Back

Rayleigh-Taylor instability

What you are seeing: a dense fluid (red) sitting above a lighter fluid (cyan) in a downward gravitational field. Any perturbation grows as exp(σt)\exp(\sigma t) with σ=Akg\sigma = \sqrt{A k g} (Atwood number AA, wavenumber kk, gravity gg). Dense spikes fall, light bubbles rise

Figure 1. RT instability of a dense-over-light interface; linear exp(sigma t) growth saturates into spike-bubble structure. Method: closed-form linear streamfunction + saturating nonlinear advection.
Atwood A0.50
k (modes)3
gravity g1.0
animation speed2

WHAT TO TRY

  • Vary each control and watch the rail readouts respond.
  • Compare the diagnostic plot against the live scene.