| 词条 | 88 Tauri |
| 释义 |
|name=88 Tauri}}{{Starbox observe 2s |constell=Taurus |epoch=J2000 |component1=88 Tau A |ra1= {{RA|04|35|39.25910}}[1] | dec1= {{DEC|+10|09|38.8396}}[1] |appmag_v1=4.250[2] |component2=88 Tau B |ra2 = {{RA|04|35|35.1775}}[4] |dec2 = {{DEC|+10|10|13.572}}[3] |appmag_v2=7.84[6] }}{{Starbox character |component1=88 Tau A |class=A6m / F5 / G2-3: / G2-3:[7] |b-v=+0.19[4] |u-b=+0.08[4] |component2=88 Tau B |class2=F8V / M?[10] |b-v2=+0.54[5] |u-b2=+0.04[5] }}{{Starbox astrometry |component1=88 Tau A |radial_v=23.97[6] |prop_mo_ra=43.13[1] |prop_mo_dec=-52.71[1] |parallax=20.88 |p_error=0.94 |parallax_footnote=[1] |absmag_v= |component2=88 Tau B |radial_v2=23.97[7] |prop_mo_ra2=51.8[2] |prop_mo_dec2=-49.4[2] }}{{Starbox orbit |reference=[8] |primary=88 Tau Aa |name=88 Tau Ab |period_unitless=6585 ± 12 d |axis_unitless=240.1 ± 5.3 mas 12.17 ± 0.17 AU |eccentricity=0.0715 ± 0.0026 |inclination=69.923 ± 0.048 |periarg=205.7 ± 1.2 |periastron=2455261 ± 22 |node=146.734 ± 0.067 }}{{Starbox orbit |reference=[8] |primary=88 Tau Aa1 |name=88 Tau Aa2 |period_unitless=3.571096 ± 0.000003 d |axis_unitless=1.359 ± 0.034 mas 0.0689 ± 0.0012 AU |eccentricity=0 |inclination=110.6 ± 2.7 |periarg=0 |periastron=2453389.3824 ± 0.0030 |node=287.5 ± 1.8 }}{{Starbox orbit |reference=[8] |primary=88 Tau Ab1 |name=88 Tau Ab2 |period_unitless=7.886969 ± 0.000066 d |axis_unitless=1.967 ± 0.054 mas 0.0997 ± 0.0021 AU |eccentricity=0 |inclination=27.23 ± 0.72 |periarg=0 |periastron=2452507.31 ± 0.02 |node=34.0 ± 8.2 }}{{Starbox orbit |reference=[9] |primary=88 Tau Ba |name=88 Tau Bb |period_unitless=1350 ± 35 d |axis=0.057 |eccentricity=0.663 ± 0.075 |periarg=223 ± 9 |periastron=2450498 ± 34 |k1=3.24 ± 0.44 }}{{Starbox detail |component1=88 Tau Aa1 |mass=2.06 ± 0.11[8] |rotational_velocity=37 ± 2[8] |component2=88 Tau Aa2 |mass2=1.361 ± 0.073[8] |rotational_velocity2=17 ± 2[8] }}{{Starbox detail |no_heading=y |component1=88 Tau Ab1 |mass=1.069 ± 0.069[8] |rotational_velocity=5 ± 3[8] |component2=88 Tau Ab2 |mass2=1.057 ± 0.068[8] |rotational_velocity2=5 ± 3[8] }}{{Starbox detail |no_heading=y |component1=88 Tau Ba |mass=1.2[9] |component2=88 Tau Bb |mass2=>0.15[9] }}{{Starbox catalog |names=ADS 3317, CCDM J04356+1010, WDS J04357+1010AB |component1=88 Tau A |names1=d Tau, 88 Tau, BD+09° 607, HD 29140, HIP 21402, SAO 94026, HR 1458, GC 5599[34] |component2=88 Tau B |names2=BD+09° 606, HD 286909, SAO 94024, GC 5596, TYC 673-1487-1[10] }}{{Starbox reference |Simbad=SHJ+45|sn=88 Tau |Simbad2=88+Tau|sn2=88 Tau A |Simbad3=88+Tau+B|sn3=88 Tau B }}{{Starbox end}}88 Tauri, also known as d Tauri, is a multiple star system in the constellation Taurus (constellation). It has an apparent magnitude of about 4.25, meaning that it is visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is located some 156 light years (48 parsecs) away from the Sun.