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MRI Channel-Mode Disk Instability (2D)

2D companion model of the magnetorotational instability: the exact linear Balbus-Hawley dispersion relation and its velocity/field polarization, solved directly (no 3D scene) and rendered as a radial-vertical cross-section and a top-down differential-rotation annulus.

Space & Astronomy2DAdvanced60 FPS📱 Mobile-adapted⇄ 3D version

A purely 2D companion to the 3D shearing-box scene: instead of rendering an oblique 3D box, this model solves the exact linear magnetorotational instability (MRI) system directly — four coupled equations for radial velocity, azimuthal velocity and the two perturbed magnetic field components — and draws the result as a radial-vertical cross-section next to a top-down view of the differentially rotating annulus. Tune orbital radius, magnetic field strength and perturbation wavenumber to move along the exact growth-rate curve, watch the field lines kink and the tracer colors flip as azimuthal velocity changes sign, and read the live Maxwell stress that shows outward angular-momentum transport falling directly out of the eigenmode's own polarization.

⚙ Under the hood

A purely 2D companion model that solves the exact linear magnetorotational instability (MRI) system directly — radial and azimuthal velocity plus both perturbed field components — and renders it as a radial-vertical cross-section next to a top-down differentially-rotating annulus, instead of a 3D scene.

black holeaccretion diskmagnetohydrodynamicsMRIastrophysicsplasma instability2D model

2D · HTML5 Canvas 2D · 60 FPS target · runs fully client-side, no install