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Fast rotating red giants in the upper part of the red giant branch have surface velocities that cannot be explained by single star evolution.\n  Aims. We check whether tides between a star and a planet followed by planet engulfment can indeed accelerate the surface rotation of red giants for a sufficient long time in order to produce these fast rotating red giants.\n  Methods. Using rotating stellar models, accounting for the redistribution of the angular momentum inside the star by different transport mechanisms, for the exchanges of angular momentum between the planet orbit and the st","authors_text":"Aline A. Vidotto, Eva Villaver, Georges Meynet, Giovanni Privitera, Michele Bianda, Patrick Eggenberger","cross_cats":["astro-ph.SR"],"headline":"","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.EP","submitted_at":"2016-06-26T12:14:59Z","title":"Star-planet interactions: II. 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