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词条 Melnick 34
释义

  1. Binary

  2. Physical characteristics

  3. Evolution

  4. References

  5. External links

{{Starbox begin
| name = BAT99-116
}}{{Starbox image
| image =
| caption = Melnick 34
| credit = Wide Field and Planetary Camera of the Hubble Space Telescope
}}{{Starbox observe
| epoch = J2000.0
| equinox = J2000.0
| constell = Dorado
| ra = {{RA|5|38|44.26}}[1]
| dec = {{DEC|−69|06|05.88}}[1]
| appmag_v = 13.09[1]
}}{{Starbox character
| type = Wolf–Rayet star
| class = WN5h:a[4]
| b-v=+0.25[1]
}}{{Starbox astrometry
| radial_v =
| prop_mo_ra =
| prop_mo_dec =
| parallax =
| p_error =
| parallax_footnote =
| dist_ly = 163,000
| dist_pc = 49,970[2]
| absmag_v = -7.9[1]
}}{{Starbox detail
| mass = 179[3]
| radius = 20[4]
| gravity =
| luminosity = 7,079,000[10]
| temperature = 53,000[1]
| metal =
| rotation =
| age_myr = ~1.7[5]
}}{{Starbox catalog
| names= BAT99 116, [HSH95] 8, Melnick 34, 2MASS J05384424-6906058, Brey 84
}}{{Starbox reference
| Simbad = BAT99+116
| ARICNS =
}}{{Starbox end}}

BAT99-116 (commonly called Melnick 34 or Mk34) is a massive luminous Wolf–Rayet star near R136 in the 30 Doradus complex (also known as the Tarantula Nebula) in the Large Magellanic Cloud.

Binary

Melnick 34 is thought to be a binary star with an orbital period of 155 days. It shows high x-ray luminosity characteristic of colliding-wind binaries, and periodic variations in luminosity, spectral absorption, and the x-ray brightness.[6]

Physical characteristics

Mk34 is a Wolf–Rayet star with surface temperature over 50,000 K .[4][1] It is estimated that at its birth the star was around {{Solar mass|275}}.[7] It has a powerful stellar wind and despite its young age it has already shed a large fraction of its initial mass.[3] Because the Mk 34 system includes two massive luminous stars that cannot be resolved, estimates of the temperature, luminosity, and mass of each are highly uncertain.[4]

Evolution

Mk34 is currently burning hydrogen in its core, although it shows strong helium and nitrogen emission due to convection of fusion products from the core to the surface. It is expected that it will evolve quickly to a hydrogen-free Wolf-Rayet star, possibly with a short time as a blue hypergiant and luminous blue variable. It will then shed more and more of its outer layers, ultimately becoming a WO star close to 200,000 K before collapsing, producing a type Ic supernova and leaving behind a black hole.[8]

