About the eclipsing Wolf-Rayet binary HD 214419, CQ Cephei

Journal Article · Thu Mar 01 04:00:00 EST 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/168503· OSTI ID:6917784

Underhill, A B; Gilroy, K K; Hill, G M ^[1]

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1. British Columbia Univ., Vancouver (Canada)

Radial velocities and line profiles from spectrograms of the eclipsing WR binary star CQ Cephei are reported. Model stars and brightness ratios in the V band are used to obtain an internally consistent model for the system. The WR star appears to be a hydrogen-burning star with M(WR) = 13.6 solar masses, R(WR) = 5.5 solar radii, and T(eff) = 29,000 K, while the companion star has M(comp) = 16.0 solar masses, R(comp) = 6.4 solar radii, and T(eff) = 30,800 K. It is probably a B0 star. The sizes of the orbits are a(WR) = 9.7 solar radii and a(comp) = 8.2 solar radii. The complex shortward-displaced absorption components of He 5876 A indicate that the stars are buried in several streams of plasma. 25 refs.

• OSTI ID: 6917784
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 351; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
ECLIPSE
HYDROGEN BURNING
MAIN SEQUENCE STARS
MASS
MATHEMATICAL MODELS
ORBITS
PLASMA
RADIAL VELOCITY
SIZE
SPECTRA
STAR BURNING
STAR MODELS
STARS
VELOCITY
VISIBLE SPECTRA
WOLF-RAYET STARS