We report on the first star discovered to host a planet detected by radial velocity (RV) observations obtained within the CARMENES survey for exoplanets around M dwarfs. HD 147379 ( V ?=?8.9 mag, M ?=?0.58?±?0.08? M _(⊙)), a bright M0.0 V star at a distance of 10.7 pc, is found to undergo periodic RV variations with a semi-amplitude of K ?=?5.1 ± 0.4 m s~(?1)and a period of P ?=?86.54 ± 0.06 d. The RV signal is found in our CARMENES data, which were taken between 2016 and 2017, and is supported by HIRES/Keck observations that were obtained since 2000. The RV variations are interpreted as resulting from a planet of minimum mass m _(P)?sin? i ?=?25?±?2? M _(⊕), 1.5 times the mass of Neptune, with an orbital semi-major axis a ?=?0.32 au and low eccentricity ( e < 0.13). HD 147379 b is orbiting inside the temperate zone around the star, where water could exist in liquid form. The RV time-series and various spectroscopic indicators show additional hints of variations at an approximate period of 21.1 d (and its first harmonic), which we attribute to the rotation period of the star.
展开▼
机译：我们报告了第一颗恒星，该恒星是由CARMENES调查中获得的M矮行星系外行星的径向速度（RV）观测发现的。 HD 147379（V？=？8.9 mag，M？=？0.58？±？0.08？M _（⊙）），距离为10.7 pc的M0.0 V明亮恒星，周期性地发生RV变化的半振幅为Kα＝ 5.1±0.4ms〜（α1），周期为Pα＝ 86.54±0.06d。 RV信号可在我们的CARMENES数据中找到，该数据在2016年至2017年之间获取，并得到自2000年以来获得的HIRES / Keck观测结果的支持。RV的变化被解释为是由质量最小的行星m _（P） ？罪？我？=？25？±？2？ M _（⊕），是海王星质量的1.5倍，轨道半长轴a = 0.32 au，偏心率低（e <0.13）。 HD 147379b在恒星周围的温带区内公转，在那儿水可能以液态存在。 RV时间序列和各种光谱指示符还显示了大约21.1 d（及其一次谐波）周期的附加变化提示，我们将其归因于恒星的自转周期。
展开▼
