Stars lose a significant amount of angular momentum between birth and death, implying that
efficient processes transporting it from the core to the surface are active. Space …

We are entering a golden era for stellar physics driven by satellite and telescope
observations of unprecedented quality and scope. New insights on stellar evolution and …

During most of their life, stars fuse hydrogen into helium in their cores. The mixing of
chemical elements in the radiative envelope of stars with a convective core is able to …

We present the first set of a new generation of models of massive stars with a solar
composition extending between 13 and 120 M☉, computed with and without the effects of …

Context. B-type stars are known to rotate at various velocities, including very fast rotators
near the critical velocity as the Be stars. Aims. In this paper, we provide stellar models …

Context. Rotational splittings are currently measured for several main sequence stars and a
large number of red giants with the space mission Kepler. This will provide stringent …

This paper presents the Geneva stellar evolution code with special emphasis on the
modeling of solar-type stars. The basic input physics used in the Geneva code as well as the …

Thus far, KIC 7760680 is the richest slowly pulsating B star, exhibiting 36 consecutive dipole
(ℓ= 1) gravity (g-) modes. The monotonically decreasing period spacing of the series, in …

Abstract The critical Richardson number, Ric, is used in studies of stably stratified turbulence
as a measure of flow laminarization. The accepted range of Ric is between 0.2 and 1. A …

This article first reviews the basic physics of rotating stars and their evolution. The changes
of the mechanical and thermal equilibrium of rotating stars are examined. An important …