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The evolution of planetary systems is intimately linked to the evolution oftheir host star. Our understanding of the whole planetary evolution process isbased on the large planet diversity observed so far. To date, only few tens ofplanets have been discovered orbiting stars ascending the Red Giant Branch.Although several theories have been proposed, the question of how planets dieremains open due to the small number statistics. In this work we study thegiant star Kepler-91 (KOI-2133) in order to determine the nature of atransiting companion. This system was detected by the Kepler Space Telescope.However, its planetary confirmation is needed. We confirm the planetary natureof the object transiting the star Kepler-91 by deriving a mass of $M_p=0.88^{+0.17}_{-0.33} ~M_{\rm Jup}$ and a planetary radius of$R_p=1.384^{+0.011}_{-0.054} ~R_{\rm Jup}$. Asteroseismic analysis produces astellar radius of $R_{\star}=6.30\pm 0.16 ~R_{\odot}$ and a mass of$M_{\star}=1.31\pm 0.10 ~ M_{\odot} $. We find that its eccentric orbit($e=0.066^{+0.013}_{-0.017}$) is just $1.32^{+0.07}_{-0.22} ~ R_{\star}$ awayfrom the stellar atmosphere at the pericenter. Kepler-91b could be the previousstage of the planet engulfment, recently detected for BD+48 740. Ourestimations show that Kepler-91b will be swallowed by its host star in lessthan 55 Myr. Among the confirmed planets around giant stars, this is theplanetary-mass body closest to its host star. At pericenter passage, the starsubtends an angle of $48^{\circ}$, covering around 10% of the sky as seen fromthe planet. The planetary atmosphere seems to be inflated probably due to thehigh stellar irradiation.

Kepler-91b: a planet at the end of its life. Planet and giant host star properties via light-curve variations