HD 214810

Last updated • a couple of secsFrom Wikipedia, The Free Encyclopedia
HD 214810
Observation data
Epoch J2000       Equinox J2000
Constellation Aquarius
Right ascension 22h 40m 47.95600s [1]
Declination −03° 33 15.2789 [1]
Apparent magnitude  (V)6.32 (6.52 + 8.63) [2]
Characteristics
Spectral type G9 V Fe-0.7 [3]
U−B color index −0.02 [4]
B−V color index +0.52 [4]
Astrometry
Radial velocity (Rv)13.73 km/s
Proper motion (μ)RA: -7.52 [1]   mas/yr
Dec.: -45.25 [1]   mas/yr
Parallax (π)28.93 ± 0.77  mas [1]
Distance 113 ± 3  ly
(34.6 ± 0.9  pc)
Orbit [5]
Period (P)54.57 ± 0.30 yr
Semi-major axis (a)0.367 ± 0.003″
Eccentricity (e)0.005 ± 0.003
Inclination (i)87.5 ± 0.5°
Longitude of the node (Ω)128.9 ± 0.5°
Periastron epoch (T) B 1969.38 ± 1.5
Argument of periastron (ω)
(secondary)
12.9 ± 20.0°
Details
HD 214810 A
Mass 1.26 [6]   M
Surface gravity (log g)4.19 [3]   cgs
Temperature 6,151 [3]   K
Metallicity [Fe/H]−0.22 [3]   dex
Age 3.7 [7]   Gyr
HD 214810 B
Mass 0.87 [6]   M
Other designations
BD-04° 5728, HD 214810, HIP 111965, HR 8629, SAO 146239.
Database references
SIMBAD data

HD 214810 is a visual binary star in the equatorial constellation of Aquarius. The pair orbit each other with a period of about 54.2 years. [2]

Related Research Articles

Zeta Trianguli Australis is a spectroscopic binary in the constellation Triangulum Australe. It is approximately 39.5 light years from Earth.

Rho Tucanae is a binary star system in the southern constellation of Tucana. It is visible to the naked eye with a combined apparent visual magnitude of +5.38. Based upon an annual parallax shift of 24.37 mas as seen from Earth, it is located 131 light years from the Sun.

<span class="mw-page-title-main">Omega Ursae Majoris</span> Binary system in the constellation Ursa Major

Omega Ursae Majoris is the Bayer designation for a binary star system in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of 4.61. Based upon an annual parallax shift of 13.24 mas, it is roughly 246 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.11 due to interstellar dust.

HD 211415 is a double star in the constellation Grus. With an apparent visual magnitude of 5.33, it is visible to the naked eye. The annual parallax shift is 72.54 mas, which yields a distance estimate of 45 light years. It has a relatively high proper motion, traversing the celestial sphere at the rate of 93.4 mas per year, and is moving closer to the Sun with a radial velocity of −13 km/s.

Theta1 Crucis is a spectroscopic binary star system in the southern constellation of Crux. It is visible to the naked eye with an apparent visual magnitude of 4.30m. The distance to this star, as determined using parallax measurements, is around 235 light years.

<span class="mw-page-title-main">HR 5553</span> Binary star system in the constellation Boötes

HR 5553 is a binary star system located thirty-eight light-years away from the Sun, in the northern constellation Boötes. It has the variable star designation DE Boötis, and is classified as an RS Canum Venaticorum variable that ranges in apparent visual magnitude from 5.97 down to 6.04, which is bright enough to be dimly visible to the naked eye. The system is drifting closer to the Sun with a radial velocity of −30 km/s, and is expected to come as close as 26.9 light-years in 210,000 years.

HD 213429 is a spectroscopic binary system in the equatorial constellation of Aquarius. It has a combined apparent magnitude of 6.16 and is located around 83 light years away. The pair orbit each other with a period of 631 days, at an average separation of 1.74 AU and an eccentricity of 0.38.

