Astronomy
A star's bow wave
Balance an outward stellar wind against an incoming interstellar flow. Change density or speed and watch the stand-off distance respond.
The model and its limits
Steady, axisymmetric, thin momentum-conserving Wilkin shell in a uniform medium. Particles trace prescribed wind and ambient flow; no hydrodynamic instabilities or radiative cooling are solved. Star size is enlarged.
Equations used in the module
Equations R₀ = √(dM/dt v_w/(4πρv_*²)); R(θ)/R₀ = csc θ √[3(1−θ cot θ)].
