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23 Orionis 
Summary
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]
| 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☉ |
| Luminosity | 1,620[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 | |
| 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 | |
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]
References edit
- ^ a b c d e f 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.
- ^ 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.
- ^ a b 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.
- ^ a b c d e Levato, H. (1975), "Rotational velocities and spectral types for a sample of binary systems", Astronomy and Astrophysics, 19: 91, Bibcode:1975A&AS...19...91L.
- ^ a b 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.
- ^ 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.
- ^ a b c 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.
- ^ a b c d 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.
- ^ a b c 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.
- ^ a b c d 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.
- ^ 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.
- ^ a b "23 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-06-08.
- ^ 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.
- ^ 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.