HD 4391 is a triple star system[8] in the constellationPhoenix that is located at a distance of 48.7 light years from the Sun. The primary has a stellar classification of G3V, which is a G-type main sequence star. The physical properties of this star are similar to the Sun, making it a solar analog. However, it is believed to have 22% greater mass than the Sun and is only 1.2 billion years old.[5] The spectrum for this star displays an abnormally low level of beryllium, which may be the result of some form of mixing process.[6]
No planet has been detected in orbit around this star,[5] nor does it emit a statistically significant excess of infrared radiation that might indicate a debris disk.[9] However, it has two companions that share a common proper motion through space with HD 4391, effectively making it a triple star system. The first, a red dwarf of type M4, lies at an angular separation of 17″ from the primary. The second is a type M5 star at a separation of 49″.[8]
^ abJohnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
^Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Alan Henry Batten; John Frederick Heard (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: Academic Press, London. p. 57. Bibcode:1967IAUS...30...57E.