WR 136 is a Wolf–Rayet star located in the constellation Cygnus. It is in the center of the Crescent Nebula. Its age is estimated to be around 4.7 million years and it is nearing the end of its life. Within a few hundred thousand years, it is expected to explode as a supernova.[8]
According to recent estimations, WR 136 is 600,000 times brighter than the Sun, 21 times more massive, and 5.1 times larger. Its surface temperature is around 70,000 kelvins.[4]
WR 136 blew off a shell of material with a mass of around 5 M☉ when it became a red supergiant around 120,000–240,000 years ago and this is still expanding at 80 km/s.[9] Currently, its fast stellar wind, ejected from the star at around 3.8 million mph (1,700 km/s[10]), is catching up to the material ejected from the star and shaping it into a shell. Ultraviolet rays emitted from WR 136's hot surface cause the shell to glow.[9]
There is some evidence WR 136 may be a binary star. Its companion would be a low-mass star of spectral classificationK or M that would complete an orbit around the Wolf-Rayet star each 5.13 days, being the progenitor of a low-mass X-ray binary system.[11]
Referencesedit
^"MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
^ abVan Leeuwen, F. (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.
^ abcDucati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
^ abcdefgSota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv:1904.04687. Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. S2CID 104292503.
^Barbier-Brossat, M.; Petit, M.; Figon, P. (1994). "Third bibliographic catalogue of stellar radial velocities (Text in French)". Astronomy and Astrophysics Supplement Series. 108: 603. Bibcode:1994A&AS..108..603B.
^ abcBrown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^Gräfener, G.; Vink, J. S.; Harries, T. J.; Langer, N. (2012). "Rotating Wolf-Rayet stars in a post RSG/LBV phase". Astronomy & Astrophysics. 547: A83. arXiv:1210.1153. Bibcode:2012A&A...547A..83G. doi:10.1051/0004-6361/201118664. S2CID 55530420.
^ abMoore, Brian D.; Hester, J. Jeff; Scowen, Paul A. (2000). "Hubble Space Telescope Observations of the Wolf-Rayet Nebula NGC 6888". The Astronomical Journal. 119 (6): 2991. arXiv:astro-ph/0003053. Bibcode:2000AJ....119.2991M. doi:10.1086/301389. S2CID 17769849.
^ abMesa-Delgado, A.; Esteban, C.; García-Rojas, J.; Reyes-Pérez, J.; Morisset, C.; Bresolin, F. (2014). "The Trace of the CNO Cycle in the Ring Nebula NGC 6888". The Astrophysical Journal. 785 (2): 100. arXiv:1402.6181. Bibcode:2014ApJ...785..100M. doi:10.1088/0004-637X/785/2/100. S2CID 118596124.
^Hamann, W.-R.; Wessolowski, U.; Koesterke, L. (1994). "Non-LTE spectral analyses of Wolf-Rayet stars: The nitrogen spectrum of the WN6 prototype HD 192163 (WR136)". Astronomy and Astrophysics. 281: 184. Bibcode:1994A&A...281..184H. ISSN 0004-6361.
^ Rustamov, D. N.; Cherepashchuk, A. M. (2011). "The Wolf-Rayet star HD 192163 as a possible evolutionary progenitor of a low-mass X-ray binary". Astronomy Reports. 55 (4): 347–358. Bibcode:2011ARep...55..347R. doi:10.1134/S1063772911010069. S2CID 121379439. Retrieved 17 July 2013.
Further readingedit
Bychkov, K. V.; Sitnik, T. G. (2006). "Stratification of optical emission from NGC 6888 as a trace of the interaction between Wolf-Rayet stellar wind and the shell of a red supergiant". Astronomy Letters. 32 (6): 406. Bibcode:2006AstL...32..406B. doi:10.1134/S1063773706060041. S2CID 123039046.
