HD 158614
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Ophiuchus[1] |
| Right ascension | Template:RA[2] |
| Declination | Template:DEC[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 Template:Engvar | Script error: No such module "val".[1] |
| Astrometry | |
| Radial velocity (Rv) | Script error: No such module "val".[1] 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 | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | 4.24[1] |
| Orbit[4] | |
| Period (P) | Script error: No such module "val". yr |
| Semi-major axis (a) | Script error: No such module "val". |
| Eccentricity (e) | Script error: No such module "val". |
| Inclination (i) | Script error: No such module "val".° |
| Longitude of the node (Ω) | Script error: No such module "val".° |
| Periastron epoch (T) | Script error: No such module "val". |
| Argument of periastron (ω) (secondary) | Script error: No such module "val".° |
| Details | |
| A | |
| Mass | Script error: No such module "val".[6] Template:Solar mass |
| Radius | 1.7[3] Template:Solar radius |
| Luminosity | 2.5[3] Template:Solar luminosity |
| Surface gravity (log g) | 4.00[3] cgs |
| Temperature | Script error: No such module "val".[3] K |
| Age | 12.3[7] Gyr |
| B | |
| Mass | Script error: No such module "val".[6] Template:Solar mass |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| Template:Odlist[8] | |
| Database references | |
| SIMBAD | data |
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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 Script error: No such module "convert". 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.[4] 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 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.Script error: No such module "Unsubst".
See also
References
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