Astronomy
When planets migrate together
Compare slow and fast convergent migration. Watch an imposed 2:1 resonance retain the period ratio as the pair moves through the disk.
The model and its limits
Prescribed exponential migration, eccentricity damping and a heuristic resonance-capture switch. Capture is an illustrative scenario, not a gravitational N-body or gas-dynamics prediction.
Equations used in the module
Equations integrated: a = −μ r/r³ + Σ G m_j d_j/d_j³ − v/(2τ_a) − 2 (v·r) r/(r² τ_e); τ_a = 400 P_in / DiskTorque, τ_e = τ_a/K, K = 2 + 8 Damping resonant angle: φ = (p+1) λ₂ − p λ₁ − ω₁; P₂/P₁ = (a₂/a₁)^(3/2)
