A spectroscopic study of the short-period eclipsing Wolf-Rayet binary CX Cephei (WN5+O5 V)

Details A spectroscopic study of the short-period eclipsing Wolf-Rayet binary CX Cephei (WN5+O5 V) A spectroscopic study of the short-period eclipsing Wolf-Rayet binary CX Cephei (WN5+O5 V)

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...405..312l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 405, no. 1, p. 312-326.

Astronomy and Astrophysics

Astrophysics

23

Eclipsing Binary Stars, Stellar Orbits, Stellar Spectrophotometry, Wolf-Rayet Stars, O Stars, Stellar Envelopes, Stellar Mass, Stellar Winds

Scientific paper

Some 60 blue 5-A resolution CCD spectra are employed to derive a greatly improved circular velocity orbit for the 2.13-d eclipsing Wolf-Rayet binary CX Cephei. It is found that K(O) = 240 +/- 8 m/s and K(WR) = 340 +/- 10 km/s, corresponding to masses of M(O) sin cubed i = 25.2 +/- 1.9 solar masses and M(WR) sin cubed i = 17.8 +/- 1.4 solar masses. Evidence is found in the velocities of the strong He II 4686-A line for a secondary period at exactly one-third of the orbital period. This is not a harmonic resulting from a slight eccentricity of the orbit, but is probably due to a tidal distortion of the envelope where He II 4686 A is emitted. The unblended emission lines He II 4686 A, N IV 4058 A, and N V 4063 A show clear, phase-dependent variations in strength, as does the He I 3888-A P Cygni absorption edge. A qualitative model to account for the differing behavior of these lines is presented.

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