External links
- HD 176051 b on The Extrasolar Planets Encyclopaedia
- Candidate substellar companions of binary systems
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18h 57m 01.60985s [1] |
| Declination | +32° 54′ 04.5723″ [1] |
| Apparent magnitude (V) | 5.22 |
| Characteristics | |
| Spectral type | G0 V + K1 V [2] |
| U−B color index | +0.029 [3] |
| B−V color index | +0.570 [3] |
| Astrometry | |
| Radial velocity (Rv) | −47.2 [4] km/s |
| Proper motion (μ) | RA: +201.96 [1] mas/yr Dec.: −145.46 [1] mas/yr |
| Parallax (π) | 67.24 ± 0.37 mas [1] |
| Distance | 48.5 ± 0.3 ly (14.87 ± 0.08 pc) |
| Absolute magnitude (MV) | 4.34 [5] |
| Orbit [6] | |
| Period (P) | 22,423 d |
| Semi-major axis (a) | 19.1 AU [7] |
| Eccentricity (e) | 0.25 (0.27 [7] or 0.54 [8] ) |
| Argument of periastron (ω) (secondary) | 102° |
| Semi-amplitude (K1) (primary) | 3.51 km/s |
| Semi-amplitude (K2) (secondary) | 0.74 km/s |
| Details | |
| HD 176051 A | |
| Mass | 1.07 [2] M☉ |
| Radius | 1.06 [9] R☉ |
| Luminosity | 1.65 [5] L☉ |
| Surface gravity (log g) | 4.60 [10] cgs |
| Temperature | 6,000 [10] K |
| Metallicity [Fe/H] | −0.11 [10] dex |
| Age | 8.1 [11] Gyr |
| HD 176051 B | |
| Mass | 0.71 [2] M☉ |
| Radius | 0.81 [9] R☉ |
| Other designations | |
| Database references | |
| SIMBAD | AB |
| A | |
| B | |
| Exoplanet Archive | data |
| ARICNS | data |
| data2 | |
| Extrasolar Planets Encyclopaedia | data |
HD 176051 is a spectroscopic binary star system [12] approximately 49 light years away from Earth in the constellation Lyra. The pair orbit with a period of 22,423 days (61.4 years) and an eccentricity of 0.25. [6] Compared to the Sun, they have a somewhat lower proportion of elements more massive than helium. [10] Their individual masses are estimated at 1.07 and 0.71 solar masses (M☉). [2] The system is moving closer to the Sun with a radial velocity of −47 [4] km/s and will reach perihelion in about 269,000 years when it comes within roughly 17 ly (5.1 pc) of the Sun. [13]
A planet orbiting one of the stars was discovered through astrometric observations. However, it is not known which stellar component the planet is orbiting around.
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 1.5 ± 0.3 MJ | 1.76 | 1016 ± 40 | 0 | — | — |
The planet parameters are given here for the 0.71 M☉ component B. [7] But, if instead the planet is orbiting the 1.07 M☉ component A, its mass is 2.26 MJ with a semimajor axis of 2.02 AU. [14]
HD 168443 is an ordinary yellow-hued star in the Serpens Cauda segment of the equatorial constellation of Serpens. It is known to have two substellar companions. With an apparent visual magnitude of 6.92, the star lies just below the nominal lower brightness limit of visibility to the normal human eye. This system is located at a distance of 127 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −48.7 km/s.
HD 142 is a wide binary star system in the southern constellation of Phoenix. The main component has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.7. The system is located at a distance of 85.5 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +6 km/s.
HD 1237 is a binary star system approximately 57 light-years away in the constellation of Hydrus.
HD 59686 is a binary star system in the northern constellation of Gemini. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.45. The distance to this system is approximately 292 light years based on parallax, but it is drifting closer with a radial velocity of −34 km/s.
Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.
HD 191104 is a star system in the equatorial constellation of Aquila. Two of the components form a close spectroscopic binary system, while a third star, also thought to be a spectroscopic binary, orbits the pair at a greater distance.
