HD 158614
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Ophiuchus[1] |
| Right ascension | 17h 30m 23.79699s[2] |
| Declination | −01° 03′ 46.4882″[2] |
| Apparent magnitude (V) | +5.31[3] (6.02 + 5.93)[4] |
| Characteristics | |
| Evolutionary stage | Subgiant[5] |
| Spectral type | G9IV-V + G9IV-V[4] |
| B−V color index | +0.715±0.013[1] |
| Astrometry | |
| Radial velocity (Rv) | −77.197±0.064[6] km/s |
| Proper motion (μ) | RA: −127.77[2] mas/yr Dec.: −168.61[2] mas/yr |
| Parallax (π) | 61.19±0.68 mas[2] |
| Distance | 53.3 ± 0.6 ly (16.3 ± 0.2 pc) |
| Absolute magnitude (MV) | 4.24[1] |
| Orbit[6] | |
| Period (P) | 46.585±0.023 yr |
| Semi-major axis (a) | 969.71±0.60 mas |
| Eccentricity (e) | 0.17636±0.00074 |
| Inclination (i) | 99.177±0.037° |
| Longitude of the node (Ω) | 151.769±0.033° |
| Periastron epoch (T) | 2008.601±0.037 |
| Argument of periastron (ω) (secondary) | 324.57±0.32° |
| Semi-amplitude (K1) (primary) | 5.00±0.11 km/s |
| Semi-amplitude (K2) (secondary) | 5.40±0.11 km/s |
| Details | |
| A | |
| Mass | 1.018±0.048[6] M☉ |
| B | |
| Mass | 0.943±0.046[6] M☉ |
| Other designations | |
| STF 2173, BD−00°3300, GJ 678, HIP 85667, HR 6516, SAO 141702, WDS J17304-0104[7] | |
| 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.[3] 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[1] and is predicted to come to within 11.0 light-years in around 196,000 years.[8] The system has been included as a candidate member of the Zeta Herculis moving group.[9] However, chemical abundances appear to rule that out.[10]
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,[11] yielding orbital elements showing a period of 46.585 years and an eccentricity of 0.17636.[6] The two components have similar spectra that match a stellar classification of G9IV-V.[4] They show almost no luminosity variation; one of the pair appears to vary by 0.002 in magnitude.[5] Both components have masses similar to that of the Sun: 102% and 94%, respectively.[6]
See also
References
- 1 2 3 4 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. XHIP record for this object at VizieR.
- 1 2 3 4 5 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.
- 1 2 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.
- 1 2 3 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.
- 1 2 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.
- 1 2 3 4 5 6 Mason, Brian D.; Tokovinin, Andrei; Mendez, Rene A.; Costa, Edgardo (October 2023). "Speckle Interferometry at SOAR in 2022". The Astronomical Journal. 166 (4): 139. Bibcode:2023AJ....166..139M. doi:10.3847/1538-3881/acedaf. ISSN 0004-6256.
- ↑ "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.
