HD 120987
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 53m 32.76039s[1] |
| Declination | −35° 39′ 51.3200″[1] |
| Apparent magnitude (V) | 5.565[2] (6.27 / 6.38)[3] |
| Characteristics | |
| Spectral type | F4V (F0V + F1V)[4] |
| U−B color index | -0.03[5] |
| B−V color index | +0.44[5] |
| Astrometry | |
| Radial velocity (Rv) | -8.00 ± 7.40[6] km/s |
| Proper motion (μ) | RA: -83.39[1] mas/yr Dec.: -25.36[1] mas/yr |
| Parallax (π) | 19.13 ± 0.93 mas[1] |
| Distance | 170 ± 8 ly (52 ± 3 pc) |
| Orbit[3] | |
| Period (P) | 373.0 yr |
| Semi-major axis (a) | 1.519″ |
| Eccentricity (e) | 0.775 |
| Inclination (i) | 74.2° |
| Longitude of the node (Ω) | 112.3° |
| Periastron epoch (T) | B 1958.57 |
| Argument of periastron (ω) (secondary) | 90.7° |
| Details | |
| HD 120987 A | |
| Mass | 1.56[7] M☉ |
| HD 120987 B | |
| Mass | 1.53[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 120987 (y Centauri or y Cen) is a star system located in the constellation Centaurus. HD 120987 is a quintuple star system located 50 pc (163 light years) from the Sun. The system has an apparent magnitude of 5.565.[2] Based on the system's parallax, it is located some 172 light-years (52 parsecs) away.[1]
HD 120987 appears to be a single F-type star with the spectral classification F4V, but closer inspection reveals it to be two similar F-type main-sequence stars with spectral classifications of F0V and F1V, respectively.[4] The two orbit each other ever 373 years, and are separated by 1.519 arcseconds while taking a very eccentric orbit.[3]
References
- ^ a b c d e f van Leeuwen, F.; et al. (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.
- ^ a b c "* y Cen". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 19 July 2017.
- ^ a b c "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Retrieved 19 July 2017.
- ^ a b Cvetkovic, Z.; Ninkovic, S. (2010). "On the Component Masses of Visual Binaries". Serbian Astronomical Journal. 180 (180): 71. Bibcode:2010SerAJ.180...71C. doi:10.2298/SAJ1080071C.
- ^ a b Cousins, A. W. J.; Lagerweij, H. C. (1970). "Comparison Stars for Long Period Variables and RY Sagittarii". Monthly Notes of the Astron. Soc. Southern Africa. 29 (7). Bibcode:1970MNSSA..29....7C.
- ^ Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv:0705.0878. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776.
- ^ a b Tokovinin, Andrei (2014). "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal. 147 (4): 87. arXiv:1401.6827. Bibcode:2014AJ....147...87T. doi:10.1088/0004-6256/147/4/87.
 | This binary or multiple star system–related article is a stub. You can help Wikipedia by expanding it. |