Lr. Penny et al., Tomographic separation of composite spectra. VI. The physical properties of the massive close binary HD 152248, ASTROPHYS J, 518(1), 1999, pp. 450-456
We present the results of a Doppler tomographic reconstruction of the UV sp
ectra of the double-lined O binary HD 152248 based on observations made wit
h IUE. We used cross-correlation methods to obtain radial velocities, confi
rm the orbital elements, estimate the UV flux ratio, and determine projecte
d rotational velocities. The individual component spectra are classified as
O7 I + O7 I using UV criteria defined by Penny, Gies, & Bagnuolo. We prese
nt a model fit of the eclipsing light curve from which we derive an orbital
inclination, i = 72 degrees + 3 degrees. This analysis indicates that neit
her star is currently experiencing Roche lobe overflow. We place the indivi
dual components in the theoretical H-R diagram and show that the individual
masses (M-p/M. = 24.2 +/- 2.0; M-s/M. = 25.8 +/- 2.0) derived from the com
bined spectroscopic and photometric analysis are significantly lower than t
hose computed from evolutionary tracks for single stars.