Context. The solar convection zone is the region between the radiative zone and the photosphere, where energy transport is carried by convection. Modelling of this region is difficult because of the many temporal- and spacial-scales having to be taken into account, as well as the high turbulence creating numerical instability.
Aims. This thesis utilizes the anelastic approximation and aims to create a code for simulation of the dynamic behaviour of the solar convection zone. This work is meant as a building block for future investigations and makes it possible to easily add additional physics.
Results. We present the development, testing, and initial results of a 2D hydrodynamical code using the anelastic approximation. The simulations show good alignment with predicted mixing length theory velocities, and flux. They also show the dynamics of large-scale structures, but found that the chosen boundary conditions was not sufficient for small-scale structure in the upper convection zone. The findings in this thesis provides a promising foundation for future research and underscores the potential of using high-resolution simulations with the anelastic approximation to explore the dynamics of the solar convection zone
Supervisors:
Professor Boris V. Gudiksen, Institute of Theoretical Astrophysics, UiO
Postdoctoral Fellow Sondre Vik Furuseth, Institute of Theoretical Astrophysics, UiO
Intern. assessor: Professor Per Barth Lilje, Institute of Theoretical Astrophysics, UiO
Extern. assessor: Post-doc Daniel Elias Nóbrega Siverio, Instituto de Astrofísica de Canarias (IAC)