Secondaries of eclipsing binaries. III - U Cephei

Details Secondaries of eclipsing binaries. III - U Cephei Secondaries of eclipsing binaries. III - U Cephei

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244..546t&link_type=abstract

Astrophysical Journal, Part 1, vol. 244, Mar. 1, 1981, p. 546-551.

Astronomy and Astrophysics

Astronomy

21

Cepheid Variables, Eclipsing Binary Stars, Infrared Astronomy, Stellar Rotation, Stellar Spectra, Circular Orbits, Infrared Spectra, Line Spectra, Magnesium, Radial Velocity, Signal To Noise Ratios

Scientific paper

High-SNR near-IR Reticon spectra of U Cep, observed during and outside primary eclipse, reveal relatively well-defined lines of the secondary. The 8806-A Mg I line is distinctly weaker immediately before and after secondary eclipse than at other out-of-eclipse phases. This is interpreted as evidence that the strength of the secondary Mg I line is affected by heating of the secondary by the much brighter primary. As a result, the velocities at these phases may not be a true measure of orbital motion. A circular orbit solution of the secondary velocities, which excludes velocities for phases 0.35 to 0.65, is adopted. It yields K2 = 182 + or - 3 km/s and gamma = -1 + or - 2 km/s

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