Abstract
CI Aur is a short-period Algol-type eclipsing binary with a period of 1.870052 days. Photometric observations in UBV bands were made at McDonald Observatory between 1984 November and 1985 January. The light curves show random flickering and short-time variations. Photometric solutions were obtained using the Wilson-Devinney method. CI Aur is found to be a semi-detached system, with the less massive secondary component filling its Roche lobe. The mass ratio is 0.687 and the orbital inclination is 74° 42. Autoregressive power spectral analysis and harmonic analysis of the light curves were made. The results show that the oscillations are multiply quasi-periodic and have low amplitudes. Gas stream from the secondary strikes the trailing hemisphere of the primary. The disk produced by the star-stream interaction, is unstable. Two models of the star are discussed.
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