@repepo That's so nice, but you say in the repo that the code is for incompressible fluids so I guess it is meant only for planetary seismic waves and not stellar seismic waves, or is it?

@mekonto the code uses the Boussinesq approximation to filter out acoustic waves (some seismic waves are acoustic, so it cannot model those). The waves it can model are those restored by gravity (g modes), Coriolis (inertial modes), or magnetic (Alfven waves). Or combination of the three regardless of whether it is a fluid core in a planet, or a subsurface ocean (like in some icy moons), or a star.

@repepo I see, I think now I understand. So what you show in the picture is just the core of the Sun, where Boussinesq approx. is fine but the external part of the Sun is not shown because cannot be modelled so no convective layer, right?

@mekonto the picture shows the whole Sun, including the convective zone (white-orange region towards the surface). We use the Boussinesq to get a rough idea of the modes. But a better approx for the actual Sun would be the anelastic approximation (more expensive computationally), which gives qualitatively similar results.

@repepo Cool, thanks for the explanation I'm curious, are you doing solar g-modes research or you did this beautiful plot just for illustration purposes?

@mekonto no prob! yes I'm doing research. Lots of exploration here and there and the plot came out from one of those 🙂