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Results of spectral photoelectric observations of HD 50896 obtained in the period 1975 February-1978 March are presented. The variations in emission-line profiles, radial velocities and light are found to be consistent with the 3.76 day period. It is concluded that the binary hypothesis is the most likely one to explain the periodic variations, and that the companion is probably a neutron star of mass m2 equals 1.3 plus or minus 0.4 solar mass. In addition, it is found that the eccentricity differs considerably from zero. It is suggested that this eccentricity is responsible for some of the more extraordinary variations observed in HD 50896.
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Firmani et al. (1980) studied this question.
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