The traditional name Furud or Phurud derives from the Arabic ألفرود al-furūd "the solitary ones". This was an appellation early Arab poets used for a number of anonymous stars. Later Arabian astronomers attempted to identify the name with particular stars, principally in the modern constellations Centaurus and Colomba. The stars of Colomba were assigned to Canis Majoris in the Almagest, leading to more recent assignment of the name for Zeta Canis Majoris.[15]
Al Sufi referred to these stars as ألأغربة al-ʼaghribah "the ravens".[16]
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[17] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[18] included a table of the first two batches of names approved by the WGSN; which included Furud for this star.
Properties
The binary nature of this system was first noted by G. E. Paddock based on observations made in 1906 from the D. O. Mills Observatory in Chile.[19] It was confirmed in 1909 by S. A. Mitchell, using radial velocity measurements made by F. E. Harpham in 1908.[20] It is a single-lined spectroscopic binary system, which means that the pair have not been individually resolved with a telescope, but the gravitational perturbations of an unseen astrometric companion can be discerned by shifts in the spectrum of the primary caused by the Doppler effect. The pair orbit around their common center of mass once every 675 days with an eccentricity of 0.57.[8]
The primary component is a large star with nearly four[10] times the Sun's radius and almost eight[9] times the mass of the Sun. It has a stellar classification of B2.5 V,[3] which means it is a B-type main sequence star that is generating energy through the nuclear fusion of hydrogen at its core. The star is emitting 3,603[11] times the luminosity of the Sun and is a suspected Beta Cephei variable.[4] This energy is being radiated from its outer envelope at an effective temperature of about 18,700 K,[11] giving it the blue-white hue of a B-type star.[21] It is relatively young for a star, with an estimated age of 32 million years.[9]
Zeta Canis Majoris is located close to the solar antapex.
References
^ abcdefvan Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
^ abcdCousins, A. W. J. (1972), "UBV Photometry of Some Very Bright Stars", Monthly Notes of the Astronomical Society of Southern Africa, 31: 69, Bibcode:1972MNSSA..31...69C
^ abHouk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 3, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1982mcts.book.....H
^ abTelting, J. H.; et al. (June 2006), "A high-resolution spectroscopy survey of β Cephei pulsations in bright stars", Astronomy and Astrophysics, 452 (3): 945–953, Bibcode:2006A&A...452..945T, doi:10.1051/0004-6361:20054730
^ abEvans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E
^Pourbaix, D.; et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits", Astronomy & Astrophysics, 424: 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
^ abAbt, Helmut A. (August 2005), "Observed Orbital Eccentricities", The Astrophysical Journal, 629 (1): 507–511, Bibcode:2005ApJ...629..507A, doi:10.1086/431207
^ abcdTetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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
^ abcUnderhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society, 189 (3): 601–605, Bibcode:1979MNRAS.189..601U, doi:10.1093/mnras/189.3.601
^ abcdHohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349–360, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483
^Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590
^"zet CMa -- Cepheid variable Star", SIMBAD Astronomical Object Database, Centre de Données astronomiques de Strasbourg, retrieved 2012-02-15
^"IAU Catalog of Star Names". Retrieved 28 July 2016.
^Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN978-1-931559-44-7.
^Allen, R. H. (1963), Star Names: Their Lore and Meaning (Reprint ed.), New York: Dover Publications Inc, p. 130, ISBN0-486-21079-0, retrieved 2010-12-12
^"IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
^"Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
^Curtis, H. D. (April 1909), "Five stars having variable radial velocities", Astrophysical Journal, 29: 229–231, Bibcode:1909ApJ....29..229C, doi:10.1086/141645.
^Mitchell, S. A. (October 1909), "Seven spectroscopic binaries", Astrophysical Journal, 30: 239–242, Bibcode:1909ApJ....30..239M, doi:10.1086/141699.
