lundi 5 novembre 2018, par Vincent Prat (AIM, CEA)
Mardi 6 novembre 2018 à 14h00 , Lieu : Salle de rĂ©union du bâtiment 14
Internal gravity waves provide us with a unique way to probe the stellar interior of intermediate-mass and massive stars. Those waves are also able to transport angular momentum. However, the propagation, the frequencies of waves and the transport they induce may be strongly affected by rotation and the presence of a magnetic field. For slow rotators, rotation can be taken into account using perturbative methods. For rapid rotators, which is the case of many early-type pulsators such as gamma Doradus, delta Scuti, SPB and Be stars, such methods fail, and the eigenvalue problem is fully 2D and computationally expensive. The traditional approximation of rotation, which neglects the horizontal component of the rotation vector, allows for efficient computation of modes. Another approach is to consider only small-wavelength waves and model them as propagating rays. Using these two complementary methods, I will discuss the impact of an axisymmetric magnetic field on gravito-inertial waves and the implications for the detection of deep magnetic fields.
