HD 4391 is a quadruplestar system[10] in theconstellationPhoenix that is located at a distance of 49.1light years from theSun. The primary has astellar classification of G3V, which is aG-type main sequence star. The physical properties of this star are similar to the Sun, making it asolar analog. However, it is believed to have 6% greater mass than the Sun[6] and is only 800 million years old.[7] The spectrum for this star displays an abnormally low level of beryllium, which may be the result of some form of mixing process.[8]
No planet has been detected in orbit around this star,[11] nor does it emit a statistically significantexcess of infrared radiation that might indicate adebris disk.[12] However, it has three companions that share acommon proper motion through space with HD 4391, effectively making it a quadruple star system. HD 4391 B, a pair ofred dwarfs of combined spectrum M4, lies at anangular separation of 17″ from the primary, with the two components designated Ba and Bb. HD 4391 C is a type M5 star at a separation of 49″.[13][10] The close red dwarf pair are also sometimes designated HD 4391 B and HD 4391 C, with the outer component being named HD 4391 D.[14][15]
^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.
