V763 Centauri

In today's world, V763 Centauri has become increasingly relevant. Whether due to its impact on society, its influence on popular culture, or its importance in academia, V763 Centauri has become a topic of interest for people of all ages and professions. Since its inception, V763 Centauri has generated passionate debate and has been the subject of intense study and research. Without a doubt, V763 Centauri is a multifaceted topic that covers a wide range of aspects, and that deserves to be explored in depth to understand its true scope and meaning in today's world.

This article is about C1 Centauri. For c1 Centauri, see HD 129456. For other stars with this Bayer designation, see C Centauri.
C1 Centauri

A light curve for V763 Centauri, plotted from Hipparcos data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Centaurus
Right ascension 11h 35m 13.28134s[2]
Declination −47° 22′ 21.2888″[2]
Apparent magnitude (V) +5.64[3]
Characteristics
Evolutionary stage AGB[4]
Spectral type M3/4III[5]
B−V color index +1.682±0.019[3]
Variable type Lb[6]
Astrometry
Radial velocity (Rv)+21.07±0.29[2] km/s
Proper motion (μ) RA: -87.503[2] mas/yr
Dec.: -6.988[2] mas/yr
Parallax (π)5.4236±0.1476 mas[2]
Distance600 ± 20 ly
(184 ± 5 pc)
Absolute magnitude (MV)−1.05[3]
Details
Radius64.7+5.9
−4.3[2] R☉
Luminosity754±24[2] L☉
Temperature3,761+130
−161[2] K
Other designations
C1 Cen, V763 Centauri, CD−46°7199, GC 15886, HD 100733, HIP 56518, HR 4463, SAO 222887, CCDM J11352-4722[7]
Database references
SIMBADdata

C1 Centauri is a single[8] star in the southern constellation of Centaurus. It has the variable star designation V763 Centauri, while C1 Centauri is the Bayer designation. The star has a red hue and is dimly visibly to the naked eye with an apparent visual magnitude that fluctuates around +5.64.[3] It is located at a distance of approximately 600 light years based on parallax, and has an absolute magnitude of −1.05.[3] It is drifting further away with a radial velocity of +21 km/s.[2] At one time it was a candidate member of the Zeta Herculis Moving Group but has since been excluded.[9]

This object is an aging red giant star on the asymptotic giant branch[4] with a stellar classification of M3/4III.[5] Samus et al. (2017) classify this as a slow irregular variable of sub-type Lb and its brightness varies from magnitude +5.52 down to +5.82.[6] It was previously classified as a semiregular variable of sub-type SRb.[10] With the supply of hydrogen and helium at its core exhausted, the star has expanded until now it has 65 times the radius of the Sun. It is radiating 754 times the luminosity of the Sun from its photosphere at an effective temperature of 3,761 K.[2]

References

  1. ^ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. ^ a b c d e f g h i j k Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. ^ a b c d e 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, S2CID 119257644.
  4. ^ a b Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal, 104 (1): 275–313, Bibcode:1992AJ....104..275E, doi:10.1086/116239.
  5. ^ a b Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 2, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  6. ^ a b Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  7. ^ "HD 100733". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-03-02.
  8. ^ 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.
  9. ^ Eggen, O. J. (June 1971), "The ζ Herculis, σ Puppis, ∈ Indi, and η Cephei Groups of Old Disk Population Stars", Publications of the Astronomical Society of the Pacific, 83 (493): 251, Bibcode:1971PASP...83..251E, doi:10.1086/129119.
  10. ^ Kerschbaum, F.; Hron, J. (September 1994), "Semiregular variables of types SRa and SRb. New JHKL'M-photometry for 200 stars", Astronomy and Astrophysics Supplement, 106: 397–411, Bibcode:1994A&AS..106..397K.