22 Orionis

Last updated
22 Orionis
Orion constellation map.svg
Red circle.svg
Location of 22 Orionis (circled)
Observation data
Epoch J2000       Equinox J2000
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  mas [1]
Distance approx. 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
Mass 9.0 [8]   M☉
Luminosity 741 [9]   L☉
Surface gravity (log g)3.56 [10]   cgs
Temperature 19,953 [9]   K
Metallicity [Fe/H]−0.06 [10]   dex
Rotational velocity (v sin i)9 [9]  km/s
Age 18.5 [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
SIMBAD data

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]

Related Research Articles

<span class="mw-page-title-main">Mu Sculptoris</span> Star in the constellation Sculptor

μ Sculptoris, Latinized as Mu Sculptoris, is a solitary, orange-hued star in the southern constellation of Sculptor. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.30. This star is located approximately 291 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +16 km/s.

<span class="mw-page-title-main">Mu Tauri</span> Star in the constellation Taurus

μ Tauri, Latinized as Mu Tauri, is a single star in the equatorial constellation of Taurus. It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.27. The star is located approximately 490 light years distant from the Sun based on parallax, and is drifting further away with a radial velocity of +16 km/s.

<span class="mw-page-title-main">Epsilon Microscopii</span> Star in the constellation Microscopium

Epsilon Microscopii, Latinized from ε Microscopii, is a single, white-hued star in the southern constellationof Microscopium. It is faintly visible to the naked eye with an apparent visual magnitude of 4.71. The annual parallax shift of the star is 19.7054 mas as measured from Earth, which yields a distance estimate of around 166 light years. It is moving further from the Sun with a radial velocity of +7 km/s.

<span class="mw-page-title-main">3 Monocerotis</span> Star in Monoceros constellation

3 Monocerotis is a binary star system in the equatorial constellation of Monoceros, located approximately 780 light years away from the Sun based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.92. The system is moving further from the Earth with a heliocentric radial velocity of +39 km/s.

<span class="mw-page-title-main">HD 102839</span> Star in the constellation Musca

HD 102839 is a class G6Ib star in the constellation Musca. Its apparent magnitude is 4.98 and it is approximately 1,550 light years away from Earth based on parallax.

<span class="mw-page-title-main">Sigma Ophiuchi</span> Star in the constellation Ophiuchus

Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.

<span class="mw-page-title-main">71 Ophiuchi</span> Giant star in the constellation of Ophiuchus

71 Ophiuchi is a single star in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.64. The star is located approximately 273 light years away from the Sun based on parallax, and is moving closer with a radial velocity of −3 km/s.

<span class="mw-page-title-main">30 Ophiuchi</span> Star in the constellation Ophiuchus

30 Ophiuchi is a single star in the equatorial constellation of Ophiuchus, and figures 0.99° east of the heart of cluster Messier 10. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.82. The distance to this star is approximately 350 light years based on parallax. Its present motion is, net, one of approaching rather than parting, at −6.7 km/s, its "radial velocity".

<span class="mw-page-title-main">29 Orionis</span> Aging giant star in the constellation of Orion

29 Orionis is a single star located around 157 light years away from the Sun in the equatorial constellation of Orion. In Bayer's Uranometria, this star is one of two stars marking the top of Orion's right boot. It has the Bayer designation e Orionis, while 29 Orionis is the Flamsteed designation. This object is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.13. It is moving closer to the Earth with a heliocentric radial velocity of -18 km/s.

<span class="mw-page-title-main">11 Orionis</span> Star in the constellation Orion

11 Orionis is a solitary Ap star in the equatorial constellation of Orion, near the border with Taurus. It is visible to the naked eye with an apparent visual magnitude of 4.65, and it is located approximately 365 light years away from the Sun based on parallax. The star is moving further from the Sun with a heliocentric radial velocity of +16.8 km/s.

