| 词条 | VFTS 352 |
| 释义 |
| name = VFTS 352 }}{{Starbox image | image = | caption = Artist's rendering of VFTS 352 binary star | credit = ESO/L. Calçada }}{{Starbox observe | epoch = J2000 | constell = Dorado | ra = {{RA|05|38|28.456}}[1] | dec = {{DEC|-69|11|19.18}}[1] | appmag_v = 14.38[2] }}{{Starbox character | type=Main Sequence[4] | class=O4.5 V(n)((fc)):z: + O5.5 V(n)((fc)):z:[3] | b-v=−0.10[2] | u-b= | variable= }}{{Starbox astrometry | dist_ly = 164,000 | dist_pc = 50,000[7] | absmag_v= | absmag_bol= | radial_v=262.8[7] }}{{Starbox orbit | reference = [7] | primary = VFTS 3521 | name = VFTS 3522 | period = | period_unitless = 1.124 days | axis = | axis_unitless = {{solar radius|17.55}} | eccentricity = 0 | inclination = 55.60 | node = 3.584 | periastron = | periarg = | periarg_primary = | k1 = 324.9 | k2 = 315.6 }}{{Starbox detail | source = [7] | component1 = VFTS 3521 | mass = 28.63 ± 0.30 | radius = 7.22 ± 0.02 | gravity = 4.18 ± 0.01 | luminosity = 180,000 | luminosity_visual = | temperature = 42,540 ± 280 | age_myr = 1 | rotation = | component2 = VFTS 3522 | mass2 = 28.85 ± 0.30 | radius2 = 7.25 ± 0.02 | gravity2 = 4.18 ± 0.01 | luminosity2 = 150,000 | luminosity_visual2 = | temperature2 = 41,120 ± 290 | age_myr2 = 1 | rotation2 = }}{{Starbox catalog | names = VFTS 352, 2MASS J05382845-6911191, IRSF J05382846-6911192 }}{{Starbox reference | Simbad = VFTS+352 }}{{Starbox end}}VFTS 352 is a contact binary star system {{convert|160000|ly|pc}} away in the Tarantula Nebula, which is part of the Large Magellanic Cloud.[4] It is the most massive and earliest spectral type overcontact system known.[5] The discovery of this O-type binary star system made use of the European Southern Observatory's Very Large Telescope,[6] and the description was published on 13 October 2015.[5] VFTS 352 is composed of two very hot (40,000 °C), bright and massive stars of equal size that orbit each other in little more than a day. The stars are so close that their atmosphere overlap.[6] Extreme stars like the two components of VFTS 352, are thought to be the main producers of elements such as oxygen.[6] The future of VFTS 352 is uncertain, and there are two possible scenarios. If the two stars merge, a very rapidly rotating star will be produced. If it keeps spinning rapidly it might end its life in a long-duration gamma-ray burst. In a second hypothetical scenario, the components would end their lives in supernova explosions, forming a close binary black hole system, hence a potential gravitational wave source through black hole–black hole merger.[5] See also
References1. ^1 {{cite journal|bibcode=2003yCat.2246....0C|title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)|journal=VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C|volume=2246|author1=Cutri|first1=R. M.|last2=Skrutskie|first2=M. F.|last3=Van Dyk|first3=S.|last4=Beichman|first4=C. A.|last5=Carpenter|first5=J. M.|last6=Chester|first6=T.|last7=Cambresy|first7=L.|last8=Evans|first8=T.|last9=Fowler|first9=J.|last10=Gizis|first10=J.|last11=Howard|first11=E.|last12=Huchra|first12=J.|last13=Jarrett|first13=T.|last14=Kopan|first14=E. L.|last15=Kirkpatrick|first15=J. D.|last16=Light|first16=R. M.|last17=Marsh|first17=K. A.|last18=McCallon|first18=H.|last19=Schneider|first19=S.|last20=Stiening|first20=R.|last21=Sykes|first21=M.|last22=Weinberg|first22=M.|last23=Wheaton|first23=W. A.|last24=Wheelock|first24=S.