Mu Centauri

Mu Centauri
Diagram showing star positions and boundaries of the Centaurus constellation and its surroundings


Location of μ Centauri (circled)

Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension 13h 49m 36.98863s[1]
Declination −42° 28′ 25.4296″[1]
Apparent magnitude (V) +3.42[2] (+2.75 to +3.25)[3]
Characteristics
Spectral type B2 IV-Ve[4]
U−B color index −0.854[2]
B−V color index −0.205[2]
Variable type γ Cas[3]
Astrometry
Radial velocity (Rv)+9.1[5] km/s
Proper motion (μ) RA: −24.25[1] mas/yr
Dec.: −18.64[1] mas/yr
Parallax (π)6.45 ± 0.16[1] mas
Distance510 ± 10 ly
(155 ± 4 pc)
Details
Mass9.1 ± 0.2[4] M☉
Radius3.4 × 4.2[6] R☉
Luminosity2,089[7] L☉
Surface gravity (log g)3.95 (3.86–4.33)[6] cgs
Temperature22,410[6] K
Rotational velocity (v sin i)194[8] km/s
Age19.8 ± 1.7[4] Myr
Other designations
CD−41°8172, FK5 508, HD 120324, HIP 67472, HR 5193, SAO 224471.
Database references
SIMBADdata

Mu Centauri (μ Cen, 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. The apparent visual magnitude of this star is 3.42,[2] 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.[1]

The spectrum of Mu Centauri matches a stellar classification of B2 IV-Ve.[4] The 'e' suffix is used to mark the presence of emission lines, which indicates this is a Be star surrounded 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.[9] During these outbursts, the star can experience transient periodicities.[10] Mu Centauri is classified as a Gamma Cassiopeiae typevariable star and its brightness varies from magnitude +2.75 to +3.25.[3]

This star is spinning rapidly, with a projected rotational velocity of 194,[8] 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.[7]

At an estimated age of nearly 20 million years,[4] this star is around 55–65% of the way through its evolutionary period on the main sequence of core hydrogen burning stars.[6] It has around nine[4] times the mass of the Sun and four[6] times the Sun's radius, but emits over 2,000[7] times as much energy as the Sun. The outer atmosphere has a mean effective temperature of 22,410 K,[6] giving the star a blue-white hue.[11]

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.[12]

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752 Freely accessible. doi:10.1051/0004-6361:20078357.
  2. 1 2 3 4 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168
  3. 1 2 3 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/gcvs. 1: 02025. Bibcode:2009yCat....102025S.
  4. 1 2 3 4 5 6 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, Bibcode:2011MNRAS.410..190T, arXiv:1007.4883 Freely accessible, doi:10.1111/j.1365-2966.2010.17434.x
  5. ↑ Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick, eds., The Revision of the General Catalogue of Radial Velocities, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E
  6. 1 2 3 4 5 6 Zorec, J.; Frémat, Y.; Cidale, L. (October 2005), "On the evolutionary status of Be stars. I. Field Be stars near the Sun", Astronomy and Astrophysics, 441 (1): 235–248, Bibcode:2005A&A...441..235Z, arXiv:astro-ph/0509119 Freely accessible, doi:10.1051/0004-6361:20053051
  7. 1 2 3 Rivinius, Th.; et al. (April 2001), "Stellar and circumstellar activity of the Be star mu Centauri. III. Multiline nonradial pulsation modeling", Astronomy and Astrophysics, 369: 1058–1077, Bibcode:2001A&A...369.1058R, doi:10.1051/0004-6361:20010185
  8. 1 2 Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago. 239 (1). Bibcode:1970CoAsi.239....1B.
  9. ↑ Rivinius, Th.; et al. (May 1998), "Stellar and circumstellar activity of the Be star MU Centauri. I. Line emission outbursts", Astronomy and Astrophysics, 333: 125–140, Bibcode:1998A&A...333..125R
  10. ↑ Rivinius, Th.; Baade, D.; Štefl, S. (November 2003), "Non-radially pulsating Be stars", Astronomy and Astrophysics, 411: 229–247, Bibcode:2003A&A...411..229R, doi:10.1051/0004-6361:20031285
  11. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16
  12. ↑ de Geus, E. J.; de Zeeuw, P. T.; Lub, J. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1-2): 44–61, Bibcode:1989A&A...216...44D
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.