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Xi Ophiuchi
Location of ξ Ophiuchi (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Ophiuchus
Right ascension 17h 21m 00.37452s [1]
Declination −21° 06′ 46.5710″ [1]
Apparent magnitude (V) 4.39 [2]
Characteristics
Spectral type F2V [3]
U−B color index -0.06 [4]
B−V color index +0.41 [4]
Astrometry
Radial velocity (Rv)−8.73±0.12 [1] km/s
Proper motion (μ) RA: +265.543  mas/ yr [1]
Dec.: -202.584  mas/ yr [1]
Parallax (π)57.0820 ± 0.1851  mas [1]
Distance57.1 ± 0.2  ly
(17.52 ± 0.06  pc)
Absolute magnitude (MV)3.19 [2]
Details [5]
A
Mass1.30  M☉
Radius1.59±0.06  R☉
Luminosity4.429±0.035 [6]  L☉
Surface gravity (log g)4.15±0.10  cgs
Temperature6,611±80  K
Metallicity [Fe/H]−0.27±0.07  dex
Rotational velocity (v sin i)20.2±0.7 km/s
Age916 [7]  Myr
Other designations
ξ Oph, 40 Ophiuchi, BD−20°4731, FK5 917, GC 23423, HD 156897, HIP 84893, HR 6445, SAO 185296, CCDM J17210-2107AB, WDS J17210-2107AB, LTT 6908 [8]
Database references
SIMBAD data

ξ Oph, Latinized as Xi Ophiuchi, is a visual binary star [9] system in the equatorial constellation of Ophiuchus. [2] It has a yellow-white hue and is faintly visible to the naked eye with a combined apparent visual magnitude of 4.39. [2] The system is located approximately 57.1 light-years (17.5 parsecs) away from the Sun based on parallax, but is drifting closer with a radial velocity of -9 km/s. [1]

The magnitude 4.40 [10] primary, designated component A, is an ordinary F-type main-sequence star with a stellar classification of F2V. [3] It is 916 [7] million years old and is rotating with a projected rotational velocity of 20 km/s. The star has 1.3 times the mass of the Sun and 1.6 times the Sun's radius. [5] It is radiating 4.4 [6] times the luminosity of the Sun from its photosphere at an effective temperature of 6,611 K. [5]

The system is a source of X-ray emission. [11] The orbiting companion, component B, is a magnitude 8.9 star at an angular separation of 35 ″ along a position angle of 27° from the primary, as of 2015. A magnitude 10.8 visual companion, component C, lies at a separation of 10.8″, as of 2004. [10]

According to Richard H. Allen's Star Names: Their Lore and Meaning (1899), ξ Oph together with θ Oph formed the Sogdian Wajrik "the Magician", the Khorasmian Markhashik "the Serpent-bitten" and with η Oph the Coptic Tshiō, "the Snake", and Aggia, "the Magician". [12]

References

  1. ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID  244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d 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 catalog entry
  3. ^ a b Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (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. ^ a b Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode: 2014JAVSO..42..443M. Vizier catalog entry
  5. ^ a b c Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z. (2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal. 836 (1): 139. Bibcode: 2017ApJ...836..139F. doi: 10.3847/1538-4357/836/1/139.
  6. ^ a b 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.
  7. ^ a b David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154. Bibcode: 2015ApJ...804..146D. doi: 10.1088/0004-637X/804/2/146. S2CID  33401607. Vizier catalog entry
  8. ^ "ksi Oph". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-08.
  9. ^ 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.
  10. ^ a b Mason, Brian D.; et al. (200). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode: 2001AJ....122.3466M. doi: 10.1086/323920. Vizier catalog entry
  11. ^ Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009). "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources". The Astrophysical Journal Supplement. 184 (1): 138–151. arXiv: 0910.3229. Bibcode: 2009ApJS..184..138H. doi: 10.1088/0067-0049/184/1/138. S2CID  119267456.
  12. ^ Allen, R.H. (1899), Star Names: Their Lore and Meaning, p. 297
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