HD 141399 is aK-typesubgiant star 121 light-years away in the constellation ofBoötes. Its surface temperature is 5602K. HD 141399 is enriched in heavy elements compared to theSun, with ametallicity Fe/H index of 0.36±0.03.[8] The star has very lowstarspot activity.[6]
In 2014, four planets orbiting HD 141399 were discovered by theradial velocity method.[9] PlanetHD 141399c is possibly located within the habitable zone.[6] The planetary orbits are close to high-ordermean-motion resonance[12] and closely conform to theTitius–Bode law. Two additional planets, one with a period of 462.9 days, are suspected by analogy with the orbits of theSolar System planets.[13] The planetary orbits around HD 141399 are expected to "jump" periodically on a timescale of a few million years between several quasi-stable configurations due to planet-planet interactions.[12] HD 141399 is one of only two known planetary systems consisting of at least four massive gas giants (the other is the system of planets around the young starHR 8799).[14]
^Cannon, A. J.; Pickering, E. C. (1993). "VizieR Online Data Catalog: Henry Draper Catalogue and Extension (Cannon+ 1918-1924; ADC 1989)".Vizier Online Data Catalog.Bibcode:1993yCat.3135....0C.
^abcdefHébrard, G.; Arnold, L.; Forveille, T.; Correia, A. C. M.; Laskar, J.; Bonfils, X.; Boisse, I.; Díaz, R. F.; Hagelberg, J.; Sahlmann, J.; Santos, N. C.; et al. (1 April 2016). "The SOPHIE search for northern extrasolar planets. X. Detection and characterization of giant planets by the dozen".Astronomy and Astrophysics.588: A145.arXiv:1602.04622.Bibcode:2016A&A...588A.145H.doi:10.1051/0004-6361/201527585.ISSN0004-6361.S2CID55138055.
^Boro Saikia, S.; Marvin, C. J.; Jeffers, S. V.; Reiners, A.; Cameron, R.; Marsden, S. C.; Petit, P.; Warnecke, J.; Yadav, A. P. (2018). "Chromospheric activity catalogue of 4454 cool stars. Questioning the active branch of stellar activity cycles".Astronomy and Astrophysics.616.arXiv:1803.11123.Bibcode:2018A&A...616A.108B.doi:10.1051/0004-6361/201629518.
^abcdeSousa, S. G.; Adibekyan, V.; Delgado-Mena, E.; Santos, N. C.; Andreasen, D. T.; Ferreira, A. C. S.; Tsantaki, M.; Barros, S. C. C.; Demangeon, O.; Israelian, G.; Faria, J. P.; Figueira, P.; Mortier, A.; Brandão, I.; Montalto, M.; Rojas-Ayala, B.; Santerne, A. (2018), "SWEET-Cat updated",Astronomy & Astrophysics,620: A58,arXiv:1810.08108,Bibcode:2018A&A...620A..58S,doi:10.1051/0004-6361/201833350,S2CID119374557
^abcVogt, Steven S.; Butler, R. Paul; Rivera, Eugenio J.; Kibrick, Robert; Burt, Jennifer; Hanson, Russell; Meschiari, Stefano; Henry, Gregory W.; Laughlin, Gregory (2014), "A Four-Planet System Orbiting the K0V Star Hd 141399",The Astrophysical Journal,787 (2): 97,arXiv:1404.7462,Bibcode:2014ApJ...787...97V,doi:10.1088/0004-637X/787/2/97,S2CID10477331
^abAgnew, Matthew T.; Maddison, Sarah T.; Horner, Jonathan (2018), "Prospecting for exo-Earths in multiple planet systems with a gas giant",Monthly Notices of the Royal Astronomical Society,481 (4):4680–4697,arXiv:1809.03730,doi:10.1093/mnras/sty2509
^Allen, Christine; Cordero-Tercero, Guadalupe; Lara, Patricia (2020), "The reliability of the Titius–Bode relation and its implications for the search for exoplanets",Publications of the Astronomical Society of Japan,72 (2),arXiv:2003.05121,doi:10.1093/pasj/psz146
