• Media type: E-Article
  • Title: The CARMENES search for exoplanets around M dwarfs : HD147379 b: A nearby Neptune in the temperate zone of an early-M dwarf : HD147379 b: A nearby Neptune in the temperate zone of an early-M dwarf
  • Contributor: Reiners, A.; Ribas, I.; Zechmeister, M.; Caballero, J. A.; Trifonov, T.; Dreizler, S.; Morales, J. C.; Tal-Or, L.; Lafarga, M.; Quirrenbach, A.; Amado, P. J.; Kaminski, A.; Jeffers, S. V.; Aceituno, J.; Béjar, V. J. S.; Guàrdia, J.; Guenther, E. W.; Hagen, H.-J.; Montes, D.; Passegger, V. M.; Seifert, W.; Schweitzer, A.; Cortés-Contreras, M.; Abril, M.; [...]
  • imprint: EDP Sciences, 2018
  • Published in: Astronomy & Astrophysics
  • Language: Not determined
  • DOI: 10.1051/0004-6361/201732165
  • ISSN: 1432-0746; 0004-6361
  • Keywords: Space and Planetary Science ; Astronomy and Astrophysics
  • Origination:
  • Footnote:
  • Description: <jats:p>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 (<jats:italic>V</jats:italic> = 8.9 mag, <jats:italic>M</jats:italic> = 0.58 ± 0.08 <jats:italic>M</jats:italic><jats:sub>⊙</jats:sub>), 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 <jats:italic>K</jats:italic> = 5.1 ± 0.4 m s<jats:sup>−1</jats:sup> and a period of <jats:italic>P</jats:italic> = 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 <jats:italic>m</jats:italic><jats:sub>P</jats:sub> sin <jats:italic>i</jats:italic> = 25 ± 2 <jats:italic>M</jats:italic><jats:sub>⊕</jats:sub>, 1.5 times the mass of Neptune, with an orbital semi-major axis <jats:italic>a</jats:italic> = 0.32 au and low eccentricity (<jats:italic>e</jats:italic> &lt; 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.</jats:p>
  • Access State: Open Access