{{Portal|Astronomy|Space}}

References

1. ^1 2 3 4 5 6 {{cite journal |last1=Doran|first1=E. I. |last2=Crowther|first2=P. A. |last3=de Koter|first3=A. |last4=Evans|first4=C. J. |last5=McEvoy|first5=C. |last6=Walborn|first6=N. R. |last7=Bastian|first7=N. |last8=Bestenlehner|first8=J. M. |last9=Grafener|first9=G. |last10=Herrero|first10=A. |last11=Kohler|first11=K. |last12=Maiz Apellaniz|first12=J. |last13=Najarro|first13=F. |last14=Puls|first14=J. |last15=Sana|first15=H. |last16=Schneider|first16=F. R. N. |last17=Taylor|first17=W. D. |last18=van Loon|first18=J. Th. |last19=Vink|first19=J. S. |year=2013 |title=The VLT-FLAMES Tarantula Survey - XI. A census of the hot luminous stars and their feedback in 30 Doradus |journal=Astronomy & Astrophysics |volume=558 |issue= |pages=134 |arxiv=1308.3412 |bibcode=2013A&A...558A.134D |doi=10.1051/0004-6361/201321824}}
2. ^{{cite journal|last=Pietrzyński|first=G|author2=D. Graczyk |author3=W. Gieren |author4=I. B. Thompson |author5=B. Pilecki |author6=A. Udalski |author7=I. Soszyński |display-authors=etal |title=An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent|journal=Nature|date=7 March 2013|volume=495|issue=7439|pages=76–79|doi=10.1038/nature11878|pmid=23467166|arxiv = 1303.2063 |bibcode = 2013Natur.495...76P }}
3. ^1 {{cite journal|bibcode=2002ApJ...574..762P|arxiv=astro-ph/0106109|title=A Dozen Colliding-Wind X-Ray Binaries in the Star Cluster R136 in the 30 Doradus Region|journal=The Astrophysical Journal|volume=574|issue=2|pages=762|author1=Portegies Zwart|first1=Simon F.|last2=Pooley|first2=David|last3=Lewin|first3=Walter H. G.|year=2002|doi=10.1086/340996}}
4. ^1 2 3 {{Cite journal | doi = 10.1051/0004-6361/201322696| title = The Wolf-Rayet stars in the Large Magellanic Cloud| journal = Astronomy & Astrophysics| volume = 565| pages = A27| year = 2014| last1 = Hainich | first1 = R.| last2 = Rühling | first2 = U.| last3 = Todt | first3 = H.| last4 = Oskinova | first4 = L. M.| last5 = Liermann | first5 = A.| last6 = Gräfener | first6 = G.| last7 = Foellmi | first7 = C.| last8 = Schnurr | first8 = O.| last9 = Hamann | first9 = W. -R. | arxiv = 1401.5474| bibcode = 2014A&A...565A..27H}}
5. ^{{Cite journal |last1=Crowther |first1=P. A. |last2=Schnurr |first2=O. |last3=Hirschi |first3=R. |last4=Yusof |first4=N. |last5=Parker |first5=R. J. |last6=Goodwin |first6=S. P. |last7=Kassim |first7=H. A. |year=2010 |title=The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit |journal=Monthly Notices of the Royal Astronomical Society |volume=408 |issue=2 |pages=731 |arxiv=1007.3284 |bibcode=2010MNRAS.408..731C |doi=10.1111/j.1365-2966.2010.17167.x }}
6. ^{{cite journal|doi=10.1093/mnras/stx2879|title=The 155-day X-ray cycle of the very massive Wolf-Rayet star Melnick 34 in the Large Magellanic Cloud|journal=Monthly Notices of the Royal Astronomical Society|volume=474|issue=3|pages=3228–3236|year=2017|last1=Pollock|first1=A. M. T|last2=Crowther|first2=P. A|last3=Tehrani|first3=K|last4=Broos|first4=Patrick S|last5=Townsley|first5=Leisa K|bibcode=2018MNRAS.474.3228P|arxiv=1803.00822}}
7. ^1 {{cite journal|bibcode=2016MNRAS.458..624C|arxiv=1603.04994|title=The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters|journal=Monthly Notices of the Royal Astronomical Society|volume=458|issue=1|pages=624–659|author1=Crowther|first1=Paul A.|last2=Caballero-Nieves|first2=S. M.|last3=Bostroem|first3=K. A.|last4=Maíz Apellániz|first4=J.|last5=Schneider|first5=F. R. N.|last6=Walborn|first6=N. R.|last7=Angus|first7=C. R.|last8=Brott|first8=I.|last9=Bonanos|first9=A.|last10=De Koter|first10=A.|last11=De Mink|first11=S. E.|last12=Evans|first12=C. J.|last13=Gräfener|first13=G.|last14=Herrero|first14=A.|last15=Howarth|first15=I. D.|last16=Langer|first16=N.|last17=Lennon|first17=D. J.|last18=Puls|first18=J.|last19=Sana|first19=H.|last20=Vink|first20=J. S.|year=2016|doi=10.1093/mnras/stw273}}
8. ^{{Cite journal | doi = 10.1051/0004-6361/201321906| title = Fundamental properties of core-collapse supernova and GRB progenitors: Predicting the look of massive stars before death| journal = Astronomy & Astrophysics| volume = 558| pages = A131| year = 2013| last1 = Groh | first1 = J. H. | last2 = Meynet | first2 = G. | last3 = Georgy | first3 = C. | last4 = Ekström | first4 = S. | bibcode = 2013A&A...558A.131G|arxiv = 1308.4681 }}

External links

  • [https://www.spacetelescope.org/images/opo9405c/ ESA/Hubble image]
{{Stars of Dorado}}{{Sky|05|38|44.25|-|69|06|05.8|165000}}

7 : Stars in the Large Magellanic Cloud|Dorado (constellation)|Large Magellanic Cloud|Tarantula Nebula|Extragalactic stars|Wolf–Rayet stars|2MASS objects
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