[1] 88 Tauri is a sextuple star system, meaning that it contains six stars in a hierarchical orbit. The brighter component, 88 Tauri A is a quadruple system consisting of two spectroscopic binaries orbiting each other with an orbital period of 18 years. The fainter component, 88 Tauri B, is also a spectroscopic binary, and is located about 69 arcseconds away, bringing up the total to six stars.[8] Orbit{{chart/start}}{{chart|border=1| | | |,|S1| |S1=Aa1 }}{{chart|border=0| | |,|(|PA| |PA=Period = 3.571d a = 1.36 mas }}{{chart|border=1| | |!|`|S2| |S2=Aa2 }}{{chart|border=0| |,|(| |PB| |PB=Period = 6585d a = 0.24″ }}{{chart|border=1| |!|!|,|S3| |S3=Ab1 }}{{chart|border=0| |(|`|(|PC| |PC=Period = 7.887d a = 1.97 mas }}{{chart|border=1| |!| |`|S4| |S4=Ab2 }}{{chart|border=0| |!| | |PD| |PD=69.6″ separation }}{{chart|border=1| |!| |,|S5| |S5=Ba }}{{chart|border=0| |`|-|(|PE| |PE=Period = 1350d a = 0.057 mas }}{{chart|border=1| | | |`|S6| |S6=Bb }}{{chart/end}} Hierarchy of orbits in the 88 Tauri system 88 Tauri A is a fourth-magnitude star[11] with two components, 88 Tauri Aa and 88 Tauri Ab. 88 Tauri Aa and Ab orbit each other once every 18 years and are separated by about 0.28 arcseconds. Those two components themselves are spectroscopic binaries – binary stars that are too close to be resolved, but can be detected by periodic Doppler shifts in their spectrum. In this case, variability in the radial velocity has been recognized as early as 1907.[12] The Aa pair has an orbital period of 3.57 days and the Ab pair has an orbital period of 7.89 days, and both have circular orbits with low orbital eccentricities.[8] 88 Tauri B, located 69.56 arcseconds away,[10] is a seventh-magnitude star that is also a binary star system. It is another spectroscopic binary whose components (88 Tauri Ba and Bb) orbit each other every 3.69 years.[8] The orbit of 88 Tauri B itself around 88 Tauri A likely takes about 70,000 years.[9] Properties88 Tauri Aa has a spectral type of A6m,[8] indicating that it is an A-type star. The "m" in its spectral type means that it is an Am star,[8] also known as a metallic-line star. These types of stars have spectra indicating varying amounts of metals, like iron.[13] The rest of the stars in 88 Tauri A have spectral types ranging from F5 to G2-3, meaning that they are regular F-type or G-type main-sequence stars. The spectral types for 88 Tauri Ab1 and Ab2 are less certain, because their spectral lines are weaker, hence the colon after G2. Aa1 does not appears to be rotating synchronously with its companion (nor does it have a convective atmosphere), unlike Aa2. (It is not known if the two stars of 88 Tauri Ab are in synchronous rotation with each other, because of the relatively high errors in their measurements.)[8] 88 Tauri B consists of a F-type main sequence star, with another low-mass star.[9] The mass of the smaller component is at least 0.15 solar mass, so it is most likely a red dwarf.[9] References1. ^1 2 3 4 5 {{cite journal | title=Validation of the new Hipparcos reduction | url=http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | date=2007 | arxiv=0708.1752 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 }} {{Stars of Taurus}}2. ^1 2 {{cite journal|title=The Tycho-2 catalogue of the 2.5 million brightest stars|author1=Høg, E.