Omega Orionis

{{Starbox begin

| name = ω Orionis

}}

{{Starbox image

|image=

{{Location mark

|image=Orion constellation map.svg|alt=|float=center|width=280

|label=|position=right

|mark=Red circle.svg|mark_width=10|mark_link=ω Orionis

|x=558|y=402

}}

|caption=Location of ω Orionis (circled)

}}

{{Starbox observe

| epoch = J2000.0

| equinox = J2000.0 (ICRS)

| constell = Orion

| ra = {{RA|05|39|11.14632}}

| dec = {{DEC|+04|07|17.2795}}

| appmag_v = 4.57

}}

{{Starbox character

| class = B3 Ve

| b-v = −0.11

| u-b = −0.76

| r-i =

| variable =

}}

{{Starbox astrometry

| radial_v = 20.4

| prop_mo_ra = +0.84

| prop_mo_dec = +0.00

| parallax = 2.36

| p_error = 0.29

| parallax_footnote =

| absmag_v =

}}

{{Starbox detail

| source =

| mass = {{Val|7.0|0.5}}

| radius = 5.9

| luminosity = 6,031

| temperature = {{Val|19000|500|fmt=commas}}

| gravity = {{Val|3.59|0.10}}

| metal_fe =

| rotational_velocity = {{Val|179|4}}

| rotation = 1.37 d

| age_myr = 43.6

}}

{{Starbox catalog

| names = ω Ori, 47 Orionis, BD+04° 1002, FK5 2423, HD 37490, HIP 26594, HR 1934, SAO 113001.

}}

{{Starbox reference

| Simbad = ome+Ori

}}

Omega Orionis (ω Ori) is a single star in the constellation Orion. Its apparent magnitude is 4.57 and is located approximately 1,400 light-years from the Solar System. It is surrounded by a cloud of dust, forming a modest reflection nebula over a light-year wide.

File:OmegaOriLightCurve.png light curve for Omega Orionis, adapted from Balona et al. (2001)]]

Omega Orionis is a B-type main sequence star of spectral type B3 Ve with an effective temperature of 19,000 K. Including a large amount of ultraviolet radiation, Omega Orionis shines with a Luminosity 6,031 times greater than the Sun's and it has a radius 5.9 times larger than solar radius, The projected rotation speed is 179 km/s – involves a period of 1.37 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. The star has a mass 7.0 times that of the Sun, just below the limit beyond which stars explode as supernovas. Its age is estimated at 43.6 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.

References

{{reflist|refs=

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{{cite journal

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| journal=Monthly Notices of the Royal Astronomical Society

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{{citation

| title=An investigation of the magnetic properties of the classical Be star ω Ori by the MiMeS Collaboration

| display-authors=1

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| postscript=. | doi-access=free }}

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{{citation

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| title=Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions

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| volume=35 | date=1999

| page=1 | bibcode=1999VeARI..35....1W | postscript=. }}

{{citation

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| title=Photoelectric photometric Catalogue of homogeneous measurements in the UBV System

| journal=Astronomy and Astrophysics Supplement Series

| volume=34 | pages=1–49 | year=1978

| bibcode=1978A&AS...34....1N | postscript=. }}

{{cite journal

| title=Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical Be Stars | year=2021

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