| 词条 | Zeta Tauri |
| 释义 |
| name = ζ Tauri }}{{Starbox image | image={{Location mark |image=Taurus constellation map.svg|alt=|float=center|width=260 |label=|position=right |mark=Red circle.svg|mark_width=10|mark_link=ζ Tau |x=101|y=398 }} |caption=Location of ζ Tauri (circled) }}{{Starbox observe | epoch = J2000.0 | equinox = J2000.0 (ICRS) | constell = Taurus | ra = {{RA|05|37|38.68542}}[1] | dec = {{DEC|+21|08|33.1588}}[1] | appmag_v = 3.010[3] {{nowrap|(2.88 - 3.17[4])}} }}{{Starbox character | class = B2 IIIpe[5] | b-v = −0.164[3] | u-b = −0.749[3] | r-i = | variable = Eclipsing + γ Cas[4] }}{{Starbox astrometry | radial_v = +20[9] | prop_mo_ra = +1.78[1] | prop_mo_dec = −20.07[1] | parallax = 7.33 | p_error = 0.82 | parallax_footnote = [1] | absmag_v = −2.67[13] }}{{Starbox orbit | reference = [5] | period_unitless = 132.987 d | axis_unitless = 1.17 AU | eccentricity = 0.0 (assumed) | inclination = 92.8 | node = −58.0 | periastron = 2,447,025.6 HJD | periarg = 0.0 (assumed) | k1 = 7.43 }}{{Starbox detail | component1 = ζ Tau A | mass = 11.2[5] | radius = 5.5[5] | luminosity = 4,169[17] | temperature = 15,500[17] | gravity = | rotational_velocity = 125[19] | age_myr = {{nowrap|22.5 ± 2.6}}[20] | component2 = ζ Tau B | mass2 = 0.94[5] }}{{Starbox catalog | names = Tianguan, 123 Tauri, HR 1910, HD 37202, BD+21°908, FK5 211, HIP 26451, SAO 77336, GC 6985.[22] }}{{Starbox reference | Simbad = zet+Tau }}{{Starbox end}}Zeta Tauri (ζ Tauri, abbreviated Zeta Tau, ζ Tau) is a binary star in the zodiac constellation of Taurus, the Bull. It has an apparent visual magnitude of 3.0,[3] which is bright enough to be seen with the naked eye. Parallax measurements place it at a distance of roughly 440 light-years from the Sun.[1] The two components are designated Zeta Tauri A (also named Tianguan[1]) and B. Nomenclatureζ Tauri (Latinised to Zeta Tauri) is the star's Bayer designation; it also bears the Flamsteed designation of 123 Tauri. The designations of the two components as Zeta Tauri A and B derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[2]In Chinese astronomy, Zeta Tauri is called 天關, Pinyin: Tiānguān, meaning Celestial Gate, an asterism within the Net (畢宿 Bì Xiù) mansion (see also: Chinese constellation).[3] 天關 (Tiānguān) has also been transliterated as Tien Kwan. (Technically, Tiānguān refers not just to Zeta Tauri but to an asterism of which Zeta Tauri is the main star, alongside 113, 126, 128, 129, 130 and 127 Tauri - see Taurus (Chinese astronomy).[4]) In 2016, the IAU organized a Working Group on Star Names (WGSN)[5] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[6] It approved the name Tianguan for the component Zeta Tauri A on 30 June 2017 and it is now so included in the List of IAU-approved Star Names.[1] PropertiesZeta Tauri is a single-lined spectroscopic binary system, which means the two components are orbiting so close to each other that they can not be resolved with a telescope. Instead, the orbital motion of the primary component is indicated by Doppler effect shifts in the absorption lines in its spectrum. The two components are separated by an estimated distance of about 1.17 astronomical units, or 117% of the distance from the Earth to the Sun. They are following circular orbits with a period of nearly 133 days.[5] Compared to the Sun, the primary, Zeta Tauri A, is an enormous star with more than 11 times the mass and 5–6 times the radius.[5] It is rotating rapidly with a projected rotational velocity of {{nowrap|125 km s−1}}.[19] The companion, Zeta Tauri B, has about 94% the mass of the Sun, although it is unknown whether this is a main sequence star, a neutron star, or a white dwarf. If it is a main sequence star, then the mass indicates it may have a stellar classification of G4.[5] The spectrum of the primary component has a stellar classification of B2 IIIpe.[5] A luminosity class of 'III' indicates this is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence. The 'p' suffix indicates an unspecified chemical peculiarity in the spectrum, while 'e' is used for stars that display emission lines. For Be stars such as this, the emission lines are produced by a rotating circumstellar disk of gas, made of material that has been ejected from the star's outer envelope. An oscillatory pattern in this spectrum is being caused by a single-armed spiral density wave in the disk. The disk may be precessing from the gravitational influence of the secondary component.[5] Zeta Tauri shows variation in its spectrum and brightness. The General Catalogue of Variable Stars lists it as an eclipsing variable and a Gamma Cassiopeiae variable,[4] but it may not be either.