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A new element is proposed to play a role in the evolution of extrasolar  planetary systems: the tidal (or elliptical) instability. It comes from a  parametric resonance and takes place in any rotating uid whose streamlines are  (even slightly) elliptically deformed. Based on theoretical, experimental and  numerical works, we estimate the growth rate of the instability for hot-jupiter  systems, when the rotation period of the star is known. We present the physical  process, its application to stars, and preliminary results obtained on a few  dozen systems, summarized in the form of a stability diagram. Most of the  systems are trapped in the so-called "forbidden zone", where the instability  cannot grow. In some systems, the tidal instability is able to grow, at short  timescales compared to the system evolution. Implications are discussed in the  framework of misaligned transiting systems, as the rotational axis of the star  would be unstable in systems where this elliptical instability grows

Tidal instability in exoplanetary systems evolution