The red dwarf companion is classified as anultra-cool dwarf, with a spectral type around M9.[5] With a visual magnitude of 15 and separated from the primary by only threearcseconds, it can only be seen with a powerful telescope.[3] It is estimated to be around 10 billion years old, although the properties of such low-mass stars are very similar across a wide range of ages. It is calculated have only 8% of themass of the Sun, a tenth ofits radius, and with a temperature of about2,645 K it produces less than a thousandth ofits luminosity.[5]
In 1989, a companion object,HD 114762 Ab, was found orbitingHD 114762 A by Latham,et al., usingDoppler spectroscopy,[11] but its existence was not confirmed until 1991 by Cochran,et al.[12] Its orbital distance and revolution is similar to that ofMercury, though it has twice theeccentricity.[12] It has aminimum mass of10.69MJ, and thus was originally thought to be a massiveexoplanet; however, in 2019, itsinclination was determined byGaiaastrometry, giving it a true mass of107MJ. This makes it ared dwarf star, or a massivebrown dwarf.[4] A 2020 study provided further confirmation of this, and revised the mass upwards to147MJ,[7] and in 2022 this mass was revised upwards still further, to 0.293 M☉, based onGaia DR3 data and a similar upwards revision to the mass of the primary star.[6]
