Zeta Canis Majoris

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Not to be confused with Z Canis Majoris.
Zeta Canis Majoris
Location of ζ Canis Majoris (circled)
Observation data
J2000.0
Constellation Canis Major
Right ascension 06h 20m 18.79204s[1]
Declination –30° 03′ 48.1202″[1]
Apparent magnitude (V) +3.025[2]
Characteristics
Spectral type B2.5 V[3]
U−B color index –0.71[2]
B−V color index –0.195[2]
Variable type Suspected β Cep[4]
Distance
362 ± 5 ly
(111 ± 2 pc)
Absolute magnitude (MV)−2.21[6]
Semi-amplitude
(K1)
(primary)		13.5 km/s
Details
Myr
HR 2282, SAO 196698[13]
Database references
SIMBADdata

Zeta Canis Majoris, or ζ Canis Majoris, also named Furud

apparent visual magnitude of +3.0,[2] making it one of the brighter stars in the constellation and hence readily visible to the naked eye. Parallax measurements from the Hipparcos mission yield a distance estimate of around 362 ly (111 pc) from the Sun.[1] It is drifting further away with a radial velocity of +32 km/s.[5]

Name

ζ Canis Majoris, Latinized from Zeta Canis Majoris, is the star's Bayer designation assigned by the German astronomer Johann Bayer in 1603.

The traditional name Furud or Phurud derives from the

Arabian astronomers attempted to identify the name with particular stars, principally in the modern constellations Centaurus and Colomba. The stars of Colomba were assigned to Canis Majoris in the Almagest, leading to more recent assignment of the name for Zeta Canis Majoris.[15]

Al Sufi referred to these stars as ألأغربة al-ʼaghribah "the ravens".[16]

In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[17] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[18] included a table of the first two batches of names approved by the WGSN; which included Furud for this star.

Properties

The binary nature of this system was first noted by

spectrum of the primary caused by the Doppler effect. The pair orbit around their common center of mass once every 675 days with an eccentricity of 0.57.[8]

The primary component is a large star with nearly four

B-type main sequence star that is generating energy through the nuclear fusion of hydrogen at its core. The star is emitting 3,603[11] times the luminosity of the Sun and is a suspected Beta Cephei variable.[4] This energy is being radiated from its outer envelope at an effective temperature of about 18,700 K,[11] giving it the blue-white hue of a B-type star.[21] It is relatively young for a star, with an estimated age of 32 million years.[9]

Zeta Canis Majoris is located close to the

solar antapex
.

References

  1. ^
    S2CID 18759600
  2. ^
    Bibcode:1972MNSSA..31...69C
  3. ^
    Bibcode:1982mcts.book.....H
  4. ^
    hdl:2066/36162
  5. ^
    Bibcode:1967IAUS...30...57E
  6. S2CID 119257644
    .
  7. S2CID 119387088
    .
  8. ^
    doi:10.1086/431207
  9. ^
    S2CID 118629873
  10. ^
    doi:10.1093/mnras/189.3.601
  11. ^
    S2CID 111387483
  12. doi:10.1086/340590
  13. ^ "zet CMa -- Cepheid variable Star", SIMBAD Astronomical Object Database, Centre de Données astronomiques de Strasbourg, retrieved 2012-02-15
  14. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  15. ISBN 978-1-931559-44-7
    .
  16. ISBN 0-486-21079-0
    , retrieved 2010-12-12
  17. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  18. ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  19. doi:10.1086/141645
    .
  20. doi:10.1086/141699
    .
  21. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16

External links

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