Laplace for 4:3:2

To constrain my 4.75-day station between Europa and Ganymede, let's look at Laplace for this. Pierre-Simon himself was working with 4:2:1. This is p+1:p and q+1:q where p=q=1. My station is the 3 in 4:3:2; my p=2 and q=3 (I tried 3 and 2, trust me, it doesn't work). Papaloizou's mean-motion equation is (p+q+1)n₂ - qn₁ - (p+1)n₃ = 0 . . . for the case where all the resonant angles are stationary or undergo small amplitude librations. I know that Jupiter+Io tides are going to mess this all up. So I'll flip Papaloizou such that, when this equation is satisfied, the librations are at minimum.

6n₂ - 3n₁ - 3n₃ = 0, then. So, the mean-motion of my sat will be (101.37472576024707 + 50.317609222086183) / 2 = 75.846167491166625 °/day; 4.746 days or, if you like, four days 17:54:14. 5.76 minutes off my 4.75 estimate - not bad, if I do say so myself.

Also kinda redundant. I suppose the next step would be longitudes. Like: when Europa is at λ₁ and Ganymede at λ₃, I need λ₂. For 4:2:1 λ₁ - 3λ₂ + 2λ₃ = 180° but what's that for 4:3:2?