HD 171301

Last updated
HD 171301
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Lyra
Right ascension 18h 32m 49.95782s [1]
Declination +30° 33′ 15.14853″ [1]
Apparent magnitude  (V)5.47 [2] + 12.7 [3]
Characteristics
Spectral type B8IV [4] or B8V [5]
U−B color index −0.463 [2]
B−V color index −0.077±0.003 [2]
Astrometry
Radial velocity (Rv)−10.3±1.5 [6]  km/s
Proper motion (μ)RA: 13.229 [1]   mas/yr
Dec.: 11.581 [1]   mas/yr
Parallax (π)9.3894 ± 0.1103  mas [1]
Distance 347 ± 4  ly
(107 ± 1  pc)
Absolute magnitude  (MV)0.27 [2]
Details
A
Mass 3.12±0.03 [7]   M☉
Radius 2.7±0.1 [8]   R☉
Luminosity 123.8+7.7
−7.1 [7]   L☉
Temperature 11,695±81 [7]   K
Metallicity [Fe/H]+0.08±0.07 [9]   dex
Rotational velocity (v sin i)36±2 [5]  km/s
Other designations
BD+30°3223, GC  25340, HD  171301, HIP  90923, HR  6968, SAO  67090, CCDM J18328+3033, GSC  02624-02539 [10]
Database references
SIMBAD data

HD 171301 is a suspected binary star [11] system in the northern constellation of Lyra. It has not been well-studied. [5] The brighter member of the pair, designated component A, [3] has a blue-white hue and is visible to the naked eye with an apparent visual magnitude of 5.47. [2] The system is located at a distance of approximately 347  light years from the Sun based on parallax, but is drifting closer with a radial velocity of −10 km/s. [6]

The stellar classification of HD 171301 is B8IV, [4] matching a late B-type star that may be a subgiant that is evolving off the main sequence. HD 171301 appears to be a type of chemically peculiar mercury-manganese star. [5] It has an estimated mass three [7] times that of the Sun and 2.7 times the Sun's radius. [8] The star is spinning with a projected rotational velocity of 36 km/s. [5] It is radiating 124 [7] times the luminosity of the Sun from its photosphere at an effective temperature of 11,695 K. [7]

Its companion, component B, is a 13th magnitude star of an unknown spectral type. [12] It was first reported by S. W. Burnham in 1891. As of 1998, it was located at an angular separation of 6.7  arcseconds from the brighter star along a position angle of 157°. [3]

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<span class="mw-page-title-main">8 Andromedae</span> Mulitple star system in the constellation Andromeda

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<span class="mw-page-title-main">10 Canis Majoris</span> Star in the constellation Canis Major

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17 Canis Majoris is a single star in the southern constellation of Canis Major, located 610 light years away from the Sun. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 5.80. The object is moving closer to the Earth with a heliocentric radial velocity of −13 km/s.

HD 69863 is a binary star system in the southern constellation of Carina. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.16. The system is located at a distance of about255 light years from the Sun based on parallax. The dual nature of this system was announced in 1832 by German astronomer Carl Rümker. As of 2015, the pair had an angular separation of 4.10″ along a position angle of 70°.

HD 5789 and HD 5788 is a pair of stars comprising a binary star system in the northern constellation of Andromeda. Located approximately 151 parsecs (490 ly) away, the primary is a hot, massive blue star with an apparent magnitude of 6.06 while the secondary is slightly smaller and cooler, with an apparent magnitude of 6.76. Both stars are main-sequence stars, meaning that they are currently fusing hydrogen into helium in their cores. As of 2016, the pair had an angular separation of 7.90″ along a position angle of 195°. While both have a similar proper motion and parallax, there's still no proof that the pair is gravitationally bound.

HD 225218 is a quadruple star system in the northern constellation of Andromeda. The primary component, HD 225218 A, is a giant star with a stellar classification of B9III, an apparent magnitude of 6.16, and is a candidate Lambda Boötis star. It has a fainter, magnitude 9.65 companion, HD 225218 B, at an angular separation of 5.2″ along a position angle of 171°. The primary itself has been identified as a binary star system through interferometry, with the two components separated by 0.165″. The pair, HD 225218 Aa and Ab, orbit each other with a period of about 70 years and an eccentricity of 0.515. Component B is likewise a spectroscopic binary.

HD 220105 is a star in the northern constellation of Andromeda, and a member of the Sirius supercluster. It lies near the lower limit of visibility to the naked eye at an apparent visual magnitude of 6.24, and can be a challenge to spot under normal viewing conditions. The star is located 238 light years away, based upon an annual parallax shift of 13.78 mas. It is moving closer to the Earth with a heliocentric radial velocity of −2 km/s.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 108 parsecs (350 ly) distant.

