Omega Orionis is a B-type main sequence star of spectral type B3 Ve[3] with an effective temperature of 19,000 K.[3] Including a large amount of ultravioletradiation, Omega Orionis shines with a Luminosity 6,031[6] times greater than the Sun's and it has a radius 5.9[5] times larger than solar radius, The projected rotation speed is 179 km/s – involves a period of 1.37[5] days rotation. However, actual rotation speed can reach 450 km / s, it estimated that its axis is inclined 24° relative to the line of sight.[8] The star has a mass 7.0[3] times that of the Sun, just below the limit beyond which stars explode as supernovas. Its age is estimated at 43.6[3] million years.
As a result of its rapid rotation, Omega Orionis is a Be class star. Among the stars of this class, Omega Orionis was the first where the magnetic field was measured and found to be 1000 times that of the Earth. Omega Orionis is, like many Be stars, a variable star whose brightness varies 0.19 magnitudes. Also, small variations have been observed due to non-radial pulsations with periods of 0.97 and 2.19 days.[8]
^Wielen, R.; et al. (1999), Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions, vol. 35, Veröffentlichungen des Astronomisches Rechen-Institut Heidelberg, Bibcode:1999VeARI..35....1W.
^ abcdeNeiner, C.; et al. (November 2012), "An investigation of the magnetic properties of the classical Be star ω Ori by the MiMeS Collaboration", Monthly Notices of the Royal Astronomical Society, 426 (4): 2738–2750, Bibcode:2012MNRAS.426.2738N, doi:10.1111/j.1365-2966.2012.21833.x.
