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LH54-425 is the bright star on the left. NGC 1955 is the cluster in the middle, dominated by the B0 supergiant HD 269925. The bright star on the right is the Wolf-Rayet/O-supergiant binary HD 36402.
Observation data
Epoch J2000      Equinox J2000
Constellation Dorado
Right ascension 05h 26m 24.2505s[1]
Declination −67° 30′ 17.194″[1]
Apparent magnitude (V) 13.13[2]
Spectral type O3V + O5V[3]
U−B color index +0.01[4]
B−V color index −0.31[4]
Period (P) 2.2474 days[5]
Semi-major axis (a) 30.4 R
Eccentricity (e) 0
Inclination (i) 55°
Semi-amplitude (K1)
201.6 km/s
Semi-amplitude (K2)
359.1 km/s
Mass 47 M
Radius 11.4 R
Luminosity 500,000 L
Surface gravity (log g) 4.00 cgs
Temperature 45,000 K
Rotational velocity (v sin i) 197 km/s
Mass 28 M
Radius 8.1 R
Luminosity 160,000 L
Surface gravity (log g) 4.07 cgs
Temperature 41,000 K
Rotational velocity (v sin i) 182 km/s
Age 2.0[6] Myr
Database references

LH54-425 is a spectroscopic binary star system in the LH 54 OB association within the Large Magellanic Cloud in the constellation Dorado.

Discovery and visibility[edit]

The OB association LH 54 was catalogued by astronomers Lucke and Hodge in 1970, listed as containing 18 member stars. It is associated with NGC 1955, part of the N51 HII region.[7] The brightness and colour of LH54-425 were measured in 1974.[4] In 1996 M.S. Oey determined that LH54-425 has an apparent (visual) magnitude of 13.13 and classified it as an O3 class giant.[2]

A series of photometric and spectroscopic observations carried out by P. Ostrov between from 1998 to 2001 revealed that LH54-425 varied very slightly with a regular period of 2.2475 days [5] due to distorted stars in a close binary system composed by an O3 class giant and an approximately O5 class companion. The masses of the two stars were estimated at 100 M and 50 M. A derivation of the orbit in 2008 using more accurate radial velocity data defined the companions as O3 and O5 main sequence stars with masses of 47 M and 28 M respectively.[3]


The binary system has an orbital period of 2 days, 5 hours, and 56 minutes. The two stars are separated by only 15 times the width of the sun, or less than twice their own diameters. The more massive primary orbits at 200 km/s, while the secondary moves at 350 km/s, and the system as a whole is approaching us at around 300 km/s.[3]


Both members of the LH54-425 binary system are hot, massive, and luminous stars. The less massive secondary has an effective surface temperature of 41,000 K and the more massive primary is 45,000 K. The stars are 8 and 11 times the size of the sun, and the combination of high temperature and large size means the primary star is 500,000 times as luminous as the sun and the secondary 160,000 times as luminous. They are emitting a stellar wind with a velocity of 2,800 km/s.[8]


Stellar evolutionary models closely match the properties of the two stars at two million years old. At this age, they have almost the same mass as when they first formed. Comparison between the models and observations suggest a small mass discrepancy, with the models predicting higher masses than those derived from the orbit. This is a long-standing and unsolved problem in the modelling of massive stars.[6]

As the pair evolve, they may merge to form a single massive star. In time, the individual stars or the result of the merger will explode as a core-collapse supernova.[9]


  1. ^ a b Bonanos, A. Z.; et al. (October 2009). "Spitzer SAGE Infrared Photometry of Massive Stars in the Large Magellanic Cloud". The Astronomical Journal. 138 (4): 1003–1021. arXiv:0905.1328Freely accessible. Bibcode:2009AJ....138.1003B. doi:10.1088/0004-6256/138/4/1003. 
  2. ^ a b Oey, M. S. (1996). "UBV Photometry of OB Associations within Superbubbles of the Large Magellanic Cloud". Astrophysical Journal Supplement. 104: 71. Bibcode:1996ApJS..104...71O. doi:10.1086/192292. 
  3. ^ a b c d e Williams, S. J.; Gies, D. R.; Henry, T. J.; Orosz, J. A.; McSwain, M. V.; Hillwig, T. C.; Penny, L. R.; Sonneborn, G.; Iping, R.; Van Der Hucht, K. A.; Kaper, L. (2008). "Dynamical Masses for the Large Magellanic Cloud Massive Binary System [L72] LH 54-425". The Astrophysical Journal. 682: 492–498. arXiv:0802.4232Freely accessible. Bibcode:2008ApJ...682..492W. doi:10.1086/589687. 
  4. ^ a b c Hill, Robert J.; Madore, Barry F.; Freedman, Wendy L. (1994). "The initial mass function for massive stars in the Magellanic Clouds. 1: UBV photometry and color-magnitude diagrams for 14 OB associations". Astrophysical Journal Supplement Series. 91: 583. Bibcode:1994ApJS...91..583H. doi:10.1086/191949. 
  5. ^ a b Ostrov, Pablo G. (2002). "A very massive spectroscopic binary in the LH 54 OB association in the Large Magellanic Cloud". Monthly Notices of the Royal Astronomical Society. 336 (1): 309–314. arXiv:astro-ph/0205028Freely accessible. Bibcode:2002MNRAS.336..309O. doi:10.1046/j.1365-8711.2002.05754.x. 
  6. ^ a b Massey, Philip; Morrell, Nidia I.; Neugent, Kathryn F.; Penny, Laura R.; Degioia-Eastwood, Kathleen; Gies, Douglas R. (2012). "Photometric and Spectroscopic Studies of Massive Binaries in the Large Magellanic Cloud. I. Introduction and Orbits for Two Detached Systems: Evidence for a Mass Discrepancy?". The Astrophysical Journal. 748 (2): 96. arXiv:1201.3280Freely accessible. Bibcode:2012ApJ...748...96M. doi:10.1088/0004-637X/748/2/96. 
  7. ^ Lucke, P. B.; Hodge, P. W. (1970). "A catalogue of stellar associations in the Large Magellanic Cloud". Astronomical Journal. 75: 171. Bibcode:1970AJ.....75..171L. doi:10.1086/110959. 
  8. ^ Iping, R. C.; et al. (April 2008). Hamann, Wolf-Rainer; Feldmeier, Achim; Oskinova, Lidia M., eds. Far-ultraviolet spectroscopy of O+O binaries in the Magellanic Clouds. Clumping in hot-star winds : proceedings of an international workshop held in Potsdam, Germany, 18. – 22. June 2007. p. 244. Bibcode:2008cihw.conf..244I. ISBN 978-3-940793-33-1. 
  9. ^ Naeye, Bob (May 28, 2007), NASA's FUSE Satellite Catches Collision of Titans, NASA, retrieved 2015-06-18