In the restricted three-body problem, where two massive bodies orbit each other in a circle, the Lagrange points are literally points - anywhere but the five ex

In the restricted three-body problem, where two massive bodies orbit each other in a circle, the Lagrange points are literally points - anywhere but the five exact 3d coordinates and there is a net acceleration away from your location. Not sure if that's what you mean, but if you're happy to assume that the massive bodies (e.g. Earth and Sun) are spherical, then you can exactly replace them with point masses, without approximation, so there's no multiplicity in Lagrange points coming from that. Of course, orbits are not circular, and there are external forces too - other planets' gravity, (tiny) orbital drag, solar wind pressure etc. so in practice it's all a bit different anyway.