Kepler-411 is a binary star system. Its primary star Kepler-411A is aK-type main-sequence star, orbited by thered dwarf star Kepler-411B on a wide orbit, discovered in 2012.[4]
The primary star's surface temperature is4,773 K. Kepler-411A is similar to theSun in its concentration of heavy elements, with ametallicity Fe/H index of 0.11±0.1,[5] but is much younger at an age of 212±31 million years.[7]
Kepler-411A exhibits significantstarspot activity, with starspots covering 1.7+0.3 −0.2% of the stellar surface.[9] Darker starspots are concentrated around the equator of the star. Kepler-411A exhibits differential rotation, but with smaller amount of differential shear compared to theSun.[6]
The companion Kepler-411B is533 au away from Kepler-411A.[8] It is a red dwarf and aflare star.[10]
In 2013, one planet, namedKepler-411b, was discovered,[11] followed by planetKepler-411c in 2016. Third planet in system detected by transit method,d, along withe detected byradial velocity method, were discovered in 2019.[12][7]
^abcZiegler, Carl; Law, Nicholas M.; Baranec, Christoph; Riddle, Reed; Duev, Dmitry A.; Howard, Ward; Jensen-Clem, Rebecca; Kulkarni, S. R.; Morton, Tim; Salama, Maïssa (2017), "Robo-AO Kepler survey. IV. The effect of nearby stars on 3857 planetary candidate systems",The Astronomical Journal,155 (4): 161,arXiv:1712.04454,doi:10.3847/1538-3881/aab042,S2CID119088873
^abFurlan, E.; Ciardi, D. R.; Cochran, W. D.; Everett, M. E.; Latham, D. W.; Marcy, G. W.; Buchhave, L. A.; Endl, M.; Isaacson, H.; Petigura, E. A.; Gautier, T. N.; Huber, D.; Bieryla, A.; Borucki, W. J.; Brugamyer, E.; Caldwell, C.; Cochran, A.; Howard, A. W.; Howell, S. B.; Johnson, M. C.; MacQueen, P. J.; Quinn, S. N.; Robertson, P.; Mathur, S.; Batalha, N. M. (2018), "The Kepler Follow-Up Observation Program. II. Stellar Parameters from Medium- and High-Resolution Spectroscopy",The Astrophysical Journal,861 (2): 149,arXiv:1805.12089,Bibcode:2018ApJ...861..149F,doi:10.3847/1538-4357/aaca34,S2CID119243987
^abcLillo-Box, J.; Lopez, T. A.; Santerne, A.; Nielsen, L. D.; Barros, S. C. C.; Deleuil, M.; Acuña, L.; Mousis, O.; Sousa, S. G.; Adibekyan, V.; Armstrong, D. J.; Barrado, D.; Bayliss, D.; Brown, D. J. A.; Demangeon, O. D. S.; Dumusque, X.; Figueira, P.; Hojjatpanah, S.; Osborn, H. P.; Santos, N. C.; Udry, S. (2020), "Masses for the seven planets in K2-32 and K2-233. Four diverse planets in resonant chain and the first young rocky worlds",Astronomy & Astrophysics,A48: 640,arXiv:2006.01102,Bibcode:2020A&A...640A..48L,doi:10.1051/0004-6361/202037896,S2CID219176756
^Wang, Ji; Xie, Ji-Wei; Barclay, Thomas; Fischer, Debra A. (2013), "Influence of Stellar Multiplicity On Planet Formation. I. Evidence of Suppressed Planet Formation Due to Stellar Companions Within 20 AU and Validation of Four Planets From the Kepler Multiple Planet Candidates",The Astrophysical Journal,783 (1): 4,arXiv:1309.7097,Bibcode:2014ApJ...783....4W,doi:10.1088/0004-637X/783/1/4,S2CID119214390
