en 3 Boötis

3 Boötis
Observation data; Epoch J2000 Equinox J2000
Constellation	Boötes
Right ascension	13h 46m 43.32359s
Declination	+25° 42′ 08.0548″
Apparent magnitude (V)	5.97
Characteristics
Evolutionary stage	HG + MS
Spectral type	kA9hF6mF6 (A7 V: + G5 III: or F2p + G0 IV)
B−V color index	0.523±0.004
Astrometry
Radial velocity (Rv)	11.9±0.9 km/s
Proper motion (μ)	RA: −18.564 mas/yr ; Dec.: −59.093 mas/yr
Parallax (π)	10.5064 ± 0.0425 mas
Distance	310 ± 1 ly ; (95.2 ± 0.4 pc)
Absolute magnitude (MV)	1.21
Orbit
Period (P)	36.006 d
Eccentricity (e)	0.543±0.002
Inclination (i)	74.5±2.0°
Semi-amplitude (K1); (primary)	52.30±0.19 km/s
Semi-amplitude (K2); (secondary)	59.0±0.6 km/s
Details
3 Boo A
Mass	1.8 M☉
Radius	3.7 R☉
Temperature	5,848 K
3 Boo A
Mass	1.6 M☉
Radius	2.6 R☉
Temperature	6,745 K
Age	1.5 Gyr
Other designations
	3 Boo, BD+26°2494, FK5 1358, HD 120064, HIP 67239, HR 5182, SAO 82993
Database references
SIMBAD	data

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]

References

^ ^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.
^ ^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, S2CID 119257644.
^ ^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, arXiv:1611.05041, Bibcode:2017MNRAS.468.3533E, doi:10.1093/mnras/stx598, S2CID 119476544.
^ 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, S2CID 122811461.
^ 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.
^ ^a ^b "3 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-10.