This is the Lane Emden equation, which states how density is related to radius in a newtonian self-gravitating spherically symmetric polytropic fluid. It involves 4 main numbers: n (the polytropic index), θ (a number related to density), ϕ (dimensionless mass), and ξ (dimensionless radius). This equation (two equations here) is integrated from the center (with x^y replaced with re(x^y) if needed) and then displayed as brightness, with the edge having brightness too. Polytropic fluids are a special type of fluid used to model things like stars, where n can be thought of as “emptiness”: n = 0 is like a rocky planet, n = 1 is like a neutron star, n = 3 is like main-sequence stars and white drawfs, and n = 5 is like a self-consistent solar system. In the limit of n -> +infinity, the fluid is isothermal and like a globular cluster, with all mass at the center. The dimensionless radius ξ is measured where ξ = 1 is the boundary of the fluid, where ρ = 0.
turbomode / turbowarp not necessary somehow, even with n = -50 (which if you look in the code, is the slowest)
