Astronomy:V810 Centauri

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Short description: Star in the constellation Centaurus
V810 Cen A/B
250px
A visual band light curve for V810 Centauri, adapted from Kienzle et al. (1998)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Centaurus
Right ascension  11h 43m 31.192s[2]
Declination −62° 29′ 21.83″[2]
Apparent magnitude (V) 5.021var[1]
Characteristics
Spectral type F8Ia + B0III[1]
U−B color index 1.762[1]
B−V color index 0.014[1]
Variable type SRd[3]
Astrometry
Radial velocity (Rv)+16.44[4] km/s
Proper motion (μ) RA: −6.0[2] mas/yr
Dec.: +1.3[2] mas/yr
Parallax (π)0.1537 ± 0.0927[2] mas
Distance7,600+200
−210 ly
(2,330+61
−65 pc)
Absolute magnitude (MV)−8.4 (A) / −5.1 (B)[1]
Details
V810 Cen A
Mass20[1] M☉
Radius222±20[5] R☉
Luminosity55,000+12,700
−12,300[5] L☉
Surface gravity (log g)0.7[1] cgs
Temperature5,970±100[5] K
V810 Cen B
Mass25[1] M☉
Radius14[1] R☉
Luminosity125,000[1] L☉
Surface gravity (log g)3.5[1] cgs
Temperature29,000[1] K
Other designations
HIP 57175, SAO 251555, CD−61°3163, HR 4511, CPD−61°2559, HD 101947.
Database references
SIMBADdata

V810 Centauri is a double star consisting of a yellow supergiant[1] primary (V810 Cen A) and a blue giant secondary (V810 Cen B). It is a small-amplitude variable star, entirely due to the supergiant primary which is visually over three magnitudes (about 12x) brighter than the secondary.[6] It is the MK spectral standard for class G0 0-Ia.[7] A 5th magnitude star, it is visible to the naked eye under good observing conditions.

Maurice Pim FitzGerald announced that the star's brightness varies, in 1973.[8] It was given its variable star designation, V810 Centauri, in 1979.[9] V810 Cen A shows semi-regular variations with several component periods. The dominant mode is around 156 days and corresponds to Cepheid fundamental mode radial pulsation. Without the other stellar pulsation modes it would be considered a Classical Cepheid variable. Other pulsation modes have been detected at 89 to 234 days, with the strongest being a possible non-radial p-mode at 107 days and a possible non-radial g-mode at 185 days.[1]

The blue giant secondary has a similar mass and luminosity to the supergiant primary, but is visually much fainter. The primary is expected to have lost around 5 M☉ since it was on the main sequence, and has expanded and cooled so it lies at the blue edge of the Cepheid instability strip. It is expected to get no cooler and may perform a blue loop while slowly increasing in luminosity.[1]

V810 Cen is thought to be a member of the Stock 14 open cluster at 2,600 parsecs (8,500 light-years).[10] There are indications that it might be part of another cluster at a similar distance, but most of its members appear to be over 1° away from V810 Cen.[5] Spectroscopic and photometric estimates were consistent with a distance between 3,200 and 3,500 parsecs (10,000 and 11,000 light-years),[1] but an analysis of the interstellar reddening exclude such high distances, indicating that the star is somewhat closer.[5]

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 1.14 1.15 1.16 Kienzle, F.; Burki, G.; Burnet, M.; Meynet, G. (1998). "The pulsating yellow supergiant V810 Centauri". Astronomy and Astrophysics 337: 779. Bibcode: 1998A&A...337..779K. 
  2. ↑ 2.0 2.1 2.2 2.3 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. ↑ 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. Bibcode: 2009yCat....102025S. 
  4. ↑ Mermilliod, J. C.; Mayor, M.; Udry, S. (2008). "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters". Astronomy and Astrophysics 485 (1): 303–314. doi:10.1051/0004-6361:200809664. Bibcode: 2008A&A...485..303M. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Kasikov, A.; Mehner, A.; Kolka, I.; Aret, A. (2026-02-02). "Painting a Family Portrait of the Yellow Super- and Hypergiants in the Milky Way I. Constraining the Distances and Luminosities". Astronomy and Astrophysics. 
  6. ↑ Eichendorf, W.; Lub, J.; Pakull, M.; Heck, A.; Isserstedt, J.; Reipurth, B.; Van Genderen, A. M. (1981). "On the nature of the 125-day Cepheid V 810 CEN /equals HR 4511/ - IUE spectra". Astronomy and Astrophysics 93: L5. Bibcode: 1981A&A....93L...5E. 
  7. ↑ Garcia, B. (1989). "A list of MK standard stars". Bulletin d'Information du Centre de Données Stellaires 36: 27. Bibcode: 1989BICDS..36...27G. 
  8. ↑ Fitzgerald, M. P. (March 1973). "Error analysis of the photoelectric catalogue". Astronomy and Astrophysics Supplement 9: 297–311. Bibcode: 1973A&AS....9..297F. 
  9. ↑ Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (April 1979). "64th Name-List of Variable Stars". Information Bulletin on Variable Stars 1581: 1–8. Bibcode: 1979IBVS.1581....1K. https://ibvs.konkoly.hu/pub/ibvs/1501/1581.pdf. Retrieved 22 December 2024. 
  10. ↑ Turner, D. G. (1982). "New UBV photometry for the open cluster Stock 14 and its Cepheid-like variable V810 Centauri /= HR 4511/". Publications of the Astronomical Society of the Pacific 94: 655. doi:10.1086/131039. Bibcode: 1982PASP...94..655T. 

Coordinates: Sky map 14h 39m 36.4951s, −60° 50′ 02.308″



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