Astronomy:WR 136

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Short description: Star in the constellation of Cygnus
WR 136
V1770CygLightCurve.png
A light curve for V1770 Cygni, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
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]
Astrometry
Radial velocity (Rv)−21.6[5] km/s
Proper motion (μ) RA: −7.54[6] mas/yr
Dec.: −7.38[6] mas/yr
Parallax (π)0.4865 ± 0.0337[6] mas
Distance6,700 ± 500 ly
(2,100 ± 100 pc)
Absolute magnitude (MV)−5.63[4]
Details
Mass21[4] M☉
Radius5.10[4] R☉
Luminosity600,000[4] L☉
Temperature70,800[4] K
Rotation37[7]
Age4.7[8] Myr
Other designations
V1770 Cyg, AG+38 1977, GSC 03151-01765, BD+37 3821, HD 192163, HIP 99546, GC 28056, SAO 69592.
Database references
SIMBADdata
WR 136 at the centre of NGC 6888

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 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

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  2. ↑ 2.0 2.1 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  3. ↑ 3.0 3.1 3.2 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. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. et al. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics A57: 625. doi:10.1051/0004-6361/201834850. Bibcode: 2019A&A...625A..57H. 
  5. ↑ 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. 
  6. ↑ 6.0 6.1 6.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  7. ↑ 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. doi:10.1051/0004-6361/201118664. Bibcode: 2012A&A...547A..83G. 
  8. ↑ 8.0 8.1 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. doi:10.1086/301389. Bibcode: 2000AJ....119.2991M. 
  9. ↑ 9.0 9.1 Mesa-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. doi:10.1088/0004-637X/785/2/100. Bibcode: 2014ApJ...785..100M. 
  10. ↑ 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. ISSN 0004-6361. Bibcode: 1994A&A...281..184H. 
  11. ↑ 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. doi:10.1134/S1063772911010069. Bibcode: 2011ARep...55..347R. http://cdsads.u-strasbg.fr/abs/2011ARep...55..347R. Retrieved 17 July 2013. 

Further reading

  • 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. doi:10.1134/S1063773706060041. Bibcode: 2006AstL...32..406B. 

External links



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