Kappa Tucanae
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Tucana |
Right ascension | 01h 15m 46.16226s[1] |
Declination | −68° 52′ 33.3356″[1] |
Apparent magnitude (V) | +4.25 (5.00 / 7.74)[2] |
Characteristics | |
Spectral type | F6 IV + G5 V + K2V + ?[3] |
B−V color index | 0.48[4] |
Astrometry | |
Proper motion (μ) | RA: +412.11[1] mas/yr Dec.: +127.74[1] mas/yr |
Parallax (π) | 47.72 ± 0.41[1] mas |
Distance | 68.3 ± 0.6 ly (21.0 ± 0.2 pc) |
Absolute magnitude (MV) | 3.50[4] |
Orbit[2] | |
Period (P) | 857.0 yr |
Semi-major axis (a) | 5.960″ |
Eccentricity (e) | 0.384 |
Inclination (i) | 127.1° |
Longitude of the node (Ω) | 10.3° |
Periastron epoch (T) | 1763.50 |
Argument of periastron (ω) (secondary) | 284.9° |
Details | |
κ Tuc A | |
Mass | 1.37[5] M☉ |
Temperature | 6,366[4] K |
Rotational velocity (v sin i) | ±3.1 61.1[4] km/s |
κ Tuc B | |
Mass | 0.85[5] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
Kappa Tucanae (κ Tuc, κ Tucanae) is a quadruple[3] star system in the constellation Tucana. It is approximately 66.6 light years from Earth and the combined apparent magnitude of the system is +4.25.
The system consists of two binary pairs separated by 5.3 arcminutes. The brightest star, Kappa Tucanae A, is a yellow-white F-type subgiant with an apparent magnitude of +5.1. Its binary companion, Kappa Tucanae B, has a magnitude of 7.74 and is located about 6″ away from the primary. It completes an orbit around the primary every 857 years.[2]
The other binary pair, the magnitude +7.8 C, and the magnitude +8.2 D, are closer to one another, at 1.12 arcseconds, or at least 23 astronomical units. They orbit each other once every 86.2 years.
References
- 1 2 3 4 5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
- 1 2 3 "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Retrieved 2017-07-01.
- 1 2 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.
- 1 2 3 4 Ammler-von Eiff, M.; Reiners, A. (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, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724.
- 1 2 Tokovinin, A.; Kiyaeva, O. (2015). "Eccentricity distribution of wide binaries". Monthly Notices of the Royal Astronomical Society. 456 (2): 2070. arXiv:1512.00278. Bibcode:2016MNRAS.456.2070T. doi:10.1093/mnras/stv2825.
- ↑ "kap Tuc -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-04-21.
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