Astronomy:Omicron Puppis

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Short description: Variable Star in the constellation Puppis
Omicron Puppis
Puppis IAU.svg
Red circle.svg
Location of ο Puppis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Puppis
Right ascension  07h 48m 05.16839s[1]
Declination −25° 56′ 13.8123″[1]
Apparent magnitude (V) +4.48[2]
Characteristics
Spectral type B1 IVnne[3]
U−B color index −1.02[2]
B−V color index −0.09[2]
Variable type LERI
Astrometry
Radial velocity (Rv)+15.0[4] km/s
Proper motion (μ) RA: −10.09[1] mas/yr
Dec.: +4.26[1] mas/yr
Parallax (π)2.30 ± 0.23[1] mas
Distance1,400 ± 100 ly
(430 ± 40 pc)
Absolute magnitude (MV)−3.77[5]
Orbit[6]
Period (P)28.903±0.004 d
Eccentricity (e)0
Periastron epoch (T)2456012.93 ± 0.04
Semi-amplitude (K2)
(secondary)		159.7±11.7 km/s
Details
Mass15.5±0.8[7] M☉
Luminosity (bolometric)59,279[8] L☉
Temperature24,200[8] K
Rotational velocity (v sin i)315[9] km/s
Age11.1±0.5[7] Myr
Other designations
ο Pup, CPD−25° 2882, HD 63462, HIP 38070, HR 3045, SAO 174558, WDS J07481-2556A[10]
Database references
SIMBADdata

Omicron Puppis (ο Puppis) is candidate binary star[6] system in the southern constellation of Puppis. It is visible to the naked eye, having a combined apparent visual magnitude of +4.48.[2] Based upon an annual parallax shift of 2.30 mas as seen from Earth,[1] it is located roughly 1,400 light years from the Sun.

This is a suspected close spectroscopic binary system. The spectrum varies with a periodicity of 28.9 days, and a helium emission component shows a radial velocity variation that matches the period. The properties indicate it may be a φ Per-like system with a Be star primary and a hot subdwarf companion of type sdO. If this is the case, then the pair have a circular orbit with a period that matches the variability. The close-orbiting pair may have undergone interaction in the past, leaving the subdwarf stripped down and the primary star spinning rapidly.[6]

ο Puppis is slightly variable. The General Catalogue of Variable Stars lists it as a possible Be star with a magnitude range of 4.43 - 4.46.[11] The International Variable Star Index classifies it as a Lambda Eridani variable.[12]

Naming

The correct Bayer designation for ο Puppis has been debated. Lacaille assigned one Greek letter sequence for the bright stars of Argo Navis. These Lacaille designations are now shared across the three modern constellations of Carina, Puppis, and Vela so that the same Greek letter is not usually found in more than one of the three.[13][14] However, ο (omicron) is commonly used for stars in both Puppis and Vela. Some authors contend that Lacaille actually assigned a Latin lower case 'o' to this star,[15] while others suggest that ο Velorum should actually be a lower case 'o'.[16] In the Coelum Australe Stelliferum itself, this star is labelled (Latin) o Argus in puppi (Pouppe du Navire in the French edition), while ο Velorum is labelled ο (omicron) Argus (du Navire in the French edition).[17][18]

In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[19] refers to an asterism consisting of ο Puppis, δ Canis Majoris, η Canis Majoris, HD 63032, HD 65456, k Puppis, ε Canis Majoris, κ Canis Majoris and π Puppis. Consequently, ο Puppis itself is known as 弧矢五 (Hú Shǐ wǔ, English: the Fifth Star of Bow and Arrow.)[20]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 Feinstein, A.; Marraco, H. G. (November 1979), "The photometric behavior of Be Stars", Astronomical Journal 84: 1713–1725, doi:10.1086/112600, Bibcode: 1979AJ.....84.1713F. 
  3. ↑ Hiltner, W. A. et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal 157: 313–326, doi:10.1086/150069, Bibcode: 1969ApJ...157..313H. 
  4. ↑ Kharchenko, N. V. et al. (2007), "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations", Astronomische Nachrichten 328 (9): 889–896, doi:10.1002/asna.200710776, Bibcode: 2007AN....328..889K. 
  5. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  6. ↑ 6.0 6.1 6.2 Koubský, P. et al. (September 2012), "o Puppis: another Be+sdO binary?", Astronomy & Astrophysics 545: 4, doi:10.1051/0004-6361/201219679, A121, Bibcode: 2012A&A...545A.121K 
  7. ↑ 7.0 7.1 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, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T. 
  8. ↑ 8.0 8.1 Hohle, M. M. et al. (2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten 331 (4): 349, doi:10.1002/asna.200911355, Bibcode: 2010AN....331..349H. 
  9. ↑ Abt, Helmut A. et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A 
  10. ↑ "omi Pup". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi+Pup. 
  11. ↑ Samus, N. N. et al. (2009), "General Catalogue of Variable Stars", Vizier Online Data Catalog 1, Bibcode: 2009yCat....102025S. 
  12. ↑ Watson, C. L. (2006), "The International Variable Star Index (VSX)", The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25 25: 47, Bibcode: 2006SASS...25...47W. 
  13. ↑ Coelum australe stelliferum .... H L Guerin & L F Delatour. 1763. pp. 7–. https://books.google.com/books?id=LIo_AAAAcAAJ&pg=PP7. 
  14. ↑ Kostjuk, N. D. (2004). "VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)". VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002) 4027. Bibcode: 2004yCat.4027....0K. 
  15. ↑ Wagman, Morton (2003). Lost Stars. McDonald and Woodward. p. 259. ISBN 0-939923-78-5. 
  16. ↑ Hoffleit, D.; Jaschek, C. (1982). "The Bright Star Catalogue". The Bright Star Catalogue. Bibcode: 1982bsc..book.....H. 
  17. ↑ La Caille, Nicolas Louis de. "Coelum Australe Stelliferum". https://www.digitale-sammlungen.de/en/view/bsb10049177?page=195. 
  18. ↑ La Caille, Nicolas Louis de. "Coelum Australe Stelliferum". http://gallica.bnf.fr/ark:/12148/bpt6k35505/f757.vertical. 
  19. ↑ 弧矢 (Hú Shǐ) is westernized into Koo She. R.H. Allen had opinion that Koo She refers to the asterism including δ Velorum and ω Velorum. AEEA opinion is, δ Velorum is member of 天社 (Tiān Shè), meaning Celestial Earth God's Temple asterism and ω Velorum is not member of any asterisms. 天社 (Tiān Shè) is westernized into Tseen She and R.H.Allen used the term Tseen She for Chinese name of η Carinae. See Richard Hinckley Allen: Star Names — Their Lore and Meaning: Argo Navis and (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日.
  20. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日



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