Back Zeta Phoenicis AST Zeta Phoenicis BS Zeta Phoenicis German Zeta Phoenicis Spanish زتا ققنوس Persian Zeta Phoenicis Finnish Zeta Phoenicis French Zeta Phoenicis Italian ほうおう座ゼータ星 Japanese Zeta Phoenicis Polish
| 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 + B8 V[2] |
| 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 mas[1] |
| Distance | 300 ± 10 ly (92 ± 3 pc) |
| Absolute magnitude (MV) | –1.49 / 0.19[2] |
| Orbit[2] | |
| Period (P) | 1.6697739 d |
| Semi-major axis (a) | 11.022 ± 0.048 R☉ |
| Eccentricity (e) | 0.0116 ± 0.0024 |
| Inclination (i) | 89.14 ± 0.11° |
| Argument of periastron (ω) (secondary) | 307 ± 12° |
| Semi-amplitude (K1) (primary) | 131.4 ± 0.7 km/s |
| Semi-amplitude (K2) (secondary) | 202.5 ± 1.3 km/s |
| Details[2] | |
| ζ Phe Aa | |
| Mass | 3.908 M☉ |
| Radius | 2.835 R☉ |
| Luminosity | 309 L☉ |
| Surface gravity (log g) | 4.1249 cgs |
| Temperature | 14,400 K |
| Rotational velocity (v sin i) | 85.89 km/s |
| ζ Phe Ab | |
| Mass | 2.536 M☉ |
| Radius | 1.885 R☉ |
| Luminosity | 66 L☉ |
| Surface gravity (log g) | 4.2917 cgs |
| Temperature | 12,000 K |
| Rotational velocity (v sin i) | 57.11 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Zeta Phoenicis (ζ Phoenicis, abbreviated Zet Phe, ζ Phe) is a multiple star system in the constellation of 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 A is itself an Algol-type eclipsing binary star. It consists of two B-type main sequence stars that orbit each other.[3] The larger and brighter (Zeta Phoenicis Aa) is formally named Wurren /ˈwʊrən/.[4] When one passes in front of one another, it blocks some of the other star's light. As a result, its apparent magnitude fluctuates between 3.9 and 4.4 with a period of 1.6697739 days (its orbital period).
The system most likely contains four stars with two other telescopic components of apparent magnitude 7.2 and 8.2 at angular separations of 0.8 and 6.4 arcseconds from the main pair.[5] The closer (Zeta Phoenicis B) is an A-type main-sequence star[6] with an orbital period around the main pair of about 210 years, as well as an eccentricity of about 0.35.[7] The further (Zeta Phoenicis C) is an F-type main-sequence star with an orbital period of over 5,000 years.[3]
- ^ a b c d e f Cite error: The named reference
hipparcoswas invoked but never defined (see the help page). - ^ a b c d Cite error: The named reference
Southworthwas invoked but never defined (see the help page). - ^ a b Kaler, Jim. "Zeta Phoenicis". Department of Astronomy, University of Illinois. Retrieved 2017-12-18.
- ^ "Naming Stars". IAU.org. Retrieved 16 December 2017.
- ^ Cite error: The named reference
aaa46_205was invoked but never defined (see the help page). - ^ 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. arXiv:0907.5172. Bibcode:2009AJ....138..664Z. doi:10.1088/0004-6256/138/2/664. S2CID 17089387.
- ^ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 2017-08-01. Retrieved 2017-02-28.