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HD 158614
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Ophiuchus
Right ascension	17h 30m 23.79699s
Declination	−01° 03′ 46.4882″
Apparent magnitude (V)	+5.31 (6.02 + 5.93)
Characteristics
Evolutionary stage	Subgiant
Spectral type	G9IV-V + G9IV-V
B−V color index	+0.715±0.013
Astrometry
Radial velocity (Rv)	−76.98±0.05 km/s
Proper motion (μ)	RA: −127.77 mas/yr ; Dec.: −168.61 mas/yr
Parallax (π)	61.19 ± 0.68 mas
Distance	53.3 ± 0.6 ly ; (16.3 ± 0.2 pc)
Absolute magnitude (MV)	4.24
Orbit
Period (P)	46.34±0.021 yr
Semi-major axis (a)	977.±3.3 mas
Eccentricity (e)	0.168±0.0025
Inclination (i)	99.1±0.11°
Longitude of the node (Ω)	332.3±0.13°
Periastron epoch (T)	1870.0±0.16 Byr
Argument of periastron (ω); (secondary)	148.±1.3°
Details
A
Mass	0.963±0.005 M☉
Radius	1.7 R☉
Luminosity	2.5 L☉
Surface gravity (log g)	4.00 cgs
Temperature	5,500±150 K
Age	12.3 Gyr
B
Mass	0.951±0.005 M☉
Other designations
	STF 2173, BD−00°3300, GJ 678, HIP 85667, HR 6516, SAO 141702, WDS J17304-0104
Database references
SIMBAD	data

HD 158614 is a visual binary star system in the equatorial constellation of Ophiuchus. The system is visible to the naked eye with a combined apparent visual magnitude of +5.31.^[2] It is located at a distance of 53.3 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −77 km/s^[5] and is predicted to come to within 11.0 light-years in around 196,000 years.^[9] The system has been included as a candidate member of the Zeta Herculis moving group.^[10] However, chemical abundances appear to rule that out.^[11]

The pair were found to be a double star by F. G. W. Struve in 1827 and given the catalogue identifier Σ 2173 (now STF 2173). Since then it has completed multiple orbits,^[12] yielding orbital elements showing a period of 46.3 years and an eccentricity of 0.17.^[3] The two components have similar spectra that match a stellar classification of G9IV-V.^[3] They show almost no luminosity variation; one of the pair appears to vary by 0.002 in magnitude.^[4] Both components have a slightly lower mass than the Sun: 96% and 95%, respectively.^[6] The system is estimated to be 12.3 billion years old.^[7]

This binary was included in a search for brown dwarfs that turned up no large companions.^{[citation needed]}

References

^ ^a ^b ^c ^d ^e van Leeuwen, F. (November 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 ^e ^f Malagnini, M. L.; Morossi, C. (November 1990). "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars". Astronomy and Astrophysics Supplement Series. 85 (3): 1015–1019. Bibcode:1990A&AS...85.1015M.
^ ^a ^b ^c ^d ^e Pourbaix, D. (2000). "Resolved double-lined spectroscopic binaries: A neglected source of hypothesis-free parallaxes and stellar masses". Astronomy and Astrophysics Supplement Series. 145 (2): 215–222. Bibcode:2000A&AS..145..215P. doi:10.1051/aas:2000237.
^ ^a ^b Lockwood, G. W. (1998). Balasubramaniam, K. S.; Harvey, Jack; Rabin, D. (eds.). "Luminosity and Chromospheric Variations of Solar Analog Stars". Synoptic Solar Physics -- 18th NSO/Sacramento Peak Summer Workshop Held at Sunspot; New Mexico 8-12 September 1997. ASP Conference Series. 140: 261. Bibcode:1998ASPC..140..261L.
^ ^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 ^c Andrade, Manuel (October 2019). "Colour-dependent accurate modelling of dynamical parallaxes and masses of visual binaries. Application to the VB+SB2 systems with definitive orbits". Astronomy & Astrophysics. 630: 11. Bibcode:2019A&A...630A..96A. doi:10.1051/0004-6361/201936199. A96.
^ ^a ^b Casagrande, L.; et al. (2011). "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey". Astronomy & Astrophysics. 530 (A138): 21. arXiv:1103.4651. Bibcode:2011A&A...530A.138C. doi:10.1051/0004-6361/201016276. S2CID 56118016.
^ "HD 158614". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-20.
^ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35.
^ Porto de Mello, G. F.; da Silva, L. (1991). "On the physical existence of the Zeta HER moving group - A detailed analysis of Phi exp 2 Pavonis". Astronomical Journal. 102: 1816–1825. Bibcode:1991AJ....102.1816P. doi:10.1086/116006.
^ Ferreira, Letícia D.; et al. (March 2010). "On the Physical Existence of the Zeta Reticuli Moving Group: A Chemical Composition Analysis". Proceedings of the International Astronomical Union. 265: 360–361. Bibcode:2010IAUS..265..360F. doi:10.1017/S174392131000092X.
^ Batten, A. H.; et al. (March 1991). "The Binary System Sigma 2173". Publications of the Astronomical Society of the Pacific. 103: 294. Bibcode:1991PASP..103..294B. doi:10.1086/132818. S2CID 123341219.