Institut de recherche sur les lois fondamentales de l'Univers

I would like to introduce some results of our MHD simulations for "perturbation-driven'" winds. Convection and turbulence are ubiquitous in various astrophysical objects. Turbulent motion excites various modes of waves and they frequently excite flows. For example, the Sun and solar-type stars posses a surface convective layer, which excites MHD waves to accelerate solar and stellar winds. Turbulence in accretion disks plays a role in not only radial transport of angular momentum but also vertical outflows. In this talk, I plan to focus on the following two topics:

(i) Saturation of winds from very active young solar-type stars.

(ii) Protoplanetary disk winds and applications to the evolution of protoplanetary disks and the planet formation.