Astronomy:22 Orionis

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Short description: Binary star system in the constellation Orion
22 Orionis
Orion constellation map.svg
Red circle.svg
Location of 22 Orionis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Orion
Right ascension  05h 21m 45.74861s[1]
Declination 0° 22′ 56.9105″[1]
Apparent magnitude (V) 4.74[2]
Characteristics
Spectral type B2 IV-V[3][4]
U−B color index -0.79[2]
B−V color index -0.16[2]
Astrometry
Radial velocity (Rv)+28.80[5] km/s
Proper motion (μ) RA: −1.320[1] mas/yr
Dec.: +3.457[1] mas/yr
Parallax (π)2.8672 ± 0.3512[1] mas
Distanceapprox. 1,100 ly
(approx. 350 pc)
Absolute magnitude (MV)−2.98[6]
Orbit[7]
Period (P)293 days
Eccentricity (e)0.15
Periastron epoch (T)2,442,175 JD
Argument of periastron (ω)
(secondary)		234°
Semi-amplitude (K1)
(primary)		4.1 km/s
Details
22 Ori A
Mass9.0[8] M☉
Luminosity741[9] L☉
Surface gravity (log g)3.56[10] cgs
Temperature19,953[9] K
Metallicity [Fe/H]−0.06[10] dex
Rotational velocity (v sin i)9[9] km/s
Age18.5[8] Myr
Other designations
o Orionis, 22 Ori, NSV 16291, BD−00°930, FK5 1147, GC 6579, HD 35039, HIP 25044, HR 1765, SAO 132028[11]
Database references
SIMBADdata

22 Orionis is a binary star[12] in the equatorial constellation of Orion. It has the Bayer designation o Orionis, while 22 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.74.[2] It is located approximately 1,100 light years away from the Sun based on parallax.[1] The system is moving further from the Earth with a heliocentric radial velocity of +28.80[5]

This is a single-lined spectroscopic binary with an orbital period of 293 days and an eccentricity of 0.15.[7] The visible member, component A, has a stellar classification of B2 IV-V,[3][4] matching a B-type star with a luminosity class that displays mixed traits of a main sequence star and a subgiant. It is a suspected Beta Cephei variable[13] or a slowly pulsating B star.[14] The star has nine[8] times the mass of the Sun and is radiating 741 times the Sun's luminosity[9] from its photosphere at an effective temperature of 19,953 K.[9]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237. Bibcode: 2002yCat.2237....0D. 
  3. ↑ 3.0 3.1 van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal 694 (2): 1085–1098. doi:10.1088/0004-637X/694/2/1085. Bibcode: 2009ApJ...694.1085V. 
  4. ↑ 4.0 4.1 Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H 5050. Bibcode: 1995yCat.5050....0H. 
  5. ↑ 5.0 5.1 Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication (Carnegie Institution for Science). Bibcode: 1953GCRV..C......0W. 
  6. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.  Vizier catalog entry
  7. ↑ 7.0 7.1 Abt, H. A.; Levy, S. G. (1978). "Binaries among B2-B5 IV, V absorption and emission stars". The Astrophysical Journal Supplement Series 36: 241–258. doi:10.1086/190498. Bibcode: 1978ApJS...36..241A. 
  8. ↑ 8.0 8.1 8.2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T.  Vizier catalog entry
  9. ↑ 9.0 9.1 9.2 9.3 9.4 Simón-Díaz, S.; Godart, M.; Castro, N.; Herrero, A.; Aerts, C.; Puls, J.; Telting, J.; Grassitelli, L. (2017). "The IACOB project . III. New observational clues to understand macroturbulent broadening in massive O- and B-type stars". Astronomy and Astrophysics 597: A22. doi:10.1051/0004-6361/201628541. Bibcode: 2017A&A...597A..22S.  Vizier catalog entry
  10. ↑ 10.0 10.1 Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent (2016). "The PASTEL catalogue: 2016 version". Astronomy & Astrophysics 591: A118. doi:10.1051/0004-6361/201628497. Bibcode: 2016A&A...591A.118S. 
  11. ↑ "22 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=22+Ori. 
  12. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  13. ↑ Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1. Bibcode: 2009yCat....102025S. 
  14. ↑ Smith, M. A. (February 1980), "Nonradial m-mode changes in the 53 Persei variable 22 Orionis", Astrophysical Journal Supplement Series 42: 261–281, doi:10.1086/190651, Bibcode: 1980ApJS...42..261S 



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