Mu Centauri
{{Short description|Variable star in the constellation Centaurus}}
{{Starbox begin}}
{{Starbox image
| image =
{{Location mark
| image=Centaurus constellation map.svg
| float=center | width=280 | position=right
| mark=Red circle.svg | mark_width=10 | mark_link=μ Cen
| x=442 | y=448
}}
| caption = Location of μ Centauri (circled)
}}
{{Starbox observe
| epoch = J2000.0
| constell = Centaurus
| dec = {{DEC|−42|28|25.4296}}
| appmag_v = {{nowrap|+3.42 (+2.92 to +3.49)}}
}}
{{Starbox character
| variable = γ Cas
}}
{{Starbox astrometry
| parallax = 6.45
| p_error = 0.16
}}
{{Starbox detail
| radius = 4.21 (equatorial)
{{Val|3.4|0.3}} (polar)
| gravity = 3.86 (equatorial)
4.33 (polar)
| metal_fe =
| temperature = 17,600 (equatorial)
{{Val|23200|200|fmt=commas}} (polar)
}}
{{Starbox catalog
| names = {{odlist | B=μ Cen | CD=−41°8172 | FK5=508 | HD=120324 | HIP=67472 | HR=5193 | SAO=224471 }}
}}
{{Starbox reference
| Simbad=HD+120324
}}
{{Starbox end}}
Mu Centauri, Latinized from μ Centauri, is a third-magnitude star in the southern constellation of Centaurus. With the stars ν and φ Centauri, it marks what has been traditionally portrayed as "dextro Latere" (the right side) of the Centaur.[https://web.archive.org/web/20071115020105/http://astro.isi.edu/reference/almagest.html] The apparent visual magnitude of this star is 3.42, making it one of the brighter members of the constellation. The distance to this star can be estimated directly using parallax measurements, which yield a value of roughly 510 light years (155 parsecs) from Earth.
File:MuCenLightCurve.png light curve for Mu Centauri, plotted from data published by Aguayo et al. (2018)]]
The spectrum of Mu Centauri is considered to be a standard for a B2 Be star with the stellar classification of B2V:e. The 'e' suffix is used to mark the presence of emission lines, caused by a circumstellar disk of hot gas that was formed from material ejected from the star. Mu Centauri is a pulsating variable star that has multiple non-radial cycles with a primary period of 0.503 days. Three other pulsation cycles have a similar period, while two have a shorter interval of about 0.28 days. It undergoes outburst events that result in the transfer of additional material to the surrounding disk. During these outbursts, the star can experience transient periodicities. Mu Centauri is classified as a Gamma Cassiopeiae type variable star and its brightness varies from magnitude +2.92 to +3.49.
This star is spinning rapidly, with a projected rotational velocity of 194, km s−1 and is completing a full rotation in about 11.615 hours. The equatorial azimuthal velocity is around 85% of the critical velocity where the star would start to break up, resulting a pronounced equatorial bulge that is about 26% wider than the radius at the poles. Because of the oblate spheroidal shape of this star, the polar region is at a higher temperature than the equator—23,000 K versus 17,600 K respectively. Likewise, the gravitational force at the poles is greater than along the equator. The axis of rotation of the star is tilted by an angle of about (19 ± 3)° to the line of sight from the Earth.
At an estimated age of nearly 20 million years, this star is around 55–65% of the way through its evolutionary period on the main sequence of core hydrogen burning stars. It has around nine times the mass of the Sun and four times the Sun's radius, but emits over 2,000 times as much energy as the Sun. The outer atmosphere has a mean effective temperature of 22,410 K, giving the star a blue-white hue.
This star is a proper motion member of the Upper Centaurus–Lupus sub-group in the
Scorpius–Centaurus OB association,
the nearest such co-moving association of massive stars to the Sun.
References
{{reflist|30em|refs=
| title=XHIP: An extended hipparcos compilation
| last1=Anderson | first1=E. | last2=Francis | first2=Ch.
| journal=Astronomy Letters
| volume=38 | issue=5 | pages=331 | year=2012
| bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015
| arxiv=1108.4971 | s2cid=119257644 | postscript=. }}
{{citation | last=Evans | first=D. S. | date=June 20–24, 1966 | editor1-last=Batten | editor1-first=Alan Henry | editor2-last=Heard | editor2-first=John Frederick | title=The Revision of the General Catalogue of Radial Velocities | work=Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30 | volume=30 | page=57 | location=University of Toronto | publisher=International Astronomical Union | bibcode=1967IAUS...30...57E }}
{{citation | last1=Tetzlaff | first1=N. | last2=Neuhäuser | first2=R. | last3=Hohle | first3=M. M. | title=A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun | journal=Monthly Notices of the Royal Astronomical Society | volume=410 | issue=1 | pages=190–200 |date=January 2011 | doi=10.1111/j.1365-2966.2010.17434.x | doi-access=free | bibcode=2011MNRAS.410..190T |arxiv = 1007.4883 | s2cid=118629873 }}
{{citation | title=The Colour of Stars | date=December 21, 2004 | work=Australia Telescope, Outreach and Education | publisher=Commonwealth Scientific and Industrial Research Organisation | url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | access-date=2012-01-16 | archive-url=https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html | archive-date=March 18, 2012 | url-status=dead }}
| display-authors=1 | last1=Samus | first1=N. N.
| last2=Kazarovets | first2=E. V. | last3=Durlevich | first3=O. V.
| last4=Kireeva | first4=N. N. | last5=Pastukhova | first5=E. N.
| title=General Catalogue of Variable Stars
| version=5.1 | journal=Astronomy Reports
| year=2017 | volume=61 | issue=1 | pages=80–88
| bibcode=2017ARep...61...80S | s2cid=125853869
| doi=10.1134/S1063772917010085 }}
}}
{{Stars of Centaurus}}
{{DEFAULTSORT:Mu Centauri}}
Category:B-type main-sequence stars
Category:Gamma Cassiopeiae variable stars
Category:Upper Centaurus Lupus