Tomographic Separation of Composite Spectra. VI. The Physical Properties of the Massive Close Binary HD 152248

Details Tomographic Separation of Composite Spectra. VI. The Physical Properties of the Massive Close Binary HD 152248 Tomographic Separation of Composite Spectra. VI. The Physical Properties of the Massive Close Binary HD 152248

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...518..450p&link_type=abstract

The Astrophysical Journal, Volume 518, Issue 1, pp. 450-456.

Astronomy and Astrophysics

Astronomy

22

Stars: Binaries: Eclipsing, Stars: Binaries: Spectroscopic, Stars: Early-Type, Stars: Fundamental Parameters, Stars: Individual (Hd 152248), Ultraviolet: Stars

Scientific paper

We present the results of a Doppler tomographic reconstruction of the UV spectra of the double-lined O binary HD 152248 based on observations made with IUE. We used cross-correlation methods to obtain radial velocities, confirm the orbital elements, estimate the UV flux ratio, and determine projected rotational velocities. The individual component spectra are classified as O7 I+O7 I using UV criteria defined by Penny, Gies, & Bagnuolo. We present a model fit of the eclipsing light curve from which we derive an orbital inclination, i=72^deg+/-3^deg. This analysis indicates that neither star is currently experiencing Roche lobe overflow. We place the individual components in the theoretical H-R diagram and show that the individual masses (M_p/M_solar=24.2+/-2.0 M_s/M_solar=25.8+/-2.0) derived from the combined spectroscopic and photometric analysis are significantly lower than those computed from evolutionary tracks for single stars.

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