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) | 6.177 ± 1.509 mas [5] |
Distance | approx. 500
ly (approx. 160 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 | |
Mass | ~2.5/~2.5 M☉ |
Luminosity | ~100/~100 L☉ |
Temperature | 5,090 [6] K |
Rotational velocity (v sin i) | 11.4±0.6 [6] km/s |
Other designations | |
Database references | |
SIMBAD | data |
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. [9] 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). [10] Kervella et al. (2019) give a parallax of 6.177±1.509 mas based on Gaia DR2 data, which gives a distance of 162 parsecs (530 ly) for this star. [5]
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]
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) | 6.177 ± 1.509 mas [5] |
Distance | approx. 500
ly (approx. 160 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 | |
Mass | ~2.5/~2.5 M☉ |
Luminosity | ~100/~100 L☉ |
Temperature | 5,090 [6] K |
Rotational velocity (v sin i) | 11.4±0.6 [6] km/s |
Other designations | |
Database references | |
SIMBAD | data |
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. [9] 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). [10] Kervella et al. (2019) give a parallax of 6.177±1.509 mas based on Gaia DR2 data, which gives a distance of 162 parsecs (530 ly) for this star. [5]
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]