[{"@context":"http:\/\/schema.org\/","@type":"BlogPosting","@id":"https:\/\/wiki.edu.vn\/en\/wiki24\/2022\/06\/21\/hd-83446-wikipedia\/#BlogPosting","mainEntityOfPage":"https:\/\/wiki.edu.vn\/en\/wiki24\/2022\/06\/21\/hd-83446-wikipedia\/","headline":"HD 83446 – Wikipedia","name":"HD 83446 – Wikipedia","description":"From Wikipedia, the free encyclopedia Star in the constellation Vela This article is about M Velorum. For m Velorum, see","datePublished":"2022-06-21","dateModified":"2022-06-21","author":{"@type":"Person","@id":"https:\/\/wiki.edu.vn\/en\/wiki24\/author\/lordneo\/#Person","name":"lordneo","url":"https:\/\/wiki.edu.vn\/en\/wiki24\/author\/lordneo\/","image":{"@type":"ImageObject","@id":"https:\/\/secure.gravatar.com\/avatar\/c9645c498c9701c88b89b8537773dd7c?s=96&d=mm&r=g","url":"https:\/\/secure.gravatar.com\/avatar\/c9645c498c9701c88b89b8537773dd7c?s=96&d=mm&r=g","height":96,"width":96}},"publisher":{"@type":"Organization","name":"Enzyklop\u00e4die","logo":{"@type":"ImageObject","@id":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","url":"https:\/\/wiki.edu.vn\/wiki4\/wp-content\/uploads\/2023\/08\/download.jpg","width":600,"height":60}},"image":{"@type":"ImageObject","@id":"https:\/\/en.wikipedia.org\/wiki\/Special:CentralAutoLogin\/start?type=1x1","url":"https:\/\/en.wikipedia.org\/wiki\/Special:CentralAutoLogin\/start?type=1x1","height":"1","width":"1"},"url":"https:\/\/wiki.edu.vn\/en\/wiki24\/2022\/06\/21\/hd-83446-wikipedia\/","wordCount":2942,"articleBody":"From Wikipedia, the free encyclopediaStar in the constellation VelaThis article is about M Velorum. For m Velorum, see HD 85622.HD 83446 is a probable astrometric binary[10]star system in the constellation Vela. It is visible to the naked eye with an apparent visual magnitude of 4.34.[2] Based upon an annual parallax shift of 30.5\u00a0mas,[1] it is located 107.1\u00a0light years from the Sun. The system is moving further away with a heliocentric radial velocity of +18\u00a0km\/s.[6]The visible component is an A-type main-sequence star with a stellar classification of A7\u00a0V.[4] Observations with the BRITE constellation led to this star’s identification as a Delta Scuti variable with pulsation frequencies of 31.0806 and 34.2098 cycles per day, corresponding to periods of 46.3 and 42.1 minutes, respectively.[5] It has a high rate of spin with a projected rotational velocity of 155\u00a0km\/s, which is giving the star an oblate shape with an equatorial bulge that is 6% larger than the polar radius.[8] The star is roughly 453[7]\u00a0million years old with 1.8[7] times the mass of the Sun. It is radiating 16[2] times the Sun’s luminosity from its photosphere at an effective temperature of 8,331\u00a0K.[7]References[edit]^ a b c d e f Brown, A. G. A.;  et\u00a0al. (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 e f 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\u00a0119257644.^ Zorec, J.; Royer, F. (2012), “Rotational velocities of A-type stars. IV. Evolution of rotational velocities”, Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A…537A.120Z, doi:10.1051\/0004-6361\/201117691, S2CID\u00a055586789.^ a b Gray, R. O.;  et\u00a0al. (July 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\u2013170, arXiv:astro-ph\/0603770, Bibcode:2006AJ….132..161G, doi:10.1086\/504637, S2CID\u00a0119476992.^ a b Zwintz, K. (September 2017), “A BRITE view on \u03b4 Scuti and \u03b3 Doradus stars”,  in Zwintz, Konnstanze; Poretti, Ennio (eds.), Second BRITE-Constellation Science Conference: Small satellites\u2014big science, Proceedings of the Polish Astronomical Society volume 5, held 22-26 August, 2016 in Innsbruck, Austria, vol.\u00a05, Bartycka 18, 00-716 Warsaw, Poland: Polish Astronomical Society, pp.\u00a0228\u2013235, arXiv:1611.04917, Bibcode:2017sbcs.conf..228Z{{citation}}:  CS1 maint: location (link)^ 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\u00a059451347, A61.^ a b c d e f g Gullikson, Kevin;  et\u00a0al. (2016), “The Close Companion Mass-Ratio Distribution of Intermediate-Mass Stars”, The Astronomical Journal, 152 (2): 40, arXiv:1604.06456, Bibcode:2016AJ….152…40G, doi:10.3847\/0004-6256\/152\/2\/40, S2CID\u00a0119179065.^ a b Belle, G. T. (2012), “Interferometric observations of rapidly rotating stars”, The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20…51V, doi:10.1007\/s00159-012-0051-2, S2CID\u00a0119273474.^ “HD 83446”. SIMBAD. Centre de donn\u00e9es astronomiques de Strasbourg. Retrieved 2018-08-08.^ 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\u00a014878976.  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