Kepler-410 is a binary star system. Its primary star, also known as Kepler-410A, is a F-typesubgiant star, orbited by theorange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.[9]
The primary star's surface temperature is 6325±75K.[11] HD 175289 is similar to theSun in its concentration of heavy elements, with ametallicity Fe/H index of 0.01±0.10,[11] but is much younger at an age of 1.81±0.27 billion years.[10]
In 2013, one planet, named Kepler-410Ab, was discovered using thetransit method.[14] It is not known if the planet is orbiting the primary or secondary star.[14] If orbiting the secondary, the planetary radius must be doubled.[15] Immediately, a second non-transiting planet was suspected due totransit-timing variations, and a 2019 study also found evidence for such a planet, though it has not yet been confirmed or given any designation.[7]
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^Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog".The Astronomical Journal.122 (6): 3466.Bibcode:2001AJ....122.3466M.doi:10.1086/323920.
^abcdeBellinger, E. P.; Hekker, S.; Angelou, G. C.; Stokholm, A.; Basu, S. (2020). "Stellar ages, masses, and radii from asteroseismic modeling are robust to systematic errors in spectroscopy".Astronomy & Astrophysics.622: A130.arXiv:1812.06979.doi:10.1051/0004-6361/201834461.S2CID119293351.
^abVan Eylen, V.; Lund, M. N.; Aguirre, V. Silva; Arentoft, T.; Kjeldsen, H.; Albrecht, S.; Chaplin, W. J.; Isaacson, H.; Pedersen, M. G.; Jessen-Hansen, J.; Tingley, B.; Christensen-Dalsgaard, J.; Aerts, C.; Campante, T. L.; Bryson, S. T. (2014). "What Asteroseismology can do for Exoplanets: Kepler-410A b is a Small Neptune around a Bright Star, in an Eccentric Orbit Consistent with Low Obliquity".The Astrophysical Journal.782 (1): 14.arXiv:1312.4938.Bibcode:2014ApJ...782...14V.doi:10.1088/0004-637X/782/1/14.S2CID15893540.
