23 Orionis

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23 Orionis
Observation data
Epoch J2000       Equinox J2000
Constellation Orion
Right ascension 05h 22m 50.00474s [1]
Declination +03° 32′ 39.9770″ [1]
Apparent magnitude  (V)4.99 [2] (4.95 + 6.76) [3]
Characteristics
Evolutionary stage main sequence
Spectral type B1V + B3V [4]
B−V color index −0.096±0.004 [2]
Astrometry
Absolute magnitude  (MV)−2.93 [2]
23 Ori A
Radial velocity (Rv)+18.0±3.7 [5]  km/s
Proper motion (μ)RA: −2.414 [1]   mas/yr
Dec.: +1.230 [1]   mas/yr
Parallax (π)2.7199 ± 0.3155  mas [1]
Distance approx. 1,200  ly
(approx. 370  pc)
23 Ori B
Radial velocity (Rv)28 [6]  km/s
Proper motion (μ)RA: +1.275 [7]   mas/yr
Dec.: −0.552 [7]   mas/yr
Parallax (π)2.5579 ± 0.0864  mas [7]
Distance 1,280 ± 40  ly
(390 ± 10  pc)
Details
23 Ori A
Mass 12.5±0.6 [8]   M☉
Radius 6.97 [9]   R☉
Luminosity 26,546 [10]   L☉
Surface gravity (log g)4.078±0.045 [11]   cgs
Temperature 25,400 [10]   K
Rotational velocity (v sin i)350 [4]  km/s
Age 15.4±0.6 [8]   Myr
23 Ori B
Mass 6.6±0.1 [8]   M☉
Radius 4.71 [9]   R☉
Luminosity1,620 [10]   L☉
Temperature 18,700 [10]   K
Rotational velocity (v sin i)370 [4]  km/s
Age 22.8±2.3 [8]   Myr
Other designations
23 Ori, SAO  112697, WDS J05228+0333 [12]
A: BD+03°871, HD  35149, HIP  25142, HR  1770, SAO  112697
B: BD+03°872, HD  35148, HIP  25145, SAO  112699
Database references
SIMBAD data
B

23 Orionis is a double star located around 1,200 light-years (370 parsecs ) [1] away from the Sun in the equatorial constellation of Orion. [12] It is visible to the naked eye as a dim, blue-white-hued point of light with a combined apparent visual magnitude of 4.99. [2] The pair are moving away from the Earth with a heliocentric radial velocity of +18 km/s, [5] and they are members of the Orion OB1 association, subgroup 1a. [13]

Howe and Clarke (2009) catalog this as a double-lined spectroscopic binary star system [14] with a wide projected separation of 9,460  AU . [9] As of 2018, they had an angular separation of 31.9″ along a position angle of 30°. [3] The brighter member, component A, is a B-type main-sequence star with a stellar classification of B1V. The secondary, component B, is of class B3V. [4] Both stars are spinning rapidly. [4]

Related Research Articles

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Mintaka, designation Delta Orionis and 34 Orionis, is a multiple star system some 1,200 light-years from the Sun in the constellation of Orion. Together with Alnitak and Alnilam, the three stars form Orion's Belt, known by many names among ancient cultures. The star is located very close to the celestial equator. When Orion is near the meridian, Mintaka is the rightmost of the Belt's stars when viewed from the Northern Hemisphere facing south.

Pi<sup>4</sup> Orionis Binary star system in the constellation Orion

Pi4 Orionis (π4 Ori, π4 Orionis) is a binary star system in the western part of the Orion constellation. It is visible to the naked eye with an apparent visual magnitude of 3.7. Based upon an annual parallax shift of 3.1 mass, it is located roughly 1,050 light-years from the Sun.

94 Aquarii is a triple star system in the equatorial constellation of Aquarius. 94 Aquarii is the Flamsteed designation. The brightest member has an apparent visual magnitude of 5.19, making it visible to the naked eye. The parallax measured by the Gaia spacecraft yields a distance estimate of around 73 light-years from Earth.

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<span class="mw-page-title-main">Pi Cassiopeiae</span> Variable star in the constellation Cassiopeia

Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949. Based upon an annual parallax shift of 18.63 mas as seen from Earth, this system is located about 175 light years from the Sun.

<span class="mw-page-title-main">Omega Cassiopeiae</span> Binary star system in constellation Cassiopeia

Omega Cassiopeiae is a binary star system in the northern constellation of Cassiopeia. It has a combined apparent visual magnitude of +4.99, which means it is a faint star but visible to the naked eye. Based upon an annual parallax shift of 4.65 mas as seen from Earth, this system is located roughly 730 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.16 due to interstellar dust.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

<span class="mw-page-title-main">12 Vulpeculae</span> Star in the constellation Vulpecula

12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.

<span class="mw-page-title-main">Kappa Crucis (star)</span> Star in the constellation Crux

Kappa Crucis is a spectroscopic binary star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

2 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located around 1,800 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.43.

