Astronomy:HD 158614
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Ophiuchus |
| Right ascension | 17h 30m 23.79699s[1] |
| Declination | −01° 03′ 46.4882″[1] |
| Apparent magnitude (V) | +5.31[2] (6.02 + 5.93)[3] |
| Characteristics | |
| Evolutionary stage | Subgiant[4] |
| Spectral type | G9IV-V + G9IV-V[3] |
| B−V color index | +0.715±0.013[5] |
| Astrometry | |
| Radial velocity (Rv) | −76.98±0.05[5] km/s |
| Proper motion (μ) | RA: −127.77[1] mas/yr Dec.: −168.61[1] mas/yr |
| Parallax (π) | 61.19 ± 0.68[1] mas |
| Distance | 53.3 ± 0.6 ly (16.3 ± 0.2 pc) |
| Absolute magnitude (MV) | 4.24[5] |
| Orbit[3] | |
| 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[6] M☉ |
| Radius | 1.7[2] R☉ |
| Luminosity | 2.5[2] L☉ |
| Surface gravity (log g) | 4.00[2] cgs |
| Temperature | 5,500±150[2] K |
| Age | 12.3[7] Gyr |
| B | |
| Mass | 0.951±0.005[6] M☉ |
| Other designations | |
| 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]
See also
References
- ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 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. doi:10.1051/aas:2000237. Bibcode: 2000A&AS..145..215P.
- ↑ 4.0 4.1 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.
- ↑ 5.0 5.1 5.2 5.3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 6.0 6.1 6.2 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. doi:10.1051/0004-6361/201936199. A96. Bibcode: 2019A&A...630A..96A.
- ↑ 7.0 7.1 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. doi:10.1051/0004-6361/201016276. Bibcode: 2011A&A...530A.138C.
- ↑ "HD 158614". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+158614.
- ↑ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics 575: 13. doi:10.1051/0004-6361/201425221. A35. Bibcode: 2015A&A...575A..35B.
- ↑ 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. doi:10.1086/116006. Bibcode: 1991AJ....102.1816P.
- ↑ Ferreira, Letícia D. et al. (March 2010). "On The Physical Existence of The Zeta Reticuli Moving Group: A Chemical Composition Analysis". Chemical Abundances in the Universe: Connecting First Stars to Planets, Proceedings of the International Astronomical Union, IAU Symposium 265: 360–361. doi:10.1017/S174392131000092X. Bibcode: 2010IAUS..265..360F.
- ↑ Batten, A. H. et al. (March 1991). "The Binary System Sigma 2173". Publications of the Astronomical Society of the Pacific 103: 294. doi:10.1086/132818. Bibcode: 1991PASP..103..294B.
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