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journal id: "astrophysicalxjournal"
| Authors | S.J. Williams, D.R. Gies, T.J. Henry, J.A. Orosz, M.V. McSwain, T.C. Hillwig, L.R. Penny, G. Sonneborn, R. Iping, K.A. van der Hucht, L. Kaper | | Title | Dynamical masses for the Large Magellanic Cloud massive binary system [L72] LH 54-425 |
| Journal | Astrophysical Journal |
| Volume | 682 |
| Year | 2008 |
| Issue | 1 |
| Pages | 492-498 |
| ISSN | 0004637X |
| Faculty | Faculty of Science |
| Institute/dept. | FNWI: Astronomical Institute Anton Pannekoek (IAP) |
| Abstract | We present results from an optical spectroscopic investigation of the massive binary system [L72] LH 54-425 in the LH 54 OB association in the Large Magellanic Cloud. We revise the ephemeris of [L72] LH 54-425 and find an orbital period of 2.24741 +/- 0.00004 days. We find spectral types of O3 V for the primary and O5 V for the secondary. We made a combined solution of the radial velocities and previously published V-band photometry to determine the inclination for two system configurations, i = 52(-3)(+2) degrees for the configuration of the secondary star being more tidally distorted and i = 55 degrees +/- 1 degrees for the primary as the more tidally distorted star. We argue that the latter case is more probable, and this solution yields masses and radii of M-1 = 47 +/- 2 M-circle dot and R-1 = 11.4 +/- 0.1 R-circle dot for the primary, and M-2 = 28 +/- 1 M-circle dot and R-2 = 8.1 +/- 0.1 R-circle dot for the secondary. Our analysis places LH 54-425 among the most massive stars known. Based on the position of the two stars plotted on a theoretical HR diagram, we find the age of the system to be similar to 1.5 Myr. |
| Document type | Article |
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