|last25=Zacarias|first25=N.|year=2003}} {{Stars of Dorado}}2. ^1 {{Cite journal |title=The VLT-FLAMES Tarantula Survey. I. Introduction and observational overview |journal=Astronomy & Astrophysics |last1=Evans |first1=C. J. |last2=Taylor |first2=W. D. |last3=Hénault-Brunet |first3=V. |last4=Sana |first4=H. |last5=De Koter |first5=A. |last6=Simón-Díaz |first6=S. |last7=Carraro |first7=G. |last8=Bagnoli |first8=T. |last9=Bastian |first9=N. |last10=Bestenlehner |first10=J. M. |last11=Bonanos |first11=A. Z. |last12=Bressert |first12=E. |last13=Brott |first13=I. |last14=Campbell |first14=M. A. |last15=Cantiello |first15=M. |last16=Clark |first16=J. S. |last17=Costa |first17=E. |last18=Crowther |first18=P. A. |last19=De Mink |first19=S. E. |last20=Doran |first20=E. |last21=Dufton |first21=P. L. |last22=Dunstall |first22=P. R. |last23=Friedrich |first23=K. |last24=Garcia |first24=M. |last25=Gieles |first25=M. |last26=Gräfener |first26=G. |last27=Herrero |first27=A. |last28=Howarth |first28=I. D. |last29=Izzard |first29=R. G. |last30=Langer |first30=N. |last31=Lennon |first31=D. J. |last32=Maíz Apellániz |first32=J. |last33=Markova |first33=N. |last34=Najarro |first34=F. |last35=Puls |first35=J. |last36=Ramirez |first36=O. H. |last37=Sabín-Sanjulián |first37=C. |last38=Smartt |first38=S. J. |last39=Stroud |first39=V. E. |last40=van Loon |first40=J. Th. |last41=Vink |first41=J. S. |last42=Walborn |first42=N. R. |display-authors=5 |volume=530 |pages=A108 |date=June 2011 |doi=10.1051/0004-6361/201116782 |bibcode=2011A&A...530A.108E |arxiv=1103.5386}} 3. ^1 {{cite journal|bibcode=2014A&A...564A..40W|arxiv=1402.6969|title=The VLT-FLAMES Tarantula Survey. XIV. The O-type stellar content of 30 Doradus|journal=Astronomy & Astrophysics|volume=564|pages=A40|author1=Walborn|first1=N. R.|last2=Sana|first2=H.|last3=Simón-Díaz|first3=S.|last4=Maíz Apellániz|first4=J.|last5=Taylor|first5=W. D.|last6=Evans|first6=C. J.|last7=Markova|first7=N.|last8=Lennon|first8=D. J.|last9=De Koter|first9=A.|year=2014|doi=10.1051/0004-6361/201323082}} 4. ^{{cite web | title=Final Kiss of Two Stars Heading for Catastrophe |url=http://www.eso.org/public/news/eso1540/ |date=15 October 2015 |work=EPB |accessdate=17 October 2015 }} 5. ^1 2 3 4 5 6 {{cite journal|doi=10.1088/0004-637X/812/2/102|bibcode=2015ApJ...812..102A|arxiv=1509.08940|title=Discovery of the Massive Overcontact Binary Vfts 352: Evidence for Enhanced Internal Mixing|journal=The Astrophysical Journal|volume=812|issue=2|pages=102|year=2015|last1=Almeida|first1=L. A.|last2=Sana|first2=H.|last3=Mink|first3=S. E. de|last4=Tramper|first4=F.|last5=Soszyn´Ski|first5=I.|last6=Langer|first6=N.|last7=Barbá|first7=R. H.|last8=Cantiello|first8=M.|last9=Damineli|first9=A.|last10=Koter|first10=A. de|last11=Garcia|first11=M.|last12=Gräfener|first12=G.|last13=Herrero|first13=A.|last14=Howarth|first14=I.|last15=Apellániz|first15=J. Maíz|last16=Norman|first16=C.|last17=Ramírez-Agudelo|first17=O. H.|last18=Vink|first18=J. S.}} 6. ^1 2 {{cite news |url=http://astronomynow.com/2015/10/21/final-kiss-of-two-stars-heading-for-catastrophe/ |title=Final kiss of two stars heading for catastrophe |work=Astronomy Now |date=21 October 2015 |accessdate=2015-10-21 }} 8 : Stars in the Large Magellanic Cloud|Binary stars|O-type main-sequence stars|Tarantula Nebula|Extragalactic stars|2MASS objects|Dorado (constellation)|Emission-line stars |
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