|display-authors=etal|date=2000|journal=Astronomy and Astrophysics|volume=355|pages=L27–L30|bibcode=2000A&A...355L..27H}} 3. ^1 {{cite journal|author1=Hog, E.|date=1998|title=The Tycho Reference Catalogue|journal=Astronomy and Astrophysics|volume=335|bibcode=1998A&A...335L..65H}} 4. ^1 2 {{cite journal|author1=Feinstein, A.|title=Photoelectric UBVRI observations of Am stars|date=1974|journal=Astronomical Journal|volume=79|page=1290|bibcode=1974AJ.....79.1290F|doi=10.1086/111675}} (Accessed using SIMBAD) 5. ^1 {{cite journal| author1=Mermilliod, J.-C.|title=Compilation of Eggen's UBV data, transformed to UBV (unpublished)|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1986EgUBV........0M&db_key=AST&nosetcookie=1|date=1986|bibcode= 1986EgUBV........0M }} 6. ^{{cite journal|bibcode=2004A&A...424..727P|doi=10.1051/0004-6361:20041213|arxiv=astro-ph/0406573|title=SB9: The ninth catalogue of spectroscopic binary orbits|journal=Astronomy and Astrophysics|volume=424|issue=2|pages=727|date=2004|author1=Pourbaix, D.|author2=Tokovinin, A. A.|author3=Batten, A. H.|author4=Fekel, F. C.|author5=Hartkopf, W. I.|author6=Levato, H.|author7=Morrell, N. I.|author8=Torres, G.|author9=Udry, S.}} 7. ^{{cite journal|title=Statistics of spectroscopic sub-systems in visual multiple stars|author1=Tokovinin, A. A.|author2=Smekhov, M. G.|journal=Astronomy and Astrophysics|volume=382|pages=118–123|date=2002|bibcode=2002A&A...382..118T|doi=10.1051/0004-6361:20011586}} 8. ^1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 {{cite journal|title=The Orbits of the Quadruple Star System 88 Tauri A from PHASES Differential Astrometry and Radial Velocity|author1=Lane, Benjamin F.|author2=Muterspaugh, Matthew W.|author3=Fekel, Francis C.|author4=Williamson, Michael|author5=Browne, Stanley|author6=Konacki, Maciej|author7=Burke, Bernard F.|author8=Colavita, M. M.|author9=Kulkarni, S. R.|author10=Shao, M.|journal=The Astrophysical Journal|volume=669|issue=2|pages=1209–1219|date=2007|bibcode=2007ApJ...669.1209L|doi=10.1086/520877|arxiv=0710.2127}} 9. ^1 2 3 4 5 6 {{cite journal|title=New spectroscopic components in multiple systems. IV|author1=Tokovinin, A. A.|author2=Gorynya, N. A.|journal=Astronomy and Astrophysics|volume=374|pages=227–234|date=2001|bibcode=2001A&A...374..227T|doi=10.1051/0004-6361:20010714}} 10. ^1 {{cite simbad|title=88 Tau B|access-date=18 February 2017}} 11. ^1 {{cite simbad|title=88 Tau|access-date=16 February 2017}} 12. ^{{cite journal|title=The orbit of 88 D Tauri|author=Daniel, Zaccheus|journal=Publications of the Allegheny Observatory of the University of Pittsburgh|volume=3|number=12|date=1916|bibcode=1916PAllO...3...93D}} 13. ^Am star, The Internet Encyclopedia of Science, David Darling. Accessed on line August 14, 2008. 10 : Taurus (constellation)|Flamsteed objects|Spectroscopic binaries|Multiple star systems|Bayer objects|HR objects|Henry Draper Catalogue objects|Hipparcos objects|Durchmusterung objects|Am stars |
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