Zeta Phoenicis

Zeta Phoenicis
Observation data
Epoch J2000      Equinox J2000
Constellation Phoenix
Right ascension 01h 08m 23.08s[1]
Declination –55° 14′ 44.7″[1]
Apparent magnitude (V) 3.9 to 4.4
Characteristics
Spectral type B6 V + B9 V
B−V color index –0.12
Variable type Algol
Astrometry
Radial velocity (Rv)+15.4 km/s
Proper motion (μ) RA: 20.87[1] mas/yr
Dec.: 30.64[1] mas/yr
Parallax (π)10.92 ± 0.39[1] mas
Distance300 ± 10 ly
(92 ± 3 pc)
Absolute magnitude (MV)–0.37 / 0.90[2]
Details[2]
ζ Phe A
Mass3.92 M☉
Radius2.85 R☉
Luminosity316 L☉
Surface gravity (log g)4.12 cgs
Temperature14,400 K
ζ Phe B
Mass2.55 M☉
Radius1.85 R☉
Luminosity65 L☉
Surface gravity (log g)4.31 cgs
Temperature12,000 K
Other designations
HR 338, CD–55° 267, CPD–55° 241, HD 6882, SAO 232306, HIP 5348.
Database references
SIMBADdata

Zeta Phoenicis (ζ Phe, ζ Phoenicis) is a B-type main sequence star in the constellation Phoenix. It is visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, it is located some 300 light years (92 parsecs) away.[1]

Zeta Phoenicis is an Algol-type eclipsing binary star. It consists of two stars that orbit each other: when one passes in front of one another, it blocks some of the other star's light. Therefore, its apparent magnitude fluctuates between 3.9 and 4.4 with a period of 1.66977 days (its orbital period).

The system most likely contains four stars: it has two other telescopic components with an apparent magnitude of 7.2 and 8.2 at an angular separation of 0.8 and 6.4 arcseconds from the main pair.[3] The companion that is 6.4 arseconds away is designated Zeta Phoenicis C, and is an A-type[4] or F-type main-sequence star.[5] A preliminary orbit has been determined, with an orbital period of about 210 years, as well as an eccentricity of about 0.35.[6]

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (2007). "HIP 5348". Hipparcos, the New Reduction. Retrieved 2009-12-14.
  2. 1 2 Torres, G.; Andersen, J.; Giménez, A. (February 2010). "Accurate masses and radii of normal stars: modern results and applications". The Astronomy and Astrophysics Review. 18 (1–2): 67–126. Bibcode:2010A&ARv..18...67T. arXiv:0908.2624 Freely accessible. doi:10.1007/s00159-009-0025-1.
  3. ↑ Clausen, J. V.; Gyldenkerne, K.; Grønbech, B. (January 1976). "Four-color photometry of eclipsing binaries. IIIb: Zeta Phoenicis, analysis of light curves and determination of absolute dimensions". Astronomy and Astrophysics. 46: 205–212. Bibcode:1976A&A....46..205C.
  4. ↑ Zasche, P.; Wolf, M.; Hartkopf, W. I.; Svoboda, P.; Uhlař, R.; Liakos, A.; Gazeas, K. (2009). "A Catalog of Visual Double and Multiple Stars With Eclipsing Components". The Astronomical Journal. 138 (2): 664–679. Bibcode:2009AJ....138..664Z. doi:10.1088/0004-6256/138/2/664.
  5. ↑ "zet Phe C". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 28 February 2017.
  6. ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.