HD 34790 is a double-lined spectroscopic binary star system in the northern constellation of Auriga. It has a combined apparent magnitude of 5.66, which means it is faintly visible to the naked eye. Based upon observations by the Hipparcos satellite, it is located around 289 light years away. It has a combined stellar classification of A1Vs, matching that of an A-type main sequence star, and shines with 35 times the luminosity of the Sun.
HD 29587 is a Sun-like star with a candidate brown dwarf companion in the northern constellation of Perseus. It has an apparent visual magnitude of 7.29, which means it is too faint to be viewed with the naked eye. Based upon an annual parallax shift of 36.3 mas, it is located 89.8 light years away. The star is moving away from the Earth with a heliocentric radial velocity of +113 km/s, having come to within 55.8 ly some 148,000 years ago. It is a hyper-velocity halo star moving at a rate of 170 km/s relative to the local standard of rest.
HD 132563 is a triple star system in the constellation Boötes. The two resolvable components of this system are designated HD 132563 AC and HD 132563 B. The primary star, HD 132563 AC, is actually a spectroscopic binary with a period of more than 15 years and an orbital eccentricity of greater than 0.65. The smaller member of this tightly orbiting pair has about 55% the mass of the Sun.
HD 81817 is a possible binary star system with two brown dwarf companions in the northern circumpolar constellation of Draco. It has an orange hue and is visible to the naked eye with an apparent visual magnitude of 4.28. The system is located at a distance of approximately 990 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −7 km/s. It is a member of the IC 2391 moving group.
Iota Coronae Borealis, Latinized from ι Coronae Borealis, is a binary star system in the constellation Corona Borealis. It is visible to the naked eye with a combined apparent visual magnitude of is 4.96. Based upon an annual parallax shift of 10.46 mas as seen from the Earth, it is located about 312 light years from the Sun.
Tau1 Eridani, Latinized from τ1 Eridani, is a binary star system in the constellation Eridanus. It has an apparent magnitude of 4.46, making it visible to the naked eye in suitably dark conditions. This a spectroscopic binary with an orbital period of 958 days. It is located about 46 light years from the Earth. At present, the system is moving away from the Sun with a radial velocity of +26 km/s. About 305,000 years ago, it made perihelion passage at an estimated distance of 30.5 ly (9.35 pc).
HD 16754 is a binary or triple-star system in the constellation Eridanus. It has the Bayer designation s Eridani; HD 16754 is the designation from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of +4.74. It is located at a distance of approximately 132 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +18 km/s. The system is a member of the Columba association of co-moving stars.
Iota Gruis, Latinized from ι Gruis, is a binary star system in the southern constellation of Grus. It has an apparent visual magnitude of 3.90, which is bright enough to be seen with the naked eye at night. The distance to this system, as determined using an annual parallax shift of 17.80 mas as seen from the Earth, is about 183 light years.
HD 106515 is a binary star in the constellation of Virgo.
HD 4747 is a star that lies approximately 61 light-years away in the constellation of Cetus. The star is a low-amplitude spectroscopic binary, with the secondary being a directly detected brown dwarf.
HD 167665 is a yellow-white hued star with a brown dwarf companion in the southern constellation of Sagittarius. With an apparent visual magnitude of 6.39, it is near the lower brightness limit for stars that are visible to the naked eye. Based upon an annual parallax shift of 32.4 mas as seen from Earth, it is located 101 light years from the Sun. The star is moving away from the Sun with a radial velocity of +8 km/s.
HD 163840 is a binary star system in the northern constellation of Hercules. It has a combined apparent visual magnitude of 6.45, which falls just below the brightness level that is visible to the naked eye for people with normal eyesight. An annual parallax shift of 35.40 mas provides a distance estimate of about 92 light years. The system is moving closer to the Sun with a radial velocity of −33 km/s. In about 769,000 years, it will make perihelion at a separation of around 27.2 ly (8.33 pc).
HD 3443 is a binary system composed of medium-mass main sequence stars in the constellation of Cetus about 50 light years away.
HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.
The substellar object is a planet 1.5 ± 0.3 times the mass of Jupiter, assuming a distance of 15 pc and a stellar mass of 0.71 M☉...