wolf, rayet, star, located, constellation, cygnus, center, crescent, nebula, estimated, around, million, years, nearing, life, within, hundred, thousand, years, expected, explode, supernova, light, curve, v1770, cygni, plotted, from, tess, data, observation, d. WR 136 is a Wolf Rayet star located in the constellation Cygnus It is in the center of the Crescent Nebula Its age is estimated to be around 4 7 million years and it is nearing the end of its life Within a few hundred thousand years it is expected to explode as a supernova 8 WR 136A light curve for V1770 Cygni plotted from TESS data 1 Observation dataEpoch J2000 Equinox J2000 Constellation Cygnus Right ascension 20h 12m 06 5421s 2 Declination 38 21 17 779 2 Apparent magnitude V 7 50 3 Characteristics Spectral type WN6 h s 4 U B color index 0 37 3 B V color index 0 01 3 AstrometryRadial velocity Rv 21 6 5 km sProper motion m RA 7 54 6 mas yr Dec 7 38 6 mas yrParallax p 0 4865 0 0337 mas 6 Distance6 700 500 ly 2 100 100 pc Absolute magnitude MV 5 63 4 DetailsMass21 4 M Radius5 10 4 R Luminosity600 000 4 L Temperature70 800 4 KRotation37 7 Age4 7 8 Myr Other designationsV1770 Cyg AG 38 1977 GSC 03151 01765 BD 37 3821 HD 192163 HIP 99546 GC 28056 SAO 69592 Database referencesSIMBADdata WR 136 at the centre of NGC 6888 According to recent estimations WR 136 is 600 000 times brighter than the Sun 21 times more massive and 5 1 times larger Its surface temperature is around 70 000 kelvins 4 WR 136 blew off a shell of material with a mass of around 5 M when it became a red supergiant around 120 000 240 000 years ago and this is still expanding at 80 km s 9 Currently its fast stellar wind ejected from the star at around 3 8 million mph 1 700 km s 10 is catching up to the material ejected from the star and shaping it into a shell Ultraviolet rays emitted from WR 136 s hot surface cause the shell to glow 9 There is some evidence WR 136 may be a binary star Its companion would be a low mass star of spectral classification K or M that would complete an orbit around the Wolf Rayet star each 5 13 days being the progenitor of a low mass X ray binary system 11 References edit MAST Barbara A Mikulski Archive for Space Telescopes Space Telescope Science Institute Retrieved 8 December 2021 a b Van Leeuwen F 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 Ducati J R 2002 VizieR Online Data Catalog Catalogue of Stellar Photometry in Johnson s 11 color system CDS ADC Collection of Electronic Catalogues 2237 0 Bibcode 2002yCat 2237 0D a b c d e f g Sota A Maiz Apellaniz J Morrell N I Barba R H Walborn N R Gamen R C Arias J I Alfaro E J Oskinova L M 2019 The Galactic WN stars revisited Impact of Gaia distances on fundamental stellar parameters Astronomy amp Astrophysics A57 625 arXiv 1904 04687 Bibcode 2019A amp A 625A 57H doi 10 1051 0004 6361 201834850 S2CID 104292503 Barbier Brossat M Petit M Figon P 1994 Third bibliographic catalogue of stellar radial velocities Text in French Astronomy and Astrophysics Supplement Series 108 603 Bibcode 1994A amp AS 108 603B a b c Brown A G A et al Gaia collaboration August 2018 Gaia Data Release 2 Summary of the contents and survey properties Astronomy amp Astrophysics 616 A1 arXiv 1804 09365 Bibcode 2018A amp A 616A 1G doi 10 1051 0004 6361 201833051 Gaia DR2 record for this source at VizieR Grafener G Vink J S Harries T J Langer N 2012 Rotating Wolf Rayet stars in a post RSG LBV phase Astronomy amp Astrophysics 547 A83 arXiv 1210 1153 Bibcode 2012A amp A 547A 83G doi 10 1051 0004 6361 201118664 S2CID 55530420 a b Moore Brian D Hester J Jeff Scowen Paul A 2000 Hubble Space Telescope Observations of the Wolf Rayet Nebula NGC 6888 The Astronomical Journal 119 6 2991 arXiv astro ph 0003053 Bibcode 2000AJ 119 2991M doi 10 1086 301389 S2CID 17769849 a b Mesa Delgado A Esteban C Garcia Rojas J Reyes Perez J Morisset C Bresolin F 2014 The Trace of the CNO Cycle in the Ring Nebula NGC 6888 The Astrophysical Journal 785 2 100 arXiv 1402 6181 Bibcode 2014ApJ 785 100M doi 10 1088 0004 637X 785 2 100 S2CID 118596124 Hamann W R Wessolowski U Koesterke L 1994 Non LTE spectral analyses of Wolf Rayet stars The nitrogen spectrum of the WN6 prototype HD 192163 WR136 Astronomy and Astrophysics 281 184 Bibcode 1994A amp A 281 184H ISSN 0004 6361 Rustamov D N Cherepashchuk A M 2011 The Wolf Rayet star HD 192163 as a possible evolutionary progenitor of a low mass X ray binary Astronomy Reports 55 4 347 358 Bibcode 2011ARep 55 347R doi 10 1134 S1063772911010069 S2CID 121379439 Retrieved 17 July 2013 Further reading editBychkov K V Sitnik T G 2006 Stratification of optical emission from NGC 6888 as a trace of the interaction between Wolf Rayet stellar wind and the shell of a red supergiant Astronomy Letters 32 6 406 Bibcode 2006AstL 32 406B doi 10 1134 S1063773706060041 S2CID 123039046 External links edithttp chandra harvard edu photo 2003 ngc6888 http www giga parsec de WRspectra html http www castfvg it stelle spettri O wr 136 01 htm Retrieved from https en wikipedia org w index php title WR 136 amp oldid 1125180618, wikipedia, wiki, book, books, library,