[39] See alsoWhite Tiger of The WestReferences1. ^1 {{cite web | url=https://www.iau.org/public/themes/naming_stars/ | title=Naming Stars |publisher=IAU.org |accessdate=16 December 2017}} [7][8][9][10][11][12][13][14][15][16][17]2. ^{{cite arXiv |title=On the naming convention used for multiple star systems and extrasolar planets |date=2010 |eprint=1012.0707 |class=astro-ph.SR |last1= Hessman |first1=F. V. |last2= Dhillon |first2=V. S. |last3= Winget |first3=D. E. |last4= Schreiber |first4=M. R. |last5= Horne |first5=K. |last6= Marsh |first6=T. R. |last7= Guenther |first7=E. |last8= Schwope |first8=A. |last9= Heber |first9=U. }} 3. ^{{zh icon}} AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 24 日 4. ^Richard Hinckley Allen: Star Names — Their Lore and Meaning: Taurus 5. ^{{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|accessdate=22 May 2016}} 6. ^{{cite web | url=https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf | page=5 | title=WG Triennial Report (2015-2018) - Star Names |accessdate=2018-07-14}} 7. ^1 {{citation | title=XHIP: An extended hipparcos compilation | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | journal=Astronomy Letters | volume=38 | issue=5 | pages=331 | year=2012 | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | arxiv=1108.4971 | postscript=. }} 8. ^1 2 3 4 5 6 {{citation| first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 |arxiv = 0708.1752 }} 9. ^1 {{cite book | last1=Evans | first1=D. S. | date=June 20–24, 1966 | editor1-last=Batten | editor1-first=Alan Henry | editor2-last=Heard | editor2-first=John Frederick | contribution=The Revision of the General Catalogue of Radial Velocities | title=Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30 | journal=Determination of Radial Velocities and their Applications | volume=30 | pages=57 | location=University of Toronto | publisher=International Astronomical Union | bibcode=1967IAUS...30...57E }} 10. ^1 2 {{citation | last1=Abt | first1=Helmut A. | last2=Levato | first2=Hugo | last3=Grosso | first3=Monica | title=Rotational velocities of B Stars | journal=The Astrophysical Journal | volume=573 | issue=1 | pages=359–365 |date=July 2002 | doi=10.1086/340590 | bibcode=2002ApJ...573..359A }} 11. ^1 2 3 4 {{citation | display-authors=1 | last1=Harmanec | first1=P. | last2=Horn | first2=J. | last3=Koubsky | first3=P. | last4=Zdarsky | first4=F. | last5=Kriz | first5=S. | last6=Pavlovski | first6=K. | title=Photoelectric photometry at the Hvar Observatory. IV - A study of UBV variations of a group of bright northern Be stars | journal=Bulletin of the Astronomical Institutes of Czechoslovakia, Bulletin | volume=31 | issue=3 | pages=144–159 | date=1980 | bibcode=1980BAICz..31..144H }} 12. ^1 2 3 4 5 6 7 8 9 10 {{citation | display-authors=1 | last1=Schaefer | first1=G. H. | last2=Gies | first2=D. R. | last3=Monnier | first3=J. D. | last4=Richardson | first4=N. D. | last5=Touhami | first5=Y. | last6=Zhao | first6=M. | last7=Che | first7=X. | last8=Pedretti | first8=E. | last9=Thureau | first9=N. | title=Multi-epoch Near-infrared Interferometry of the Spatially Resolved Disk around the Be Star ζ Tau | journal=The Astronomical Journal | volume=140 | issue=6 | pages=1838–1849 |date=December 2010 | doi=10.1088/0004-6256/140/6/1838 | bibcode=2010AJ....140.1838S |arxiv = 1009.5425 }} 13. ^1 2 {{citation | last1=Balona | first1=L. A. | last2=Dziembowski | first2=W. A. | title=Excitation and visibility of high-degree modes in stars | journal=Monthly Notices of the Royal Astronomical Society | volume=309 | issue=1 | pages=221–232 |date=October 1999 | doi=10.1046/j.1365-8711.1999.02821.x | bibcode=1999MNRAS.309..221B }} 14. ^1 {{citation | title=zet Tau -- Be Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Zeta+Tauri | accessdate=2012-01-20 }} 15. ^1 {{citation | last1=Tetzlaff | first1=N. | last2=Neuhäuser | first2=R. | last3=Hohle | first3=M. M. | title=A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun | journal=Monthly Notices of the Royal Astronomical Society | volume=410 | issue=1 | pages=190–200 |date=January 2011 | doi=10.1111/j.1365-2966.2010.17434.x | bibcode=2011MNRAS.410..190T |arxiv = 1007.4883 }} 16. ^1 2 3 {{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}} 17. ^1 {{cite journal|doi=10.1051/aas:1997213 |title=UBV photometry of Be stars at Hvar: 1972?1990 |journal=Astronomy and Astrophysics Supplement Series |volume=125 |pages=75 |year=1997 |last1=Pavlovski |first1=K. |last2=Harmanec |first2=P. |last3=Bozic |first3=H. |last4=Koubský|first4=P. |last5=Hadrava |first5=P. |last6=Kriz |first6=S. |last7=Ruzic |first7=?. |last8=?Tefl |first8=S. |bibcode = 1997A&AS..125...75P }} 18. ^{{cite journal|bibcode=2015A&A...576A.112E|arxiv=1503.00590|title=2.5D global-disk oscillation models of the Be shell star ζ Tauri. I. Spectroscopic and polarimetric analysis|journal=Astronomy & Astrophysics|volume=576|pages=A112|author1=Escolano|first1=C.|last2=Carciofi|first2=A. C.|last3=Okazaki|first3=A. T.|last4=Rivinius|first4=T.|last5=Baade|first5=D.|last6=Štefl|first6=S.|year=2015|doi=10.1051/0004-6361/201425446}}
12 : Bayer objects|B-type giants|Gamma Cassiopeiae variable stars|Eclipsing binaries|Spectroscopic binaries|Taurus (constellation)|Stars with proper names|Flamsteed objects|HR objects|Hipparcos objects|Henry Draper Catalogue objects|Durchmusterung objects |
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