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

Xi Orionis is a binary star system in the northeastern part of the constellation of Orion, well above the red giant star Betelgeuse in the sky. It lies next to another blue main-sequence star, Nu Orionis, which is somewhat closer at 520 light-years' distance. The apparent visual magnitude of Xi Orionis is 4.47, which is bright enough to be seen with the naked eye. The distance to this star, as determined using the parallax method, is roughly 610 light-years.

Tau<sup>9</sup> Eridani Binary star in the constellation Eridanus

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<span class="mw-page-title-main">22 Orionis</span> Binary star system in the constellation Orion

22 Orionis is a binary star 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. It is located approximately 1,100 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +28.80

<span class="mw-page-title-main">35 Cygni</span> Binary star in the constellation Cygnus

35 Cygni is a spectroscopic binary star in the constellation Cygnus. Its apparent magnitude is 5.18. Located around 1,000 parsecs (3,300 ly) distant, its primary is a yellow supergiant of spectral type F6Ib, a massive star that has used up its core hydrogen and is now fusing heavier elements.

Phi<sup>1</sup> Orionis Binary star system in the constellation Orion

Phi1 Orionis is a binary star system in the constellation Orion, positioned less than a degree to the south of Meissa. It is visible to the naked eye with an apparent visual magnitude of 4.42. The distance to this system, based upon an annual parallax shift of 3.0 mas, is around 1,090 light-years.

<span class="mw-page-title-main">12 Lacertae</span> Star in the constellation Lacerta

12 Lacertae is a wide binary star system in the northern constellation of Lacerta, located roughly 1,260 light years away from the Sun based on parallax. It is visible to the naked eye as a dim, blue-white hued point of light with a baseline apparent visual magnitude of 5.23. The system is drifting closer to the Earth with a mean heliocentric radial velocity of –12.5. It is a probable member of the I Lacertae OB association.

HD 26670, also known as HR 1305, is a star located in the northern circumpolar constellation of Camelopardalis, the giraffe. The object has been designated as 26 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.70, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the object is estimated to be 491 light years away from the Solar System. It appears to be slowly receding with a heliocentric radial velocity of 0.4 km/s.

<span class="mw-page-title-main">HD 197630</span> Star in the constellation of Microscopium

HD 197630, also known as HR 7933 or rarely 23 G. Microscopii, is a probable astrometric binary located in the southern constellation Microscopium. The visible component is a bluish-white hued star that is faintly visible to the naked eye with an apparent magnitude of 5.47. Based on parallax measurements from the Gaia satellite, the system is estimated to be 328 light years away. However, it is drifting closer with a heliocentric radial velocity of −30 km/s. At its current distance, HD 197630's brightness is diminished by 0.11 magnitudes due to interstellar dust. A 2012 multiplicity survey failed to confirm the velocity variations.

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 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 Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 .
  4. 1 2 3 4 5 Levato, H. (1975), "Rotational velocities and spectral types for a sample of binary systems", Astronomy and Astrophysics, 19: 91, Bibcode:1975A&AS...19...91L.
  5. 1 2 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048 , Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID   59451347, A61.
  6. ↑ Morrell, Nidia; Levato, Hugo (1991), "Spectroscopic Binaries in the Orion OB1 Association", The Astrophysical Journal Supplement Series, 75: 965, Bibcode:1991ApJS...75..965M, doi:10.1086/191556.
  7. 1 2 3 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.
  8. 1 2 3 4 Tetzlaff, N.; et al. (January 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.
  9. 1 2 3 Howe, K. S.; Clarke, C. J. (January 2009), "An analysis of v sin (i) correlations in early-type binaries", Monthly Notices of the Royal Astronomical Society , 392 (1): 448–454, Bibcode:2009MNRAS.392..448H, doi: 10.1111/j.1365-2966.2008.14073.x .
  10. 1 2 3 4 Hohle, M. M.; et al. (2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv: 1003.2335 , Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID   111387483.
  11. ↑ Huang, Wenjin; et al. (October 2010), "A Stellar Rotation Census of B Stars: From ZAMS to TAMS", The Astrophysical Journal, 722 (1): 605–619, arXiv: 1008.1761 , Bibcode:2010ApJ...722..605H, doi:10.1088/0004-637X/722/1/605, S2CID   118532653.
  12. 1 2 "23 Ori". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-06-08.
  13. ↑ Welty, Daniel E.; et al. (October 1999), "The Diffuse Interstellar Clouds toward 23 Orionis", The Astrophysical Journal Supplement Series, 124 (2): 465–501, arXiv: astro-ph/9905234 , Bibcode:1999ApJS..124..465W, doi:10.1086/313263, S2CID   13966185.
  14. ↑ Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925–1929, arXiv: 1205.5238 , Bibcode:2012MNRAS.424.1925C, doi: 10.1111/j.1365-2966.2012.21317.x , S2CID   119120749.
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