HD 222399 is a double star in the northern constellation of Andromeda. The magnitude 6.57 primary is an F-type subgiant star with a stellar classification of F2IV. It has a magnitude 10.57 companion at an angular separation of 14.7″ along a position angle of 162°.

HD 82785 is star in the southern constellation of Antlia. With an apparent visual magnitude of 6.43, it is near the lower limit of visibility to the naked eye. The distance to this star, based on parallax measurements, is 240 light years. It is drifting further away from the Sun with a radial velocity of 28 km/s, having come to within 142 light-years some 1.7 million years ago. It has an absolute magnitude of 2.06.

HD 161988, also known as HR 6635, is a solitary, orange hued star located in the southern circumpolar constellation Apus. It has an apparent magnitude of 6.07, allowing it to be faintly visible to the naked eye. Parallax measurements place it at a distance of 621 light years, and it is currently receding with a heliocentric radial velocity of 36.8 km/s.

HD 16955, also known as HR 803, is a double or multiple star. With an apparent visual magnitude of 6.376, is lies at or below the nominal limit for visibility with a typical naked eye. The measured annual parallax shift is 9.59 milliarcseconds, which yields an estimated distance of around 340 light years. The star is moving closer to the Sun with a heliocentric radial velocity of around -10 km/s.

HD 3 is a single, white-hued star in the northern constellation Andromeda. With an apparent visual magnitude of 6.71, it is below the nominal brightness limit for visibility with the typical naked eye but may still be visible by some observers under ideal viewing conditions. It is also the first star indexed in the Bright Star Catalogue. Based upon an annual parallax shift of 6.3137±0.0826 mas, it is located roughly 517 light years away. The star is moving closer with a heliocentric radial velocity of −18 km/s, and will make perihelion in around 2.9 million years at a separation of around 351 ly (107.71 pc).

6 Equulei is a probable astrometric binary star system in the northern constellation of Equuleus, located 380 light years from the Sun. It is barely visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 6.07. The system is moving further away from the Earth with a heliocentric radial velocity of +6.9 km/s. It forms a wide optical double with γ Equulei, at an angular separation of 336 arcseconds in 2011.

HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.

f Eridani Multiple star system in the constellation Eridanus

f Eridani is a binary, or possibly a triple, star system in the equatorial constellation of Eridanus, consisting of stars HD 24071 and HD 24072. They share a single Hipparcos catalogue entry, HIP 17797, but have separate Bright Star Catalogue listings, HR 1189 and 1190. f Eridani is the Bayer designation of the pair.

HD 49268 is a solitary star in the southern circumpolar constellation Volans. It has an apparent magnitude of +6.49, placing it near the limit of naked eye visibility. Parallax measurements place the object at a distance of 456 light years; it is receding with a heliocentric radial velocity of 20.6 km/s.

HD 193472 is a solitary star in the equatorial constellation Delphinus. It has an apparent magnitude of 5.94, making it visible with the naked eye if viewed under ideal conditions. Parallax measurements put it at a distance of 282 light years and has a radial velocity of −8 km/s, indicating that the object drifting towards the Solar System.

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 5 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.
  3. 1 2 3 Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
  4. 1 2 Osawa, Kiyoteru (1959), "Spectral Classification of 533 B8-A2 Stars and the Mean Absolute Magnitude of A0 V Stars", Astrophysical Journal, 130: 159, Bibcode:1959ApJ...130..159O, doi: 10.1086/146706
  5. 1 2 3 4 5 Adelman, S. J.; et al. (June 2017). "Elemental abundance analyses with DAO spectrograms: XL". Astronomische Nachrichten. 338 (5): 584–597. Bibcode:2017AN....338..584A. doi:10.1002/asna.201613214.
  6. 1 2 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  7. 1 2 3 4 5 6 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv: 1201.2052 . Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID   55586789.
  8. 1 2 Kervella, Pierre; et al. (March 2019). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy & Astrophysics. 623: 23. arXiv: 1811.08902 . Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. S2CID   119491061. A72.
  9. ↑ Gáspár, András; et al. (2016). "The Correlation between Metallicity and Debris Disk Mass". The Astrophysical Journal. 826 (2): 171. arXiv: 1604.07403 . Bibcode:2016ApJ...826..171G. doi:10.3847/0004-637x/826/2/171. S2CID   119241004.
  10. ↑ "HD 171301". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved October 16, 2007.
  11. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society . 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  12. ↑ "CCDM J18328+3033B". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved October 16, 2007.
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