Gliese 880 is a red dwarf star 22.4 light-years away in the northern constellation of Pegasus. No stellar companions to Gliese 880 have been discovered as of 2020.[9]
Search for planets
editIn June 2019, a candidate planet detected by radial velocity in orbit around Gliese 880 was reported in a preprint. This would have a minimum mass about 8.5 times that of Earth and orbit with a period of 39.4 days,[10] which is close to the star's rotation period of 37.5 days.[7] A 2024 study did not detect the exact period of 39.4 days, but detected two radial velocity signals at 37.2 and 40.5 days, which correspond to the stellar rotation and an alias of it. Presumably, the previously claimed planet candidate is an artifact of stellar activity.[11]
References
edit- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g h i Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ Fuhrmeister, B.; et al. (2019), "The CARMENES search for exoplanets around M dwarfs. Period search in H{alpha}, Na I D, and Ca II IRT lines", Astronomy & Astrophysics, 623: A24, arXiv:1901.05173, Bibcode:2019A&A...623A..24F, doi:10.1051/0004-6361/201834483, S2CID 119064800
- ^ Boyajian, Tabetha S.; von Braun, Kaspar; van Belle, Gerard; McAlister, Harold A.; Brummelaar, Theo A. ten; Kane, Stephen R.; Muirhead, Phil; Jones, Jeremy; White, Russel; Schaefer, Gail; Ciardi, David; Henry, Todd; López-Morales, Mercedes; Ridgway, Stephen; Gies, Douglas (2012-10-01). "Stellar Diameters and Temperatures II. Main Sequence K & M Stars". The Astrophysical Journal. 757 (2): 112. arXiv:1208.2431. doi:10.1088/0004-637X/757/2/112. ISSN 0004-637X.
- ^ Abia, C.; et al. (2020), "The CARMENES search for exoplanets around M dwarfs: Rubidium abundances in nearby cool stars", Astronomy & Astrophysics, 642: A227, arXiv:2009.00876, Bibcode:2020A&A...642A.227A, doi:10.1051/0004-6361/202039032, S2CID 221447685
- ^ a b Lindgren, Sara; Heiter, Ulrike (2017). "Metallicity determination of M dwarfs. Expanded parameter range in metallicity and effective temperature". Astronomy and Astrophysics. 604: A97. arXiv:1705.08785. Bibcode:2017A&A...604A..97L. doi:10.1051/0004-6361/201730715. S2CID 119216828.
- ^ a b Suárez Mascareño, A.; et al. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv:1506.08039. Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441.
- ^ "HD 216899". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-11-23.
- ^ Lamman, Claire; et al. (2020), "Robo-AO M-dwarf Multiplicity Survey: Catalog", The Astronomical Journal, 159 (4): 139, arXiv:2001.05988, Bibcode:2020AJ....159..139L, doi:10.3847/1538-3881/ab6ef1, S2CID 210718832
- ^ Barnes, J. R.; et al. (2019-06-11). "Frequency of planets orbiting M dwarfs in the Solar neighbourhood". arXiv:1906.04644 [astro-ph.EP].
- ^ Mignon, L.; Delfosse, X.; et al. (September 2024). "Radial velocity homogeneous analysis of M dwarfs observed with HARPS". Astronomy & Astrophysics. 689: A32. doi:10.1051/0004-6361/202346570.
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