Wikipedia

Omicron Puppis

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.

Omicron Puppis
Location of ο Puppis (circled)
Observation data
Epoch J2000.0      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 mas[1]
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

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]

A light curve for Omicron Puppis, plotted from TESS data.[11] The 2.0651 day period[12] is shown in red.

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.[13] The International Variable Star Index classifies it as a Lambda Eridani variable.[12]

Naming

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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 (except for omicron) each Greek letter is found in only one of the three.[14][15] However, ο (omicron) is now commonly used for two stars, one each in Vela and Puppis. 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).[16][17][18] Some later authors state the reverse, that Lacaille actually assigned omicron to ο Puppis and Latin lower case 'o' to ο Velorum.[19] Modern catalogs and atlases generally use omicron for both stars.

In Chinese, 弧矢 (Hú Shǐ), meaning Bow and Arrow,[20] 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.)[21]

References

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  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d Feinstein, A.; Marraco, H. G. (November 1979), "The photometric behavior of Be Stars", Astronomical Journal, 84: 1713–1725, Bibcode:1979AJ.....84.1713F, doi:10.1086/112600.
  3. ^ Hiltner, W. A.; et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal, 157: 313–326, Bibcode:1969ApJ...157..313H, doi:10.1086/150069.
  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, arXiv:0705.0878, Bibcode:2007AN....328..889K, doi:10.1002/asna.200710776, S2CID 119323941.
  5. ^ 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.
  6. ^ a b c Koubský, P.; et al. (September 2012), "o Puppis: another Be+sdO binary?", Astronomy & Astrophysics, 545: 4, Bibcode:2012A&A...545A.121K, doi:10.1051/0004-6361/201219679, A121
  7. ^ a b 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, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  8. ^ a b Hohle, M. M.; et al. (2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  9. ^ Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590
  10. ^ "omi Pup". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-07-19.{{cite web}}: CS1 maint: postscript (link)
  11. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 28 September 2024.
  12. ^ a b 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. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009), "General Catalogue of Variable Stars", Vizier Online Data Catalog, 1, Bibcode:2009yCat....102025S.
  14. ^ Coelum australe stelliferum ... H L Guerin & L F Delatour. 1763. pp. 7–.
  15. ^ 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.
  16. ^ La Caille, Nicolas Louis de. "Coelum Australe Stelliferum". Retrieved 2017-07-21.
  17. ^ La Caille, Nicolas Louis de. "Coelum Australe Stelliferum". Retrieved 2017-07-21.
  18. ^ Wagman, Morton (2003). Lost Stars. McDonald and Woodward. p. 259. ISBN 0-939923-78-5.
  19. ^ Hoffleit, D.; Jaschek, C. (1982). "The Bright Star Catalogue". The Bright Star Catalogue. Bibcode:1982bsc..book.....H.
  20. ^ 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 Archived 2012-02-04 at the Wayback Machine.
  21. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日 Archived 2012-02-04 at the Wayback Machine
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