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Binary star in the constellation Ophiuchus From Wikipedia, the free encyclopedia
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]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
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 mas[1] |
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 |
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]
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