LH54-425
| 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] |
| Characteristics | |
| Spectral type | O3V + O5V[3] |
| Orbit[4] | |
| Period (P) | 2.2474 days |
| Semi-major axis (a) | 30.4 R☉ |
| Eccentricity (e) | 0 |
| Inclination (i) | 55° |
| Semi-amplitude (K1) (primary) | 201.6 km/s |
| Semi-amplitude (K2) (secondary) | 359.1 km/s |
| Details[4] | |
| O3 | |
| 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 |
| O5 | |
| 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[5] Myr |
| Database references | |
| SIMBAD | [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=[L72]+LH+54-425 data] |
LH54-425 is a star system that was identified as a spectroscopic binary by astronomer Pablo G. Ostrov in 2002. It is located in the LH 54 OB association within the Large Magellanic Cloud[6] Both members are O-type stars and the pair is among the most massive known. They are emitting a stellar wind with a velocity of 2,800 km/s.[3] As the pair evolve, they may merge to form a single star with a mass 80 times that of the Sun. In time, they will explode as a core-collapse supernova.[7]
References
- 1 2 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:0905.1328, Bibcode:2009AJ....138.1003B, doi:10.1088/0004-6256/138/4/1003
- ↑ "[L72] LH 54-425 -- Spectroscopic binary", SIMBAD (Centre de Données astronomiques de Strasbourg), retrieved 2015-06-18
- 1 2 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
- 1 2 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:0802.4232. Bibcode:2008ApJ...682..492W. doi:10.1086/589687.
- ↑ 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:1201.3280. Bibcode:2012ApJ...748...96M. doi:10.1088/0004-637X/748/2/96.
- ↑ Ostrov, Pablo G. (October 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/0205028, Bibcode:2002MNRAS.336..309O, doi:10.1046/j.1365-8711.2002.05754.x
- ↑ Naeye, Bob (May 28, 2007), NASA's FUSE Satellite Catches Collision of Titans, NASA, retrieved 2015-06-18
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