<span class="mw-page-title-main">31 Orionis</span> Binary star in the constellation Orion

31 Orionis is a binary star system in the equatorial constellation of Orion, located near the bright star Mintaka. It is visible to the naked eye as a faint, orange-hued point of light with a baseline apparent visual magnitude of 4.71. The distance to this system is approximately 490 light years away based on parallax, and it is drifting further away with a mean radial velocity of +6 km/s.

<span class="mw-page-title-main">51 Orionis</span> Star in the constellation of Orion

51 Orionis is a single star in the equatorial constellation of Orion. It has the Bayer designation b Orionis, while 51 Orionis is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.90. It is located approximately 299 light-years away from the Sun based on parallax, and is drifting further away with a radial velocity of +88 km/s.

<span class="mw-page-title-main">17 Persei</span> Star in the constellation Perseus

17 Persei is a single star in the northern constellation of Perseus, located about 390 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.53. This object is moving further from the Earth at a heliocentric radial velocity of +13 km/s.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

<span class="mw-page-title-main">HD 65810</span> Star in the constellation Puppis

HD 65810 is a class A2V star in the constellation Puppis. Its apparent magnitude is 4.61 and it is approximately 241 light years away based on parallax.

<span class="mw-page-title-main">HD 59890</span> Star in the constellation Puppis

HD 59890 is a class G3Ib yellow supergiant star in the constellation Puppis. Its apparent magnitude is 4.65 and it is approximately 1,360 light years away based on parallax.

<span class="mw-page-title-main">9 Persei</span> Blue supergiant star in the constellation Perseus

9 Persei is a single variable star in the northern constellation Perseus, located around 4,300 light years away from the Sun. It has the Bayer designation i Persei; 9 Persei is the Flamsteed designation. This body is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of about 5.2. It is moving closer to the Sun with a heliocentric radial velocity of −15.2 km/s. The star is a member of the Perseus OB1 association of co-moving stars.

<span class="mw-page-title-main">42 Persei</span> Binary star system in the constellation Perseus

42 Persei is a binary star system in the northern constellation of Perseus. It has the Bayer designation n Persei, while 42 Persei is the Flamsteed designation. The system is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude of 5.11. It is located around 93 parsecs (302 ly) distant from the Sun, but is drifting closer with a radial velocity of −12.4 km/s.

<span class="mw-page-title-main">31 Persei</span> Star in the constellation Perseus

31 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a dim, blue-white hued point of light with an apparent visual magnitude of 5.05. This star is located around 172 parsecs (560 ly) away from the Sun, and it is drifting closer with a radial velocity of −1.6 km/s. It is likely a member of the Alpha Persei Cluster.

<span class="mw-page-title-main">Lambda Octantis</span> Star in the constellation Octans

λ Octantis, Latinized as Lambda Octantis, is a binary star system in the southern circumpolar constellation of Octans. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.27. The distance to this system is approximately 398–409 light years, based on parallax, but it is moving closer with a radial velocity of −10 km/s.

References

  1. 1 2 3 4 5 6 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 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. 1 2 van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal (abstract). 694 (2): 1085–1098. arXiv: 0901.1206 . Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. S2CID   18370219.
  4. 1 2 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. 1 2 Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. LCCN   54001336.
  6. ↑ 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
  7. 1 2 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. Bibcode:1978ApJS...36..241A. doi:10.1086/190498.
  8. 1 2 3 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. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi: 10.1111/j.1365-2966.2010.17434.x . S2CID   118629873. Vizier catalog entry
  9. 1 2 3 4 5 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. arXiv: 1608.05508 . Bibcode:2017A&A...597A..22S. doi:10.1051/0004-6361/201628541. S2CID   3478126. Vizier catalog entry
  10. 1 2 Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent (2016). "The PASTEL catalogue: 2016 version". Astronomy & Astrophysics. 591: A118. arXiv: 1605.07384 . Bibcode:2016A&A...591A.118S. doi:10.1051/0004-6361/201628497. S2CID   119258214.
  11. ↑ "22 Ori". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-06-09.
  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. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . S2CID   14878976.
  13. ↑ Samus, N. N.; Durlevich, O. V.; 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, Bibcode:1980ApJS...42..261S, doi: 10.1086/190651
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.