A double star in the constellation Corvus
! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.0
       Equinox J2000.0
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Spectral type
! style="text-align:left" | B−V 
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HD 111031 (50 G. Corvi) is a double star in the southern constellation of Corvus. With an apparent visual magnitude of 6.87, it is considered too faint to be readily visible to the naked eye. The distance to this star is 102 light years, but it is drifting closer to the Sun with a radial velocity of −20 km/s. It has an absolute magnitude of 4.42. The star has a relatively large proper motion, traversing the celestial sphere at an angular rate of .
This object is a solar analog with a stellar classification of G5 V; a G-type main-sequence star like the Sun that is generating energy through core hydrogen fusion. It is around five billion years old and is chromospherically inactive, with a projected rotational velocity of 1.7 km/s. The star has 1.13 times the mass and 1.27 times the radius of the Sun. It is radiating 1.5 times the Sun's luminosity from its photosphere at an effective temperature of 5,836 K.
In 2020, a stellar companion was identified using high-contrast imaging. The study authors deem this most likely a K-type main-sequence star with a class of K5V, an angular separation of along a position angle (PA) of 300° corresponding to a projected separation of , and around 11–15% of the mass of the Sun. An independent study published in 2021 identified a companion through speckle imaging. They propose this is a faint red dwarf with a class of M6 or later and a visual magnitude difference of 7.9 or more compared to the primary. It is located at a separation of along a PA of 121°, as of 2021.
A 2022 study claimed the presence of a brown dwarf companion to this star based on radial velocity and astrometry observations, but according to a 2023 follow-up study this was in fact a detection of the previously known stellar companion, poorly characterized due to the baseline of observations being much shorter than the companion's orbital period.
References.
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