LHS 2090 is a red dwarf star of spectral type M6.5V, located in constellation Cancer at 20.8 light-years from Earth.[10]
The star was identified to be a red dwarf at short distance (6 parsecs from Sun) in 2001.[11] As typical for very cool red dwarfs, its spectrum is dominated by molecular water absorption. Stellar metallicity is similar to that of Sun`s.[8]
Radial velocity measurements did not yield any detection of stellar companion or giant planet on orbit around LHS 2090, as in 2018.[2]
^ abCutri, R. M.; et al. (2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog. Bibcode:2003yCat.2246....0C.
^ abcdeHenry, Todd J.; Jao, Wei-Chun; Winters, Jennifer G.; Dieterich, Sergio B.; Finch, Charlie T.; Ianna, Philip A.; Riedel, Adric R.; Silverstein, Michele L.; Subasavage, John P.; Vrijmoet, Eliot Halley (2018), "The Solar Neighborhood XLIV: RECONS Discoveries within 10 parsecs", The Astronomical Journal, 155 (6): 265, arXiv:1804.07377, Bibcode:2018AJ....155..265H, doi:10.3847/1538-3881/aac262, S2CID 53983430
^Alonso-Floriano, F. J.; Morales, J. C.; Caballero, J. A.; Montes, D.; Klutsch, A.; Mundt, R.; Cortés-Contreras, M.; Ribas, I.; Reiners, Ansgar; Amado, P. J.; Quirrenbach, A.; Jeffers, S. V. (2015). "CARMENES input catalogue of M dwarfs" (PDF). Astronomy & Astrophysics. 577: A128. arXiv:1502.07580. Bibcode:2015A&A...577A.128A. doi:10.1051/0004-6361/201525803. S2CID 53135130.
^Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
^Davison, Cassy L.; White, R. J.; Henry, T. J.; Riedel, A. R.; Jao, W-C.; Bailey Iii, J. I.; Quinn, S. N.; Cantrell, J. R.; Subasavage, J. P.; Winters, J. G. (2015), "A 3D Search for Companions to 12 Nearby M Dwarfs", The Astronomical Journal, 149 (3): 106, arXiv:1501.05012, Bibcode:2015AJ....149..106D, doi:10.1088/0004-6256/149/3/106, S2CID 9719725
^ abcCite error: The named reference Fouque2017 was invoked but never defined (see the help page).
^ abDieterich, Sergio B.; Henry, Todd J.; Jao, Wei-Chun; Winters, Jennifer G.; Hosey, Altonio D.; Riedel, Adric R.; Subasavage, John P. (2013), "The Solar Neighborhood. Xxxii. The Hydrogen Burning Limit", The Astronomical Journal, 147 (5): 94, arXiv:1312.1736, doi:10.1088/0004-6256/147/5/94, S2CID 21036959
^ abRojas-Ayala, Bárbara; Covey, Kevin R.; Muirhead, Philip S.; Lloyd, James P. (2011), "Metallicity and Temperature Indicators in M Dwarfk-Band Spectra: Testing New and Updated Calibrations with Observations of 133 Solar Neighborhood M Dwarfs", The Astrophysical Journal, 748 (2): 93, arXiv:1112.4567, doi:10.1088/0004-637X/748/2/93, S2CID 41902340
^"LHS 2090". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 29 January 2018.
^Cite error: The named reference Henry2006 was invoked but never defined (see the help page).
^Scholz, R.-D.; Meusinger, H.; Jahreiß, H. (2001), "Search for nearby stars among proper motion stars selected by optical-to-infrared photometry", Astronomy & Astrophysics, 374 (2): L12–L15, arXiv:astro-ph/0106222, doi:10.1051/0004-6361:20010811, S2CID 8488435
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