidal motion for early-type eclipsing binaries.
KHALIULLIN K.F. and KHALIULLINA A.I.
Abstract (from CDS):
Our analysis yielded the following results. (i) There is a clear correlation between ω_r/ωsyn_ and t/tsyn: the younger a star, the higher the angular velocity of its axial rotation in units of ωsyn, the angular velocity at pseudo-synchronization. This correlation is more significant and obvious if the synchronization time, tsyn, is computed in terms of the Zahn theory. (ii) This observational fact implies that the synchronization of early-type components in close binary systems continues on the main sequence. The synchronization times for the inner layers of the components (i.e. those that are responsible for apsidal motion) are about 1.6 and 3.1 dex longer than those predicted by the theories of Zahn and Tassoul, respectively. The average initial angular velocities (for the zero-age main sequence) are equal to ω0/ωsyn~ 2.0. The dependence of the parameter E2 on stellar mass probably needs to be refined in the Zahn theory. (iii) Some components of the eclipsing systems of the sample studied show radially differential axial rotation. This is consistent with the Zahn theory, which predicts that the synchronization starts at the surface, where radiative damping of dynamical tides occurs, and develops toward the interior. Therefore, one would expect the inner parts of young double early-type stars to rotate faster than the outer parts.
Abstract Copyright: 2007 The Authors. Journal compilation © 2007 RAS
Journal keyword(s): binaries: eclipsing - stars: interiors - stars: rotation
Simbad objects: 36
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