The early B-type eclipsing binary FZ CMa (HD 52942) - A massive triple system

Details The early B-type eclipsing binary FZ CMa (HD 52942) - A massive triple system The early B-type eclipsing binary FZ CMa (HD 52942) - A massive triple system

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...120..278m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 120, no. 2, April 1983, p. 278-286. Research supported by the National Researc

Astronomy and Astrophysics

Astrophysics

20

B Stars, Early Stars, Eclipsing Binary Stars, Stellar Spectrophotometry, Electrophotometry, Ephemerides, Light Curve, Radial Velocity, Stellar Evolution

Scientific paper

New photoelectric observations in uvby are used to construct a light curve of this double-line eclipsing system in which two components (A, B), each of type B2.5 IV-V, revolve in a 1.27 d orbit. A consistent solution of the light curve could be achieved only if a third body, denoted X, contributes 43% to the total flux in v, b, y and 36% in u. The third body manifests itself independently by periodic modulation in the times of minimum light, although it is not seen directly in the spectrum. Photographic coudé spectroscopy of the A+B components yields the masses mA ⪆ mB ≅ 5.3 M_sun; and orbital radii aA ⪉ aB ≅ 5.5 R_sun;. These masses are low for B2.5 IV-V and may be the result of insufficient correction for line blending due to the third body and/or of mass loss from the system during an earlier mass transfer phase. The spectral lines are very broad, even at conjunction. This may be due to line-broadening by the third body and/or to a previous contraction phase spin-up. The authors estimate mxsin ix ≅ 12 ± 4 M_sun; and Tx ≈ 16,000K. Along with the derived amount of third light, this corresponds to a B4 giant.

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