3 Boötis

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3 Boötis
Observation data
Epoch J2000      Equinox J2000
Constellation Cepheus
Right ascension  13h 46m 43.32359s[1]
Declination +25° 42′ 08.0548″[1]
Apparent magnitude (V) 5.97[2]
Evolutionary stage HG + MS[3]
Spectral type kA9hF6mF6[4] (A7 V: + G5 III:[5] or F2p + G0 IV[3])
B−V color index 0.523±0.004[2]
Radial velocity (Rv)11.9±0.9[2] km/s
Proper motion (μ) RA: −18.564[1] mas/yr
Dec.: −59.093[1] mas/yr
Parallax (π)10.5064 ± 0.0425[1] mas
Distance310 ± 1 ly
(95.2 ± 0.4 pc)
Absolute magnitude (MV)1.21[2]
Period (P)36.006 d
Eccentricity (e)0.543±0.002
Inclination (i)74.5±2.0°
Semi-amplitude (K1)
52.30±0.19 km/s
Semi-amplitude (K2)
59.0±0.6 km/s
3 Boo A
Mass1.8[3] M
Radius3.7[3] R
Temperature5,848[3] K
3 Boo A
Mass1.6[3] M
Radius2.6[3] R
Temperature6,745[3] K
Age1.5[3] Gyr
Other designations
3 Boo, BD+26°2494, FK5 1358, HD 120064, HIP 67239, HR 5182, SAO 82993[6]
Database references

3 Boötis is a close binary star system in the northern constellation of Boötes,[6] located 310 light years away from the Sun based upon parallax.[1] It can be viewed with the naked eye in excellent seeing conditions as a dim star with an apparent visual magnitude of 5.97.[2] The system is moving further from the Earth with a heliocentric radial velocity of 12 km/s.[2]

This is a double-lined spectroscopic binary system with an orbital period of 36 days and an eccentricity of 0.543. The orbital plane is inclined 74.5° and the system does not form an eclipsing binary. The primary component is an evolving star currently in the Hertzsprung gap, its companion is a main sequence star. Both members have more mass than the Sun and they are around 1.5 billion years old.[3]


  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d e f 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.
  3. ^ a b c d e f g h i j k Eggleton, Peter P.; Yakut, Kadri (July 2017), "Models for 60 double-lined binaries containing giants", Monthly Notices of the Royal Astronomical Society, 468 (3): 3533−3556, Bibcode:2017MNRAS.468.3533E, doi:10.1093/mnras/stx598.
  4. ^ Abt, Helmut A. (January 2009), "MK Classifications of Spectroscopic Binaries", The Astrophysical Journal Supplement, 180 (1): 117–118, Bibcode:2009ApJS..180..117A, doi:10.1088/0067-0049/180/1/117.
  5. ^ Cowley, A. P.; Bidelman, W. P. (February 1979), "MK spectral types for some F and G stars", Publications of the Astronomical Society of the Pacific, 91: 83–86, Bibcode:1979PASP...91...83C, doi:10.1086/130446.
  6. ^ a b "3 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-10.

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