BRUCALASSI, ANNAANNABRUCALASSIPasquini, L.L.PasquiniSaglia, R.R.SagliaRuiz, M.T.M.T.RuizBonifacio, PPBonifacioLeão, I.I.LeãoCanto Martins, B.L.B.L.Canto MartinsDe Medeiros, J.R.J.R.De MedeirosBEDIN, LuigiLuigiBEDINBIAZZO, KatiaKatiaBIAZZOMelo, C.C.MeloLovis, C.C.LovisRANDICH, Maria SofiaMaria SofiaRANDICH2020-06-112020-06-1120160004-6361http://hdl.handle.net/20.500.12386/26003Since 2008 we used high-precision radial velocity (RV) measurements obtained with different telescopes to detect signatures of massive planets around main-sequence and evolved stars of the open cluster (OC) M67. We aimed to perform a long-term study on giant planet formation in open clusters and determine how this formation depends on stellar mass and chemical composition. A new hot Jupiter (HJ) around the main-sequence star YBP401 is reported in this work. An update of the RV measurements for the two HJ host-stars YBP1194 and YBP1514 is also discussed. Our sample of 66 main-sequence and turnoff stars includes 3 HJs, which indicates a high rate of HJs in this cluster (5.6% for single stars and 4.5% for the full sample). This rate is much higher than what has been discovered in the field, either with RV surveys or by transits. High metallicity is not a cause for the excess of HJs in M67, nor can the excess be attributed to high stellar masses. When combining this rate with the non-zero eccentricity of the orbits, our results are qualitatively consistent with a HJ formation scenario dominated by strong encounters with other stars or binary companions and subsequent planet-planet scattering, as predicted by N-body simulations.STAMPAenArticle10.1051/0004-6361/2015275612-s2.0-84978128647000384722600044https://www.aanda.org/articles/aa/abs/2016/08/aa27561-15/aa27561-15.html2016A&A...590A..78BFIS/05 - ASTRONOMIA E ASTROFISICA