Melnick 42

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

Melnick 42
Grand star-forming region R136 in NGC 2070 (captured by the Hubble Space Telescope).jpg
Melnick 42 (annotated in Commons)
Credit: Hubble Space Telescope
Observation data
Epoch J2000      Equinox J2000
Constellation Dorado
Right ascension  05h 38m 42.12s[1]
Declination −69° 05′ 55.19″[1]
Apparent magnitude (V) 12.78[1]
Spectral type O2If*[2]
B−V color index +0.08[3]
Radial velocity (Rv)173[4] km/s
Distance163,000 ly
(49,970[5] pc)
Absolute magnitude (MV)−7.4[3]
Mass189[3] M
Radius21.1[6] R
Luminosity3,600,000[3] L
Surface gravity (log g)3.90[7] cgs
Temperature47,300[3] K
Rotational velocity (v sin i)240[7] km/s
Age~1 million[8] years
Other designations
MK42, Brey 77, BAT99 105, 2MASS J05384212-6905552
Database references
The RMC 136 cluster. Melnick 42 is just above the main cluster in the rightmost image.

Melnick 42 is a massive blue supergiant star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Although it is only 21 times the size of the sun, its high temperature of 47,300 K makes it one of the most luminous stars of the Tarantula Nebula at 3,600,000 L. It is less than two parsecs from the centre of the R136 cluster, although that is well outside the central core.

Mk 42 was originally classified as spectral type WN when it was discovered, then as O3 If. When the slash stars were defined it was given the spectral type O3 If*/WN6. Finally, the introduction of the spectral class O2 and the refinement of slash star classifications led to it being tagged as O2 If*. Although it is given a supergiant luminosity class, it is effectively a main sequence star still burning hydrogen in its core. It is thought to be less than a million years old.[8]


  1. ^ a b c Doran, E. I.; Crowther, P. A.; De Koter, A.; Evans, C. J.; McEvoy, C.; Walborn, N. R.; Bastian, N.; Bestenlehner, J. M.; Gräfener, G.; Herrero, A.; Köhler, K.; Maíz Apellániz, J.; Najarro, F.; Puls, J.; Sana, H.; Schneider, F. R. N.; Taylor, W. D.; Van Loon, J. Th.; Vink, J. S. (2013). "The VLT-FLAMES Tarantula Survey. XI. A census of the hot luminous stars and their feedback in 30 Doradus". Astronomy & Astrophysics. 558: A134. arXiv:1308.3412. Bibcode:2013A&A...558A.134D. doi:10.1051/0004-6361/201321824.
  2. ^ Crowther, P. A.; Walborn, N. R. (2011). "Spectral classification of O2-3.5 If*/WN5-7 stars". Monthly Notices of the Royal Astronomical Society. 416 (2): 1311. arXiv:1105.4757. Bibcode:2011MNRAS.416.1311C. doi:10.1111/j.1365-2966.2011.19129.x.
  3. ^ a b c d e Bestenlehner, J. M.; Gräfener, G.; Vink, J. S.; Najarro, F.; De Koter, A.; Sana, H.; Evans, C. J.; Crowther, P. A.; Hénault-Brunet, V.; Herrero, A.; Langer, N.; Schneider, F. R. N.; Simón-Díaz, S.; Taylor, W. D.; Walborn, N. R. (2014). "The VLT-FLAMES Tarantula Survey. XVII. Physical and wind properties of massive stars at the top of the main sequence". Astronomy & Astrophysics. 570: A38. arXiv:1407.1837. Bibcode:2014A&A...570A..38B. doi:10.1051/0004-6361/201423643.
  4. ^ Schnurr, O.; Moffat, A. F. J.; St-Louis, N.; Morrell, N. I.; Guerrero, M. A. (2008). "A spectroscopic survey of WNL stars in the Large Magellanic Cloud: General properties and binary status". Monthly Notices of the Royal Astronomical Society. 389 (2): 806. arXiv:0806.2801. Bibcode:2008MNRAS.389..806S. doi:10.1111/j.1365-2966.2008.13584.x.
  5. ^ Pietrzyński, G; D. Graczyk; W. Gieren; I. B. Thompson; B. Pilecki; A. Udalski; I. Soszyński; et al. (7 March 2013). "An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent". Nature. 495 (7439): 76–79. arXiv:1303.2063. Bibcode:2013Natur.495...76P. doi:10.1038/nature11878. PMID 23467166.
  6. ^ Hainich, R.; Rühling, U.; Todt, H.; Oskinova, L. M.; Liermann, A.; Gräfener, G.; Foellmi, C.; Schnurr, O.; Hamann, W. -R. (2014). "The Wolf-Rayet stars in the Large Magellanic Cloud: A comprehensive analysis of the WN class". Astronomy & Astrophysics. 565: A27. arXiv:1401.5474v1. Bibcode:2014A&A...565A..27H. doi:10.1051/0004-6361/201322696.
  7. ^ a b Puls, J.; Kudritzki, R.-P.; Herrero, A.; Pauldrach, A. W. A.; Haser, S. M.; Lennon, D. J.; Gabler, R.; Voels, S. A.; Vilchez, J. M.; Wachter, S.; Feldmeier, A. (1996). "O-star mass-loss and wind momentum rates in the Galaxy and the Magellanic Clouds Observations and theoretical predictions". Astronomy and Astrophysics. 305: 171. Bibcode:1996A&A...305..171P.
  8. ^ a b Crowther, P. A.; Schnurr, O.; Hirschi, R.; Yusof, N.; Parker, R. J.; Goodwin, S. P.; Kassim, H. A. (2010). "The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M stellar mass limit". Monthly Notices of the Royal Astronomical Society. 408 (2): 731. arXiv:1007.3284. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x.