Abstract: The stagger code simulates the 3D radiation hydrodynamics and magnetic field at the solar surface. It addresses sophisticated processes including ionization effects, compressibility, and solves the equations of radiation transfer and induction. I will present solar model atmospheres computed with the OPAL EoS and the most recent solar composition (Asplund et al. 2009).
Those models account for the effects of the magnetic field. They offer a means of interpreting the observations of the space borne missions dedicated to the solar surface dynamics (SDO, Picard).
In particular I will discuss the impact of magnetism on the limb darkening profile. But the surface convection 3D models also offer more realistic boundary conditions to the solar structure than the phenomenologies of convection. I will present the work we have been undertaking to account for 3D atmospheresin 1D solar structure secular modelling.
Bio: Not Available
Time: 4:00pm – 5:30pm
Location: Physics and Astrophysics Conference Room 102/103
Light refreshments available 4:00pm; Presentation begiins 4:15pm
Open to All