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VW~LMi is the tightest known quadruple system with 2+2 hierarchy. It consistsof a W UMa-type eclipsing binary (P12 = 0.47755 days) and another detachednon-eclipsing binary (P34 = 7.93 days) orbiting around a common center of massis about P1234 = 355 days. We present new observations of the system extendingthe time baseline to study long-term perturbations in the system and to improveorbital elements. The multi-dataset modeling of the system (4 radial-velocitycurves for the components and the timing data) clearly showed an apsidal motionin the non-eclipsing binary at a rate of 4.6 degrees/yr, but no otherperturbations. This is consistent with the nearly co-planarity of the outer,355-day orbit, and the 7.93-day orbit of the non-eclipsing binary. ExtensiveN-body simulations enabled us to constrain the mutual inclination of thenon-eclipsing binary and the outer orbits to j34-1234 < 10 degrees.

Secular changes in the orbits of the quadruple system VW LMi