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The recent characterization of transiting close-in planets has revealed anintriguing population of sub-Neptunes with highly tilted and even polar orbitsrelative to their host star's equator. Any viable theory for the origin ofthese close-in, polar planets must explain (1) the observed stellarobliquities, (2) the substantial eccentricities, and (3) the existence ofJovian companions with large mutual inclinations. In this work, we propose atheoretical model that satisfies these requirements without invoking tidaldissipation or large primordial inclinations. Instead, tilting is facilitatedby the protoplanetary disk dispersal during the late stage of planet formation,initiating a process of resonance sweeping and parametric instability. Thismechanism consists of two steps. First, a nodal secular resonance excites theinclination to large values; then, once the inclination reaches a criticalvalue, a linear eccentric instability is triggered, which detunes the resonanceand ends inclination growth. The critical inclination is pushed to high valuesby general relativistic precession, making polar orbits an inherentlypost-Newtonian outcome. Our model predicts that polar, close-in sub-Neptunescoexist with cold Jupiters in low stellar obliquity orbits.

A disk-driven resonance as the origin of high inclinations of close-in planets