| 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−Vcolor 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 | |
| Wurren,HR 338,CD–55° 267,CPD–55° 241,HD 6882,SAO 232306,HIP 5348. | |
| Database references | |
| SIMBAD | data |
Zeta Phoenicis (ζ Phoenicis, abbreviatedZet Phe,ζ Phe) is a multiplestar system in theconstellation ofPhoenix. It is visible to the naked eye. Based uponparallax measurements made by theHipparcosspacecraft, it is located some 300light-years (92parsecs) away.[1]
Zeta Phoenicis A is itself anAlgol-typeeclipsing binary star. It consists of twoB-typemain sequencestars that orbit each other.[3] The larger and brighter (Zeta Phoenicis Aa) is formally namedWurren/ˈwʊrən/.[4] When one passes in front of one another, it blocks some of the other star's light. As a result, itsapparent magnitude fluctuates between 3.9 and 4.4 with a period of 1.6697739 days (itsorbital 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 6.4arcseconds from the main pair.[5] The closer (Zeta Phoenicis B) is anA-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 anF-type main-sequence star with an orbital period of over 5,000 years.[3]
ζ Phoenicis (Latinised toZeta Phoenicis) is the system'sBayer designation. The designations of the three constituents asζ Phoenicis A,B andC, and those ofA's components—ζ Phoenicis Aa andAb—derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiplestar systems, and adopted by theInternational Astronomical Union (IAU).[8]
The system bore the traditional nameWurren in the culture of theWardaman people of theNorthern Territory ofAustralia,[9] meaningchild, but in this context refers to a "Little Fish", a star adjacent toAchernar (Gawalyan = porcupine or echidna) to whom little fish provides water.[10] In 2016, the IAU organized aWorking Group on Star Names (WGSN)[11] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entiremultiple systems.[12] It approved the nameWurren for the component Zeta Phoenicis Aa on 19 November 2017 and it is now so included in the List of IAU-approved Star Names.[4]
InChinese occasioned by adaptation of the Europeansouthern hemisphere constellations into the Chinese system,水委 (Shuǐ Wěi), meaningCrooked Running Water, refers to anasterism consisting of Zeta Phoenicis, Alpha Eridani (Achernar) andEta Phoenicis. Consequently, Zeta Phoenicis itself is known as水委二 (Shuǐ Wěi èr, English:the Second Star of Crooked Running Water).[13]
