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Record: oai:ARNO:305784

AuthorsS.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
TitleDynamical masses for the Large Magellanic Cloud massive binary system [L72] LH 54-425
JournalAstrophysical Journal
Volume682
Year2008
Issue1
Pages492-498
ISSN0004637X
FacultyFaculty of Science
Institute/dept.FNWI: Astronomical Institute Anton Pannekoek (IAP)
AbstractWe 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 typeArticle
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