Astronomy:V Centauri

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Short description: Variable star in the constellation Centaurus

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V Centauri
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A light curve for V Centauri, plotted from Hipparcos data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Centaurus
Right ascension  14h 32m 33.0833s[2]
Declination −56° 53′ 15.774″[2]
Apparent magnitude (V) 6.42 - 7.22[3]
Characteristics
Spectral type F5 Ib/II[4]
B−V color index 0.87[5]
Variable type Classical Cepheid[3]
Astrometry
Radial velocity (Rv)−18.90 ± 1.4[6] km/s
Proper motion (μ) RA: −6.697[2] mas/yr
Dec.: −7.068[2] mas/yr
Parallax (π)1.3898 ± 0.0221[2] mas
Distance2,350 ± 40 ly
(720 ± 10 pc)
Details
Mass4.3[7] M☉
Radius40[2] R☉
Luminosity1,657[8] L☉
Surface gravity (log g)1.89[2] cgs
Temperature5,500[8] K
Metallicity [Fe/H]+0.12[9] dex
Age103[10] Myr
Other designations
V Cen, CD−56°5479, HD 127297, HIP 71116, HR 5421, SAO 241777[5]
Database references
SIMBADdata

V Centauri (V Cen) is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years (720 parsecs) away based on parallax.

Alexander W. Roberts discovered this star in 1894, and from 267 visual observations he determined is period of variation.[11] V Centauri varies regularly between visual magnitudes 6.42 and 7.22 every 5.5 days. It is classified as a Cepheid variable on the basis of its light variations, with the brightness increase from minimum to maximum taking only a third of the time of the decrease from maximum to minimum. Cepheids are pulsating variable stars and V Centauri expands and contracts over its pulsation cycle as well as changing temperature.[3]

According to the South African Astronomical Observatory, the chemical composition was derived as being high in sodium (Na) and aluminium (Al) and low in magnesium (Mg).[12] Following a normal composition for a Cepheid star, V Cen does not have any unusual characteristics. V Centauri's composition was observed alongside six other Classical Cepheid variable stars with the support of Russian, Chilean, and Ukrainian observatories.[12]

References

  1. ↑ "Hipparcos Tools Interactive Data Access". ESA. https://www.cosmos.esa.int/web/hipparcos/interactive-data-access. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1: B/GCVS. Bibcode: 2009yCat....102025S. 
  4. ↑ Houk, N.; Cowley, A. P. (1975). "University of Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars. Volume I. Declinations -90°.0 to -53°.0.". Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars 1. Bibcode: 1975mcts.book.....H. 
  5. ↑ 5.0 5.1 "V* V Cen". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+V+Cen. 
  6. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  7. ↑ Marconi, Marcella et al. (July 2020). "Predicted Masses of Galactic Cepheids in the Gaia Data Release 2". The Astrophysical Journal Letters 898 (1): L7. doi:10.3847/2041-8213/aba12b. L7. Bibcode: 2020ApJ...898L...7M. 
  8. ↑ 8.0 8.1 Groenewegen, M. A. T. (2020). "Analysing the spectral energy distributions of Galactic classical Cepheids". Astronomy and Astrophysics 635: A33. doi:10.1051/0004-6361/201937060. Bibcode: 2020A&A...635A..33G. 
  9. ↑ Ripepi, V.; Catanzaro, G.; Clementini, G.; De Somma, G.; Drimmel, R.; Leccia, S.; Marconi, M.; Molinaro, R. et al. (2022). "Classical Cepheid period-Wesenheit-metallicity relation in the Gaia bands". Astronomy and Astrophysics 659: A167. doi:10.1051/0004-6361/202142649. Bibcode: 2022A&A...659A.167R. 
  10. ↑ Skowron, D. M.; Skowron, J.; Mróz, P.; Udalski, A.; Pietrukowicz, P.; Soszyński, I.; Szymański, M. K.; Poleski, R. et al. (2019). "Mapping the Northern Galactic Disk Warp with Classical Cepheids". Acta Astronomica 69 (4): 305. doi:10.32023/0001-5237/69.4.1. Bibcode: 2019AcA....69..305S. 
  11. ↑ Voûte, J. (1927). "V Centauri". Annals of the Bosscha Observatory Lembang (Java) Indonesia 2: B42-B45. Bibcode: 1927AnBos...2B..42V. https://articles.adsabs.harvard.edu/pdf/1927AnBos...2B..42V. Retrieved 14 January 2025. 
  12. ↑ 12.0 12.1 Usenko, I. A.; Kniazev, A. Yu; Berdnikov, L. N.; Kravtsov, V. V.; Fokin, A. B. (2013-07-01). "Spectroscopic studies of southern-hemisphere Cepheids: Six objects in Centaurus (V Cen, V737 Cen) and Sagittarius (BB Sgr, W Sgr, X Sgr, Y Sgr)" (in en). Astronomy Letters 39 (7): 432–445. doi:10.1134/S1063773713070074. ISSN 1063-7737. Bibcode: 2013AstL...39..432U. 



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