Gamma Centauri,
Latinized from γ Centauri, is a
binary star system in the
southernconstellation of
Centaurus. It has the proper name Muhlifain,[10] not to be confused with Muliphein, which is
γ Canis Majoris; both names derive from the same Arabic root. The system is visible to the naked eye as a single point of light with a combined
apparent visual magnitude of +2.17;[2] individually they are third-magnitude stars.[3]
This system is located at a distance of about 130
light-years (40
parsecs) from the
Sun based on
parallax. In 2000, the pair had an angular separation of 1.217
arcseconds with a
position angle of 351.9°.[3] Their positions have been observed since 1897, which is long enough to estimate an
orbital period of 84.5 years and a
semimajor axis of 0.93 arcsecond.[11][8] At the distance of this system, this is equivalent to a physical separation of about 93
AU.[12]
The combined
stellar classification of the pair is A1IV+;[4] when they are separated out they have individual classes of A1IV and A0IV,[5] suggesting they are
A-typesubgiant stars in the process of becoming
giants. The star
Tau Centauri is relatively close to Gamma Centauri, with an estimated separation of 1.72 light-years (0.53 parsecs).[9] There is a 98% chance that they are
co-moving stars.[8]
^
abcdJohnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99.
Bibcode:
1966CoLPL...4...99J.
^
abcFabricius, C.; Makarov, V. V. (April 2000). "Two-colour photometry for 9473 components of close Hipparcos double and multiple stars". Astronomy and Astrophysics. 356: 141–145.
Bibcode:
2000A&A...356..141F.