Models of stars rotating near the critical limit

Details Models of stars rotating near the critical limit Models of stars rotating near the critical limit

2009-10-20

arxiv.org/abs/0910.3853v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

4 pages, 3 figures, conference proceedings "Interferometric view of hot stars", Rev. Mexi. de Astron. y Astrofis

Scientific paper

When the surface angular velocity is above about 70% of the critical angular velocity, many interesting features appear which may be tested by interferometric observations, like significant deformation of stars, variation of the effective temperature with the latitude. Also polar winds become important and equatorial disks may appear. Near the critical limit, convection is also favored in the outer layers. In the present paper, we emphasize the need for a proper estimate of the critical velocity since this is the ratio of the actual velocity of the star to that critical velocity which determines the amplitude of the above effects. We recall the existence of two critical velocities. The first one, also called the classical critical velocity is the one to consider when the star has an Eddington factor inferior to 0.639, while the second one is the one to be considered when the Eddington factor is above 0.639. The features of the star at these two critical limits may be very different.

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