Two-dimensional models of early-type fast rotating stars: new challenges in stellar physics

Abstract

Two-dimensional models of rapidly rotating stars are already unavoidable for the interpretation of interferometric or asteroseismic data of this kind of stars. When combined with time evolution, they will allow the including of a more accurate physics for the computation of element transport and the determination of surface abundances. In addition, modeling the evolution of rotation will improve gyrochronology. Presently, two-dimensional ESTER models predict the structure and the large-scale flows (differential rotation and meridional circulation) of stars with mass larger than 1.7Msun at any rotation rate. Main sequence evolution can be mimicked by varying the hydrogen content of the convective core. Models have been successfully tested on half a dozen of nearby fast rotating stars observed with optical or infra-red interferometers. They are now the right tool to investigate the oscillation spectrum of early-type fast rotators.

10 pages, to appear in the proceedings of the conference "New advances in stellar physics: from microscopic to macroscopic processes", Roscoff, May 2013

References in corpus (7)

• Imaging the Surface of Altair
• Gravito-inertial and pressure modes detected in the B3 IV CoRoT target HD 43317
• Resolving Vega and the inclination controversy with CHARA/MIRC
• Self-consistent 2D models of fast rotating early-type star
• Imaging and Modeling Rapidly Rotating Stars: Alpha Cephei and Alpha Ophiuchi
• The dynamics of the radiative envelope of rapidly rotating stars. I. A spherical Boussinesq model
• Lithium-7 surface abundance in pre-MS stars. Testing theory against clusters and binary systems

Cited by in corpus (3)

• Tidal disruption events: the role of stellar spin
• Rossby numbers and stiffness values inferred from gravity-mode asteroseismology of rotating F- and B-type dwarfs: consequences for mixing, transport, magnetism, and convective penetration
• Photometric determination of rotation axis inclination, rotation rate, and mass of rapidly rotating intermediate-mass stars