Beta Phoenicis

Beta Phoenicis
Observation data
Epoch J2000      Equinox J2000
Constellation Phoenix
Right ascension 01h 06m 05.03952s[1]
Declination −46° 43′ 06.2785″[1]
Apparent magnitude (V) 3.30[2]
(4.10 / 4.19)[3]
Characteristics
Spectral type G8III + G8III:[4]
Astrometry
Proper motion (μ) RA: −80.81[1] mas/yr
Dec.: +34.97[1] mas/yr
Parallax (π)17.63 ± 2.09 mas[5]
Distanceapprox. 190 ly
(approx. 57 pc)
Absolute magnitude (MV)0.29[6]
Orbit[7]
Period (P)170.7±5.0 yr
Semi-major axis (a)0.946±0.016″
Eccentricity (e)0.718±0.016
Inclination (i)144.0±1.5°
Longitude of the node (Ω)126.4±3.5°
Periastron epoch (T)2003.41±0.10
Argument of periastron (ω)
(secondary)		293.5±4.4°
Details
Mass2.7–3[8] M☉
Radius~14/~14[8][a] R☉
Luminosity~100/~100[8] L☉
Temperature5,090[6] K
Rotational velocity (v sin i)11.4±0.6[6] km/s
Other designations
CD−47 324, HD 6595, HIP 5165, HR 322, SAO 215365.[9]
Database references
SIMBADdata

Beta Phoenicis (β Phoenicis, β Phe) is a binary star in the constellation Phoenix. Its apparent magnitude is 3.30,[2] meaning that it can be seen with the naked eye (see Bortle scale).

The distance to Beta Phoenicis is poorly known. The original reduction of the Hipparcos satellite's data yielded a parallax value of 16 milliarcseconds, yet its standard error was larger than the parallax value itself.[10] An individual note in the Hipparcos catalogue provided a more likely parallax of 17.63±2.09 mas, corresponding to a distance of 185±22 light-years,[5] consistent with the expected distance implied by the absolute visual magnitude of a G8 giant.[8] The new reduction of the Hipparcos data gave 0.12 ± 14.62 milliarcseconds, still unusable.[1] The General Catalogue of Trigonometric Parallaxes, an older catalogue of ground-based parallaxes, lists the parallax as 20 ± 16 milliarcseconds, corresponding to about 200 light-years (61 pc).[11]

Beta Phoenicis is a relatively wide visual binary consisting of two G-type giant stars, both with spectral types of G8III.[4] The two orbit each other every 170.7 years and have a relatively eccentric orbit. The stars are separated by almost one arcsecond.[7]

  1. ^ a b c d e Cite error: The named reference vanLeeuwen2007 was invoked but never defined (see the help page).
  2. ^ a b Cite error: The named reference Ducati was invoked but never defined (see the help page).
  3. ^ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 2017-08-01. Retrieved 2017-03-11.
  4. ^ a b Cite error: The named reference Eggleton2008 was invoked but never defined (see the help page).
  5. ^ a b "Hipparcos notes: General notes". vizier.cds.unistra.fr. Retrieved 2024-07-20.
  6. ^ a b c Cite error: The named reference vonEiff2012 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Argyle_et_al_2015 was invoked but never defined (see the help page).
  8. ^ a b c d "Beta Phoenicis". stars.astro.illinois.edu. Retrieved 2024-07-20.
  9. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  10. ^ Perryman, M. A. C.; et al. (April 1997). "The HIPPARCOS Catalogue". Astronomy & Astrophysics. 323: L49–L52. Bibcode:1997A&A...323L..49P.
  11. ^ van Altena, W. F.; Lee, J. T.; Hoffleit, E. D. (1995). The General Catalogue of Trigonometric [Stellar] Parallaxes (4th ed.). New Haven, CT: Yale University Observatory. Bibcode:1995gcts.book.....V.


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