B_Velorum_(supergiant)

HD 74180

HD 74180

Supergiant star in the constellation Vela

This article is about b Velorum. For B Velorum, see HD 70930.

HD 74180 is a single[11] star in the constellation Vela. It is a yellow-white F-type supergiant with a mean apparent magnitude of +3.81 and a spectral classification F8Ib. Estimates of its distance to Earth vary between 3,200 and 8,300 light-years.

A light curve for HD 74180, adapted from van Leeuwen et al. (1998)[5]
Quick Facts Observation data Epoch J2000 Equinox J2000, Constellation ...

b Velorum has been classified as a suspected α Cygni variable star which varies by only 0.06 magnitude. There are possible periods near 53, 80, and 160 days, but the variation is largely irregular.[5] It lies less than a degree from the small open cluster NGC 2645, but is not a member.[3]

Several studies have considered b Velorum to be a highly luminous supergiant or hypergiant with an early F spectral type, for example F2 Ia+,[5] F0 Ia,[12] and F4 I.[13] There were corresponding luminosity estimates of several hundred thousand L☉. A 2015 study used the Barbier-Chalonge-Divan (BCD) system to derive a luminosity of 38,000 L☉ and a cooler less luminous F8 Ib spectral type.[3]

Distance

Multiple papers give different distances for b Velorum. Bailer-Jones et al. (2021) give a distance of about 2,530 pc (8,300 ly).[8] The Hipparcos spacecraft give a parallax of 0.67±0.16 mas, translating into a distance of 1,492.5 pc (4,868 ly).[1] Aidelman et al. (2015) give a distance of 990 pc (3,200 ly).[3]

In chinese astronomy

In Chinese, 天社 (Tiān Shè), meaning Celestial Earth God's Temple, refers to an asterism consisting of Kappa Velorum, Gamma2 Velorum, b Velorum and Delta Velorum.[14] Consequently, Kappa Velorum itself is known as 天社五 (Tiān Shè wǔ), "the Fifth Star of Celestial Earth God's Temple".[15]

Notes

    1. Radius from temperature and bolometric magnitude. The bolometric magnitude is converted to solar luminosites in the equation (L = 10^(0.4*(4.74-(Mbol)))), where L is the luminosity and Mbol the bolometric magnitude
    2. From L = 10^(0.4*(4.74-(Mbol))), where L is the luminosity and Mbol the bolometric magnitude

    References

    1. [1]
      van Leeuwen, F. (2007-11-01). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474: 653–664. arXiv:0708.1752. doi:10.1051/0004-6361:20078357. ISSN 0004-6361. b Velorum's database entry at VizieR.
    2. [2]
      Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
    3. [3]
      Aidelman, Y.; Cidale, L. S.; Zorec, J.; Panei, J. A. (2015). "Open clusters. II. Fundamental parameters of B stars in Collinder 223, Hogg 16, NGC 2645, NGC 3114, and NGC 6025". Astronomy & Astrophysics. 577: A45. Bibcode:2015A&A...577A..45A. doi:10.1051/0004-6361/201425085. hdl:11336/14076.
    4. [4]
      Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672 b Velorum's database entry at VizieR.
    5. [5]
      Van Leeuwen, F.; Van Genderen, A. M.; Zegelaar, I. (1998). "Hipparcos photometry of 24 variable massive stars (α Cygni variables)". Astronomy and Astrophysics Supplement Series. 128: 117–129. Bibcode:1998A&AS..128..117V. doi:10.1051/aas:1998129.
    6. [6]
      Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
    7. [7]
      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.
    8. [8]
      Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021-03-01). "Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. ISSN 0004-6256. Data about this star can be seen here.
    9. [9]
      Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011-01-01). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410: 190–200. arXiv:1007.4883. doi:10.1111/j.1365-2966.2010.17434.x. ISSN 0035-8711. b Velorum's database entry at VizieR.
    10. [10]
      Luck, R. Earle (2014). "Parameters and Abundances in Luminous Stars". The Astronomical Journal. 147 (6): 137. Bibcode:2014AJ....147..137L. doi:10.1088/0004-6256/147/6/137.
    11. [11]
      Eggleton, P. P.; Tokovinin, A. A. (2008-09-01). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389: 869–879. arXiv:0806.2878. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. b Velorum's database entry at VizieR.
    12. [12]
      Humphreys, R. M. (1978). "Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way". Astrophysical Journal. 38: 309. Bibcode:1978ApJS...38..309H. doi:10.1086/190559.
    13. [13]
      Mersch, G.; Heck, A. (1980). "Prediction of spectral classification from photometric observations - Application of the UVBY beta photometry and the MK spectra classification. II - General case". Astronomy and Astrophysics. 85: 93. Bibcode:1980A&A....85...93M.
    14. [14]
      (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
    15. [15]
      (in Chinese) 香港太空館 – 研究資源 – 亮星中英對照表 Archived 2008-10-25 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
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