^"The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16
External links
Kaler, James B., "FURUD (Zeta Canis Majoris)", Stars, University of Illinois, retrieved 2012-02-16
March 11, 2023
zeta, canis, majoris, canis, majoris, also, named, furud, jʊər, binary, star, system, southern, constellation, canis, major, this, system, apparent, visual, magnitude, making, brighter, stars, constellation, hence, readily, visible, naked, parallax, measuremen. Zeta Canis Majoris or z Canis Majoris also named Furud ˈ f jʊer e d 14 is a binary star system in the southern constellation of Canis Major This system has an apparent visual magnitude of 3 0 2 making it one of the brighter stars in the constellation and hence readily visible to the naked eye Parallax measurements from the Hipparcos mission yield a distance estimate of around 362 ly 111 pc from the Sun 1 It is drifting further away with a radial velocity of 32 km s 5 Zeta Canis MajorisLocation of z Canis Majoris circled Observation dataEpoch J2000 0 Equinox J2000 0Constellation Canis MajorRight ascension 06h 20m 18 79204s 1 Declination 30 03 48 1202 1 Apparent magnitude V 3 025 2 CharacteristicsSpectral type B2 5 V 3 U B color index 0 71 2 B V color index 0 195 2 Variable type Suspected b Cep 4 AstrometryRadial velocity Rv 32 2 5 km sProper motion m RA 7 32 1 mas yr Dec 4 03 1 mas yrParallax p 9 00 0 13 mas 1 Distance362 5 ly 111 2 pc Absolute magnitude MV 2 21 6 Orbit 7 8 Period P 675 daysEccentricity e 0 57Periastron epoch T 2 416 508 JDArgument of periastron w secondary 207 Semi amplitude K1 primary 13 5 km sDetailsMass7 7 0 2 9 M Radius3 9 10 R Luminosity3 603 11 L Surface gravity log g 4 0 10 cgsTemperature18 700 11 KRotational velocity v sin i 25 12 km sAge32 0 0 4 9 MyrOther designationsFurud Phurud z CMa Zeta CMa 1 Canis Majoris CD 30 3038 FK5 240 HD 44402 HIP 30122 HR 2282 SAO 196698 13 Database referencesSIMBADdata Contents 1 Name 2 Properties 3 References 4 External linksName Editz Canis Majoris Latinized from Zeta Canis Majoris is the star s Bayer designation assigned by the German astronomer Johann Bayer in 1603 The traditional name Furud or Phurud derives from the Arabic ألفرود al furud the solitary ones This was an appellation early Arab poets used for a number of anonymous stars Later Arabian astronomers attempted to identify the name with particular stars principally in the modern constellations Centaurus and Colomba The stars of Colomba were assigned to Canis Majoris in the Almagest leading to more recent assignment of the name for Zeta Canis Majoris 15 Al Sufi referred to these stars as ألأغربة al ʼaghribah the ravens 16 In 2016 the International Astronomical Union organized a Working Group on Star Names WGSN 17 to catalog and standardize proper names for stars The WGSN s first bulletin of July 2016 18 included a table of the first two batches of names approved by the WGSN which included Furud for this star Properties EditThe binary nature of this system was first noted by G E Paddock based on observations made in 1906 from the D O Mills Observatory in Chile 19 It was confirmed in 1909 by S A Mitchell using radial velocity measurements made by F E Harpham in 1908 20 It is a single lined spectroscopic binary system which means that the pair have not been individually resolved with a telescope but the gravitational perturbations of an unseen astrometric companion can be discerned by shifts in the spectrum of the primary caused by the Doppler effect The pair orbit around their common center of mass once every 675 days with an eccentricity of 0 57 8 The primary component is a large star with nearly four 10 times the Sun s radius and almost eight 9 times the mass of the Sun It has a stellar classification of B2 5 V 3 which means it is a B type main sequence star that is generating energy through the nuclear fusion of hydrogen