Astronomy:Beta Phoenicis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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: −33.6±2.4[5] mas/yr Dec.: +15.0±1.6[5] mas/yr |
| Parallax (π) | 17.63 ± 2.09[5] mas |
| Distance | approx. 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[8] | |
| β Phe A | |
| Mass | 2.7–3 M☉ |
| Radius | 14[lower-alpha 1] R☉ |
| Luminosity | 100 L☉ |
| Temperature | 4,950 K |
| β Phe B | |
| Mass | 2.7–3 M☉ |
| Radius | 14[lower-alpha 1] R☉ |
| Luminosity | 100 L☉ |
| Temperature | 4,950 K |
| 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).
This is a relatively wide visual binary consisting of two G-type red 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] The presence of similar-brightness stars at such separation has made parallax measurements difficult, often with margins of error higher than the standard value, since these measurements assume the star to be single. Based on the typical absolute magnitude of a G-type giant and the apparent magnitude of the stars, the distance has been estimated at 200 light-years.[8] Despite this, a reanalysis of the (uncertain) Hipparcos data, taking in account the binarity of Beta Phoenicis, found a more likely parallax of 17.63±2.09 mas, corresponding to a distance of 185±22 light-years.[5]
Notes
- ↑ 1.0 1.1 Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
- .
References
- ↑ 1.0 1.1 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237. Bibcode: 2002yCat.2237....0D.
- ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6.
- ↑ 4.0 4.1 Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E.
- ↑ 5.0 5.1 5.2 "Hipparcos notes: General notes". https://vizier.cds.unistra.fr/viz-bin/VizieR-6?-out.form=+H&-source=I/239/hd_notes,I/239/hg_notes,I/239/hp_notes&HIP=5165.
- ↑ Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012). "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?". Astronomy & Astrophysics 542: A116. doi:10.1051/0004-6361/201118724. Bibcode: 2012A&A...542A.116A.
- ↑ 7.0 7.1 Argyle, R. W. et al. (May 2015). "Micrometric measures and orbits of southern visual double stars". Astronomische Nachrichten 336 (4): 378–387. doi:10.1002/asna.201412166. Bibcode: 2015AN....336..378A.
- ↑ 8.0 8.1 "Beta Phoenicis". http://stars.astro.illinois.edu/sow/betaphe.html.
- ↑ "* bet Phe". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+bet+Phe.
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