HD 214448 is a binary star system in the equatorial constellation of Aquarius. They orbit each other with a period of around 147 years. The combined mass of the pair is twice that of the Sun.

HD 200375 is a binary star system in the equatorial constellation of Aquarius. Their orbit does not yet have a unique solution available.

HD 180555 is a binary star in the equatorial constellation of Aquila. It consists of a two stars, orbiting with an orbital period of 8.95 years and an eccentricity of 0.43. A third component lies at an angular separation of 8.32″, but it is unrelated to the system.

HD 188405 is a binary star in the equatorial constellation of Aquila. The pair have an orbital period of roughly 425 years and an angular separation of 1.085″.

HD 149837 is a binary star in the southern constellation of Ara.

HD 118889 is a binary star system in the northern constellation of Boötes. It is faintly visible to the naked eye as a point of light with an apparent visual magnitude of 5.57. The system is located at a distance of approximately 196 light years from the Sun based on stellar parallax, but is drifting closer with a radial velocity of −26 km/s.

HD 127726 is a binary star system in the northern constellation of Boötes. The pair consist of a rapidly-rotating A-type main-sequence star and a fainter F-type companion, orbiting each other with a period of 29.93 years and an orbital eccentricity (ovalness) of 0.16. They have a combined apparent visual magnitude of 5.88, which is bright enough to be dimly visible to the naked eye. The system is located at a distance of approximately 240 light years from the Sun.

39 Draconis is a wide binary star system in the northern circumpolar constellation of Draco. It has the Bayer designation b Draconis, while 39 Draconis is the Flamsteed designation. This system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.0. Parallax measurements made by the Hipparcos spacecraft put it at a distance of 184 light-years, or 56 parsecs away from the Sun. The system is moving closer to the Earth with a heliocentric radial velocity of -24.5 km/s.

66 Tauri, also known as r Tauri, is a binary star in the constellation of Taurus. The combined apparent magnitude of the system is 5.098, with the magnitudes of the two components being 5.8 and 5.9, respectively. Parallax measurements by Hipparcos put 66 Tauri at some 400 light-years away.

78 Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.93. Parallax estimates by Hipparcos put it at a distance of 83 light-years (25 pc), but it is drifting closer with a radial velocity of −5 km/s. The system is a candidate member of the Ursa Major Moving Group.

ω Leonis, is a star system located in the zodiac constellation of Leo. It is visible to the naked eye in the absence of light pollution, with an apparent visual magnitude of about 5.4. The distance to this star, as determined using parallax measurements, is around 108 light years from the Sun. Because of its location close to the ecliptic, it is subject to being obscured by the Moon, and potentially by planets.

171 G. Puppis is a triple star system in the constellation of Puppis – the stern of Argo Navis – of apparent magnitude +5.38. Lacking a Bayer designation, it is instead known by its Gould designation. Based upon parallax measurements, the system is 49.6 light years away from the Solar System.

Lambda Crateris, Latinized from λ Crateris, is the Bayer designation for a suspected binary star system in the southern constellation of Crater. With an annual parallax shift of 23.32 milliarcsecond as observed from Earth, it is located around 140 light years from the Sun. It is faintly visible to the naked eye with an apparent visual magnitude of 5.08.

References

  1. 1 2 3 4 5 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. 1 2 Cvetkovic, Z.; Ninkovic, S. (2010), "On the Component Masses of Visual Binaries", Serbian Astronomical Journal, 180 (180): 71–80, Bibcode:2010SerAJ.180...71C, doi: 10.2298/SAJ1080071C
  3. 1 2 3 4 Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal , 132 (1): 161–170, arXiv: astro-ph/0603770 , Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID   119476992
  4. 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M
  5. "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 1 August 2017. Retrieved 21 May 2017.
  6. 1 2 Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 14, arXiv: 1401.6827 , Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID   56066740, 87
  7. Holmberg, J.; Nordström, B.; Andersen, J. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv: 0811.3982 , Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID   118577511