at its core The star is emitting 3 603 11 times the luminosity of the Sun and is a suspected Beta Cephei variable 4 This energy is being radiated from its outer envelope at an effective temperature of about 18 700 K 11 giving it the blue white hue of a B type star 21 It is relatively young for a star with an estimated age of 32 million years 9 Zeta Canis Majoris is located close to the solar antapex References Edit a b c d e f van Leeuwen F November 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b c d Cousins A W J 1972 UBV Photometry of Some Very Bright Stars Monthly Notes of the Astronomical Society of Southern Africa 31 69 Bibcode 1972MNSSA 31 69C a b Houk Nancy 1979 Michigan catalogue of two dimensional spectral types for the HD stars vol 3 Ann Arbor Michigan Dept of Astronomy University of Michigan Bibcode 1982mcts book H a b Telting J H et al June 2006 A high resolution spectroscopy survey of b Cephei pulsations in bright stars Astronomy and Astrophysics 452 3 945 953 Bibcode 2006A amp A 452 945T doi 10 1051 0004 6361 20054730 a b Evans D S June 20 24 1966 The Revision of the General Catalogue of Radial Velocities in Batten Alan Henry Heard John Frederick eds Determination of Radial Velocities and their Applications Proceedings from IAU Symposium no 30 vol 30 University of Toronto International Astronomical Union p 57 Bibcode 1967IAUS 30 57E 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 Pourbaix D et al 2004 SB9 The Ninth Catalogue of Spectroscopic Binary Orbits Astronomy amp Astrophysics 424 727 732 arXiv astro ph 0406573 Bibcode 2004A amp A 424 727P doi 10 1051 0004 6361 20041213 S2CID 119387088 a b Abt Helmut A August 2005 Observed Orbital Eccentricities The Astrophysical Journal 629 1 507 511 Bibcode 2005ApJ 629 507A doi 10 1086 431207 a b c d Tetzlaff N Neuhauser R Hohle M M 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 Underhill A B et al November 1979 Effective temperatures angular diameters distances and linear radii for 160 O and B stars Monthly Notices of the Royal Astronomical Society 189 3 601 605 Bibcode 1979MNRAS 189 601U doi 10 1093 mnras 189 3 601 a b c d Hohle M M Neuhauser R Schutz B F April 2010 Masses and luminosities of O and B type stars and red supergiants Astronomische Nachrichten 331 4 349 360 arXiv 1003 2335 Bibcode 2010AN 331 349H doi 10 1002 asna 200911355 S2CID 111387483 Abt Helmut A Levato Hugo Grosso Monica July 2002 Rotational Velocities of B Stars The Astrophysical Journal 573 1 359 365 Bibcode 2002ApJ 573 359A doi 10 1086 340590 zet CMa Cepheid variable Star SIMBAD Astronomical Object Database Centre de Donnees astronomiques de Strasbourg retrieved 2012 02 15 IAU Catalog of Star Names Retrieved 28 July 2016 Kunitzsch Paul Smart Tim 2006 A Dictionary of Modern star Names A Short Guide to 254 Star Names and Their Derivations 2nd rev ed Cambridge Massachusetts Sky Pub ISBN 978 1 931559 44 7 Allen R H 1963 Star Names Their Lore and Meaning Reprint ed New York Dover Publications Inc p 130 ISBN 0 486 21079 0 retrieved 2010 12 12 IAU Working Group on Star Names WGSN Retrieved 22 May 2016 Bulletin of the IAU Working Group on Star Names No 1 PDF Retrieved 28 July 2016 Curtis H D April 1909 Five stars having variable radial velocities Astrophysical Journal 29 229 231 Bibcode 1909ApJ 29 229C doi 10 1086 141645 Mitchell S A October 1909 Seven spectroscopic binaries Astrophysical Journal 30 239 242 Bibcode 1909ApJ 30 239M doi 10 1086 141699 The Colour of Stars Australia Telescope Outreach and Education Commonwealth Scientific and Industrial Research Organisation December 21 2004 retrieved 2012 01 16External links EditKaler James B FURUD Zeta Canis Majoris Stars University of Illinois retrieved 2012 02 16 Retrieved from https en wikipedia org w index php title Zeta Canis Majoris amp oldid 1079514014, wikipedia, wiki, book, books, library,
