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Stellar spin-orbit angle in planetary systems

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If you have a question about this talk, please contact Jean Teyssandier.

The first exoplanets detected around solar-type stars were mostly hot Jupiters. These observations were puzzling because such planets cannot form so close to their star. It has thus been proposed that these planets get born much further out and then migrate inward by interaction with the protoplanetary disk. A second revolution happened when observations showed that several of the hot Jupiters were on highly inclined orbits with respect to the equatorial plane of their stars. A series of alternative scenarios to the disk migration has then been proposed, most of them involving high eccentricity excitations. In this talk, I will review the different migration scenarios and tilting processes. I will then focus on multiplanet systems for which the high eccentricity migration scenario is excluded. In particular, I will discuss their secular evolution when they are perturbed by an inclined stellar companion as in the case of the 55 Cancri planet system. I will also describe the geometrical structure hidden beneath this interesting problem.

This talk is part of the DAMTP Astro Mondays series.

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