Astronomy
The expanding remains of a star
Expand a shock through interstellar gas. Increase the explosion energy or ambient density and compare the shock radius and speed.
The model and its limits
Adiabatic Sedov–Taylor similarity solution for a uniform medium, γ=5/3. Filaments and false colours are illustrative; early ejecta and radiative cooling are outside the model.
Equations used in the module
Equations R = 1.15167(E/ρ)^(1/5)t^(2/5); v = 2R/(5t); T_s = 3μm_pv²/(16k)
