HD 164427

HD 164427 is a star with a likely red dwarf companion in the southern constellation of Pavo. It has an apparent visual magnitude of 6.88, placing it just below the nominal limit for visibility with the typical naked eye. The annual parallax shift of $0.624$ yields a distance estimate of 139 ly. It is moving further from the Earth with a heliocentric radial velocity of +3.4 km/s.

This is an inactive G-type main-sequence star given a stellar classification of G0+V by Gray et al. (2006), although Evans et al. (1964) classified it as a subgiant star with luminosity class IV. It is 6.6 billion years old with 1.125 times the mass of the Sun and 1.40 times the Sun's radius. The star is somewhat over-luminous for its class, radiating 2.33 times the Sun's luminosity from its photosphere at an effective temperature of 5,876 K.

Companions
In 2001, a brown dwarf candidate companion was announced by Anglo-Australian Planet Search program. It was detected by the Doppler velocity technique with an echelle spectrograph attached to the 3.92m Anglo-Australian Telescope. A magnitude 12.60 companion star designated HD 164427 B lies at an angular separation of $3.4$ along a position angle of 336°, as of 2010. This is a suspected common proper motion companion with 52% of the Sun's mass and a physical separation of as much as $3.98$.

HD 164427 b was initially thought to be a brown dwarf based on its minimum mass of 46 times that of Jupiter. In 2023, an astrometric orbit for this object was published using data from Gaia, showing its true mass to be, making it a likely red dwarf star. This stellar companion orbits at nearly half an astronomical unit or Earth-to-Sun distance away from its primary. The angular separation between the two stars as viewed from Earth is 11.76 milliarcseconds. It takes 108.55 Earth days to orbit eccentrically around HD 164427. It has a very high semi-amplitude of almost 1400 m/s, because this is a very massive object which exerts strong gravitational pull on its tugging star.