Student colloquium - Peter Fløche Juelsgaard
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Modeling stars has long been a key tool for understanding stellar evolution, and while we have a relatively good understanding of the equations of state that govern the behaviour in the stellar interior and radiative energy transport, the theory of convective energy transport still poses significant challenges. In this kollokvium, I examine the progress in the treatment of convection, starting with one-dimensional mixing-length theory. I also take a look at the use of semi-empirical atmosphere models, before moving on the look at 3D MHD models. For this purpose I focus on the STAGGER code, which solves the hydrodynamical equations for conservation of mass and couples these to the radiation field through heating and cooling of elements.
Following the presentation of the STAGGER code, I examine solar models I have computed in STAGGER, and compare them with similar models computed using the popular MESA code.