Abstract:

The origin of the magnetic field in cool stars with convective envelopes, such as the Sun, is not understood. Forthcoming observations of solar and stellar oscillations may provide the information that is required to constrain models of the dynamo. Professor Gizon will show how the solar interior can be imaged in three dimensions to infer flow velocities, structural inhomogeneities, and the magnetic field. In the near future, the seismology of solar-type stars of different ages, masses, and rotation periods should reveal crucial relationships between stellar internal properties (rotation, convection) and activity cycles. To give a taste of the possibilities in a Sun-like star observed by CoRot.