Close to each stellar center the equipotential surfaces are approximately spherical and concentric with the nearer star. Far from the stellar system, the equipotentials are approximately ellipsoidal and elongated parallel to the axis joining the stellar centers. A critical equipotential intersects itself at the center of mass of the system. It is this equipotential which defines the Roche lobes.
Where matter moves relative to the corotating frame it will be acted upon by a coriolis force. This is not derivable from the Roche lobe model as the coriolis force is a non-conservative force (i.e. not representable by a scalar potential).
See also Roche limit
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