Epoch J2000.0 Equinox J2000.0 (ICRS)
|Right ascension||06h 03m 55.18482s|
|Declination||+20° 08′ 18.4316″|
|Apparent magnitude (V)||4.63|
|U−B color index||−0.68|
|B−V color index||+0.28|
|R−I color index||+0.22|
|Variable type||α Cyg|
|Radial velocity (Rv)||16.8 ± 0.9 km/s|
|Proper motion (μ)|| RA: 1.88 mas/yr |
Dec.: −2.10 mas/yr
|Parallax (π)||1.81 ± 0.28 mas|
|Distance||approx. 1,800 ly |
(approx. 550 pc)
|Absolute magnitude (MV)||-7.6|
|Mass||42.3 ± 1.0 M☉|
|Surface gravity (log g)||2.35 cgs|
|Rotational velocity (v sin i)||72 km/s|
|Age||5 ± 0.6 Myr|
Chi2 Orionis (Chi2 Ori / χ2 Orionis / χ2 Ori) // is a B-type supergiant star in the constellation of Orion. It has an apparent visual magnitude of 4.63 but being quite distant, and heavily extinguished it burns with the greatest absolute visual light magnitude among stars in Orion within the near reaches of the galaxy, 0.9 of a magnitude greater than Rigel. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.
In apparent brightness it ranks, within Orion, admitting the higher published mean brightness of much more variable stars ranked above it, 35th.
Chi1 Orionis is an unrelated, yellow, main sequence star over two degrees away.
χ2 Orionis has a B2 bright supergiant spectrum and is one of the standard B2 Ia stars. It has been reported as having unusually narrow absorption lines and some weak emission lines and was included as one of the original Be stars. It is no longer treated as a Be star since many supergiants show some emission features at high resolution and Be stars is usually defined to exclude supergiants.
χ2 Orionis was listed as having likely small amplitude variability in photometry for the Third Catalogue of Stars measured in the Geneva Observatory Photometric System, specifically varying by 22 thousandths of a magnitude. It was included in the General Catalogue of Variable Stars based on Hipparcos satellite photometry with a magnitude range (in the Hipparchos photometric system) of 4.68 - 4.72 and a period of 2.8 days. A detailed study of the Hipparcos photometry confirmed the star as an α Cyg variable and gave the amplitude of variation as 0.057 magnitudes.
- van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
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- HR 2135, database entry, The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version), D. Hoffleit and W. H. Warren, Jr., CDS ID V/50. Accessed on line January 14, 2011.
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- Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (1999). "The 74th Special Name-list of Variable Stars". Information Bulletin on Variable Stars. 4659: 1. Bibcode:1999IBVS.4659....1K.
- Lefèvre, L.; Marchenko, S. V.; Moffat, A. F. J.; Acker, A. (2009). "A systematic study of variability among OB-stars based on HIPPARCOS photometry". Astronomy and Astrophysics. 507 (2): 1141. Bibcode:2009A&A...507.1141L. doi:10.1051/0004-6361/200912304.