Zeta Persei

Zeta Persei
Diagram showing star positions and boundaries of the Perseus constellation and its surroundings


Location of ζ Persei (circled)

Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 54m 07.92248s[1]
Declination +31° 53′ 01.0812″[1]
Apparent magnitude (V) 2.86[2]
Characteristics
Spectral type B1 Ib[3]
U−B color index –0.72[2]
B−V color index +0.10[2]
Astrometry
Radial velocity (Rv)20.1 ± 1.2[4] km/s
Proper motion (μ) RA: +5.77[1] mas/yr
Dec.: –9.92[1] mas/yr
Parallax (π)4.34 ± 0.19[1] mas
Distance750 ± 30 ly
(230 ± 10 pc)
Details
Mass14.5 ± 1.9[5] M☉
Radius26–27[6] R☉
Luminosity47,039[5] L☉
Temperature20,800[5] K
Rotation2.9–17.3 days
Rotational velocity (v sin i)40[3] km/s
Age12.6 ± 1.5[7] Myr
Other designations
44 Per, FK5 144, HD 24398, HIP 18246, HR 1203, SAO 56799.[8]

Zeta Persei (ζ Per, ζ Persei) is a star in the northern constellation of Perseus. With an apparent visual magnitude of 2.9,[2] it can be readily seen with the naked eye. Parallax measurements place it at a distance of about 750 light-years (230 parsecs) from Earth.[1]

This is a lower luminosity supergiant star with a stellar classification of B1 Ib.[3] This is an enormous star, with an estimated 26–27[6] times the Sun's radius and 13–16 times the Sun's mass.[6] It has about 47,000 times the luminosity of the Sun and it is radiating this energy at an effective temperature of 20,800 K,[5] giving it the blue-white hue of a B-type star.[9] The spectrum displays anomalously high levels of carbon.[10] Zeta Persei has a strong stellar wind that is expelling 0.23 × 10−6 times the mass of the Sun per year, or the equivalent of the Sun's mass every 4.3 million years.[11]

Zeta Persei has a 9th magnitude companion at an angular separation of 12.9 arcseconds. The two stars have the same proper motion, so they may be physically associated. If so, they are separated by at least 4,000 Astronomical Units.[12] Zeta Persei is a confirmed member of the Perseus OB2 association (Per OB2), also called the Zeta Persei association, which is a moving group of stars that includes 17 massive, high luminosity members with spectral types of O or B, giving them a blue hue. These stars have a similar trajectory through space,[4] suggesting they originated in the same molecular cloud and are about the same age.[13]

See also

Ambiguity

Some sources, including Starry Night (planetarium software), an atlas,[14] and a web site[15] attribute the name 'Atik' to Zeta Persei instead of nearby Omicron Persei.

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357
  2. 1 2 3 4 Lutz, T. E.; Lutz, J. H. (June 1977), "Spectral classification and UBV photometry of bright visual double stars", Astronomical Journal, 82: 431–434, Bibcode:1977AJ.....82..431L, doi:10.1086/112066
  3. 1 2 3 Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590
  4. 1 2 Steenbrugge, K. C.; et al. (May 2003), "Radial velocities of early-type stars in the Perseus OB2 association", Astronomy and Astrophysics, 402: 587–605, arXiv:astro-ph/0302428Freely accessible, Bibcode:2003A&A...402..587S, doi:10.1051/0004-6361:20030277
  5. 1 2 3 4 Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335Freely accessible, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355
  6. 1 2 3 Pasinetti-Fracassini, L. E.; et al. (February 2001) [November 2000 (arXiv)], "Catalogue of Stellar Diameters (CADARS)", Astronomy and Astrophysics, 367: 521–524, arXiv:astro-ph/0012289Freely accessible, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451
  7. ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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:1007.4883Freely accessible, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x
  8. ↑ "zet Per -- Variable Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-12
  9. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16
  10. ↑ Jaschek, M.; Jaschek, C. (December 1974), "The CNO stars", Astronomy and Astrophysics, 36 (3): 401–408, Bibcode:1974A&A....36..401J
  11. ↑ Morel, T.; et al. (June 2004), "Large-scale wind structures in OB supergiants: a search for rotationally modulated Hα variability", Monthly Notices of the Royal Astronomical Society, 351 (2): 552–568, arXiv:astro-ph/0403155Freely accessible, Bibcode:2004MNRAS.351..552M, doi:10.1111/j.1365-2966.2004.07799.x
  12. ↑ Burnham, Robert (1978), Burnham's celestial handbook: an observer's guide to the universe beyond the solar system, Dover books explaining science, 3 (2nd ed.), Courier Dover Publications, p. 1422, ISBN 0-486-23673-0
  13. ↑ de Zeeuw, P. T.; et al. (January 1999), "A HIPPARCOS Census of the Nearby OB Associations", The Astronomical Journal, 117 (1): 354–399, arXiv:astro-ph/9809227Freely accessible, Bibcode:1999AJ....117..354D, doi:10.1086/300682
  14. ↑ Mullaney, James & Tirion, Wil (2009). The Cambridge Double Star Atlas, Chart 7. University Press, Cambridge. ISBN 978-0-521-49343-7.
  15. ↑ Your Sky Object Catalogue: Named Stars
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