Tomographic Separation of Composite Spectra. IX. The Massive Close Binary HD 115071

Details Tomographic Separation of Composite Spectra. IX. The Massive Close Binary HD 115071 Tomographic Separation of Composite Spectra. IX. The Massive Close Binary HD 115071

2002-01-29

arxiv.org/abs/astro-ph/0201480v2

Astrophys.J. 575 (2002) 1050-1056

Astronomy and Astrophysics

Astrophysics

Submitted to ApJ

Scientific paper

10.1086/341432

We present the first orbital elements for the massive close binary, HD 115071, a double-lined spectroscopic binary in a circular orbit with a period of 2.73135 +/- 0.00003 days. The orbital semiamplitudes indicate a mass ratio of M_2/M_1 = 0.58 +/- 0.02 and yet the stars have similar luminosities. We used a Doppler tomography algorithm to reconstruct the individual component optical spectra, and we applied well known criteria to arrive at classifications of O9.5 V and B0.2 III for the primary and secondary, respectively. We present models of the Hipparcos light curve of the ellipsoidal variations caused by the tidal distortion of the secondary, and the best fit model for a Roche-filling secondary occurs for an inclination of i = 48.7 +/- 2.1 degrees. The resulting masses are 11.6 +/- 1.1 and 6.7 +/- 0.7 solar masses for the primary and secondary, respectively, so that both stars are very overluminous for their mass. The system is one of only a few known semi-detached, Algol-type binaries that contain O-stars. We suggest that the binary has recently emerged from extensive mass transfer (possibly through a delayed contact and common envelope process).

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