Knowledge Base Wiki

Search for LIMS content across all our Wiki Knowledge Bases.

Type a search term to find related articles by LIMS subject matter experts gathered from the most trusted and dynamic collaboration tools in the laboratory informatics industry.

HD 176051
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]
Distance48.5 ± 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
Mass1.07[2] M☉
Radius1.06[9] R☉
Luminosity1.65[5] L☉
Surface gravity (log g)4.60[10] cgs
Temperature6,000[10] K
Metallicity [Fe/H]−0.11[10] dex
Age8.1[11] Gyr
HD 176051 B
Mass0.71[2] M☉
Radius0.81[9] R☉
Other designations
ADS 11871, HR 7162, BD+32°3267, GJ 738, HD 176051, LTT 15567, SAO 67612, HIP 93017.[12]
Database references
SIMBADAB
A
B
Exoplanet Archivedata
ARICNSdata
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]

Planetary system

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.

The HD 176051 planetary system[14]
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]

See also

References

  1. ^ a b c d e van Leeuwen, F. (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.
  2. ^ a b c d Muterspaugh, Matthew W.; et al. (2006). "Limits to tertiary astrometric companions in binary systems". The Astrophysical Journal. 653 (2): 1469–1479. arXiv:astro-ph/0608640. Bibcode:2006ApJ...653.1469M. doi:10.1086/508743. S2CID 15218103.
  3. ^ a b Rakos, K. D.; et al. (February 1982). "Photometric and astrometric observations of close visual binaries". Astronomy and Astrophysics Supplement Series. 47: 221–235. Bibcode:1982A&AS...47..221R.
  4. ^ a b Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington D.C.: Carnegie Institute. Bibcode:1953GCRV..C......0W.
  5. ^ a b 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, S2CID 119257644.VizieR
  6. ^ a b Pourbaix, D.; et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits", Astronomy & Astrophysics, 424: 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.VizierR (obsoleted)
  7. ^ a b c Muterspaugh, Matthew W.; Lane, Benjamin F.; et al. (2010). "The PHASES Differential Astrometry Data Archive. V. Candidate Substellar Companions to Binary Systems". The Astronomical Journal. 140 (6): 1657–1671. arXiv:1010.4048. Bibcode:2010AJ....140.1657M. doi:10.1088/0004-6256/140/6/1657. 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☉...
  8. ^ Simonetti, Paolo; et al. (2020). "Statistical Properties of Habitable Zones in Stellar Binary Systems". The Astrophysical Journal. 903 (2): 141. arXiv:2010.05585. Bibcode:2020ApJ...903..141S. doi:10.3847/1538-4357/abc074. S2CID 222291409.
  9. ^ a b Johnson, H. M.; et al. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". The Astrophysical Journal Supplement Series. 53: 643. Bibcode:1983ApJS...53..643J. doi:10.1086/190905."VizieR−GJ 738A/738B"
  10. ^ a b c d Luck, R. E.; Heiter, U. (2006). "Dwarfs in the local region". Astronomical Journal. 131 (6): 3069–3092. Bibcode:2006AJ....131.3069L. doi:10.1086/504080.
  11. ^ Holmberg, J.; et al. (2007). "The Geneva-Copenhagen survey of the Solar neighbourhood. II. New uvby calibrations and rediscussion of stellar ages, the G dwarf problem, age-metallicity diagram, and heating mechanisms of the disk". Astronomy & Astrophysics. 475 (2): 519–537. arXiv:0707.1891. Bibcode:2007A&A...475..519H. doi:10.1051/0004-6361:20077221. S2CID 119054949.
  12. ^ a b "Simbad Query Result: HD 176051 -- Spectroscopic binary". Simbad. Centre de Données astronomiques de Strasbourg. Retrieved 2009-05-07.
  13. ^ 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.
  14. ^ a b Schneider, J (1995). "Notes for star HD 176051 b". Extrasolar Planets Encyclopaedia. Retrieved 2010-10-22.
source: https://en.wikipedia.org/wiki/HD_176051