A possible companion star was discovered in 1984 based upon its ultraviolet spectrum. The distribution of the far ultraviolet flux matches that of a white dwarf star of class DA.[6] A 2020 study finds it unlikely that there is a white dwarf companion; instead claiming the radial velocity variations are caused by a substellar object HD 80817 b, probably a brown dwarf, and possibly another substellar object. HD 80817 b would have a minimum mass of 27.1MJ and orbit at 3.3 AU with a period of 1047.1 days and an eccentricity of 0.17. Gaia DR2astrometry also suggested a companion with a mass of about 124MJ (with a high margin of error) orbiting at 2.67 AU, consistent with the radial velocity detection. If the latter mass estimate is correct, this object would be a low-mass star, probably a red dwarf.[4] Further observations through 2022 have confirmed that the companion is indeed a brown dwarf, in addition to the detection of a second brown dwarf on a closer orbit.[7] By some definitions, these objects could be considered supermassive planets, similar to those around Nu Ophiuchi.[citation needed]
^ abReimers, D. (July 1984). "Discovery of a white dwarf companion of the "hybrid" K giant HD 81817". Astronomy and Astrophysics. 136: L5–L6. Bibcode:1984A&A...136L...5R.