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Beta Chamaeleontis is the third-brightest star in the southern constellation of Chamaeleon. Its name is a Bayer designation that is Latinized from β Chamaeleontis, and abbreviated Beta Cha or β Cha. A solitary,[14] suspected variable star,[4] it is visible to the naked eye as a faint blue-white point of light with an apparent visual magnitude that has been measured ranging between 4.24 and 4.30.[4] Parallax measurements yield a distance estimate of 298 light-years (91 pc) from the Sun. It is drifting further away with a radial velocity of +23 km/s.[9]

This is a B-type main-sequence star with a stellar classification of B4 V[6] that is generating energy through core hydrogen fusion. It has been catalogued both as a Be star[3] and a normal star.[15] Based on pulsation measurements made by the TESS space telescope, this is a slowly pulsating B-type variable.[7]

Beta Chamaeleontis is about 23[10] million years old with a high projected rotational velocity of 255 km/s.[8] The rapid rotation is creating an equatorial bulge that is 12% larger than the polar radius.[16] The star has five[10] times the mass of the Sun and 2.8[11] times the Sun’s radius. It is radiating 212[12] times the luminosity of the Sun from its photosphere at an effective temperature of 14,495 K.[11]

References

  1. ^ a b Anderson, E.; Francis, Ch. (2012), “XHIP: An extended hipparcos compilation”, Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL…38..331A, doi:10.1134/S1063773712050015 XHIP record for this object at VizieR.
  2. ^ a b c d van Leeuwen, F. (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, S2CID 18759600.
  3. ^ a b c d Feinstein, A.; Marraco, H. G. (November 1979), “The photometric behavior of Be Stars”, Astronomical Journal, 84: 1713–1725, Bibcode:1979AJ…..84.1713F, doi:10.1086/112600.
  4. ^ a b c Samus’, N. N; et al. (2017), “General catalogue of variable stars”, Astronomy Reports, 5.1, 61 (1): 80, Bibcode:2017ARep…61…80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  5. ^ Vallenari, A.; et al. (Gaia collaboration) (2023), “Gaia Data Release 3. Summary of the content and survey properties”, Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A…674A…1G, doi:10.1051/0004-6361/202243940, S2CID 244398875 Gaia DR3 record for this source at VizieR.
  6. ^ a b Houk, N.; Cowley, A. P. (1975), “Catalogue of two-dimensional spectral types for the HD stars”, University of Michigan, I, Bibcode:1975mcts.book…..H
  7. ^ a b c Balona, L. A.; Ozuyar, D. (2020), “Pulsation among TESS a and B stars and the Maia variables”, Monthly Notices of the Royal Astronomical Society, 493 (4): 5871, arXiv:2001.04497, Bibcode:2020MNRAS.493.5871B, doi:10.1093/mnras/staa670.
  8. ^ a b c Hoffleit, D.; Warren, Jr., W. H., “HR 4674, database entry”, The Bright Star Catalogue (5th Revised (Preliminary Version) ed.), Centre de Données astronomiques de Strasbourg, retrieved September 5, 2008. ID V/50.
  9. ^ a b Wielen, R.; et al. (1999), “Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions”, Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg, 35 (35), Astronomisches Rechen-Institut Heidelberg: 1, Bibcode:1999VeARI..35….1W.
  10. ^ a b c d Tetzlaff, N.; et al. (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, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873
  11. ^ a b c d e Fitzpatrick, E. L.; Massa, D. (March 2005), “Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry”, The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ….129.1642F, doi:10.1086/427855, S2CID 119512018
  12. ^ a b McDonald, I.; et al. (2012), “Fundamental Parameters and Infrared Excesses of Hipparcos Stars”, Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  13. ^ “bet Cha”, SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-12-10.
  14. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), “A catalogue of multiplicity among bright stellar systems”, Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  15. ^ Grady, C. A.; et al. (September 1987), “Highly Ionized Stellar Winds in Be Stars: The Evidence for Aspect Dependence”, Astrophysical Journal, 320: 376, Bibcode:1987ApJ…320..376G, doi:10.1086/165551
  16. ^ van Belle, Gerard T. (March 2012), “Interferometric observations of rapidly rotating stars”, The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20…51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.