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HD 120987

From Wikipedia, the free encyclopedia
Binary star system in the constellation Centaurus
This article is about y Centauri. Not to be confused withγ (gamma) Centauri. For the variable star, seeHIP 70969.
HD 120987
Observation data
EpochJ2000      EquinoxJ2000
ConstellationCentaurus
Right ascension13h 53m 32.76039s[1]
Declination−35° 39′ 51.3200″[1]
Apparent magnitude (V)5.565[2]
(6.27 / 6.38)[3]
Characteristics
Spectral typeF4V (F0V + F1V)[4]
U−Bcolor index-0.03[5]
B−Vcolor 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]
Distance170 ± 8 ly
(52 ± 3 pc)
Orbit[3]
Period (P)373.0yr
Semi-major axis (a)1.519″
Eccentricity (e)0.775
Inclination (i)74.2°
Longitude of the node (Ω)112.3°
Periastronepoch (T)B 1958.57
Argument of periastron (ω)
(secondary)
90.7°
Details
HD 120987 A
Mass1.56[7] M
HD 120987 B
Mass1.53[7] M
Other designations
CD−35° 9090,HD 120987,HIP 67819,HR 5222,SAO 204955[2]
Database references
SIMBADdata

HD 120987 (y Centauri ory Cen) is astar system located in theconstellationCentaurus. HD 120987 is a quintuplestar system located 50 pc (163light years) from theSun. The system has an apparent magnitude of 5.565.[2] Based on the system'sparallax, it is located some 172 light-years (52 parsecs) away.[1]

HD 120987 appears to be a singleF-type star with thespectral classification F4V, but closer inspection reveals it to be two similarF-type main-sequence stars with spectral classifications of F0V and F1V, respectively.[4] The two orbit each other every 373 years, and are separated by 1.519 arcseconds while taking a veryeccentric orbit.[3]

References

[edit]
  1. ^abcdefvan 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.S2CID 18759600.
  2. ^abc"* y Cen".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved19 July 2017.
  3. ^abc"Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived fromthe original on 1 August 2017. Retrieved19 July 2017.
  4. ^abCvetkovic, 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.
  5. ^abCousins, 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.
  6. ^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.S2CID 119323941.
  7. ^abTokovinin, 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.S2CID 56066740.
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