| 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
[2] or +4.86
[3] (5.00 + 7.74 + 7.84 + 8.44) [4] |
| Characteristics | |
| Spectral type | F6 IV + G5 V + K2V + ? [5] |
| B−V color index | 0.48 [6] |
| Astrometry | |
| Radial velocity (Rv) | +7.7±1.7 [2] km/s |
| Proper motion (μ) |
RA: +412.11
[1]
mas/
yr Dec.: +127.74 [1] mas/ yr |
| Parallax (π) | 47.72 ± 0.41 mas [1] |
| Distance | 68.3 ± 0.6
ly (21.0 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.50 [6] |
| Orbit [7] | |
| 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 [8] M☉ |
| Temperature | 6,366 [6] K |
| Rotational velocity (v sin i) | 61.1±3.1 [6] km/s |
| κ Tuc B | |
| Mass | 0.85 [8] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kappa Tucanae, Latinised from, κ Tucanae, is a quadruple [5] star system in the southern constellation Tucana. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of either +4.25 [2] or +4.86, [3] depending on the source. The system is located approximately 68 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8 km/s. [2]
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 +5.0. 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. [7]
The other binary pair, the magnitude +7.8 C, and the magnitude +8.4 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
- ^ a b c d e 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, S2CID 18759600.
- ^ a b c d Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971, Bibcode: 2012AstL...38..331A, doi: 10.1134/S1063773712050015, S2CID 119257644.
- ^ a b Hoffleit, D.; Warren, Jr., W. H. (1991), The Bright Star Catalogue (5th Revised ed.), retrieved 2019-09-16.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920.
- ^ a b 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, S2CID 14878976.
- ^ a b c d 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, arXiv: 1204.2459, Bibcode: 2012A&A...542A.116A, doi: 10.1051/0004-6361/201118724, S2CID 53666672.
- ^ a b "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 2017-08-01. Retrieved 2017-07-01.
- ^ a b 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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| 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
[2] or +4.86
[3] (5.00 + 7.74 + 7.84 + 8.44) [4] |
| Characteristics | |
| Spectral type | F6 IV + G5 V + K2V + ? [5] |
| B−V color index | 0.48 [6] |
| Astrometry | |
| Radial velocity (Rv) | +7.7±1.7 [2] km/s |
| Proper motion (μ) |
RA: +412.11
[1]
mas/
yr Dec.: +127.74 [1] mas/ yr |
| Parallax (π) | 47.72 ± 0.41 mas [1] |
| Distance | 68.3 ± 0.6
ly (21.0 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.50 [6] |
| Orbit [7] | |
| 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 [8] M☉ |
| Temperature | 6,366 [6] K |
| Rotational velocity (v sin i) | 61.1±3.1 [6] km/s |
| κ Tuc B | |
| Mass | 0.85 [8] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kappa Tucanae, Latinised from, κ Tucanae, is a quadruple [5] star system in the southern constellation Tucana. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of either +4.25 [2] or +4.86, [3] depending on the source. The system is located approximately 68 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +8 km/s. [2]
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 +5.0. 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. [7]
The other binary pair, the magnitude +7.8 C, and the magnitude +8.4 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
- ^ a b c d e 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, S2CID 18759600.
- ^ a b c d Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971, Bibcode: 2012AstL...38..331A, doi: 10.1134/S1063773712050015, S2CID 119257644.
- ^ a b Hoffleit, D.; Warren, Jr., W. H. (1991), The Bright Star Catalogue (5th Revised ed.), retrieved 2019-09-16.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920.
- ^ a b 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, S2CID 14878976.
- ^ a b c d 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, arXiv: 1204.2459, Bibcode: 2012A&A...542A.116A, doi: 10.1051/0004-6361/201118724, S2CID 53666672.
- ^ a b "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 2017-08-01. Retrieved 2017-07-01.
- ^ a b 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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Star clusters |
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| Galaxies |
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