Spectrograms of the eclipse of 32 Cygni in 1981 were taken. The authors select 22 spectrograms obtained at the times of ingress, totality and outside totality to determine radial velocities of the K supergiant. The observed radial velocities are in general agreement with the theoretical curve calculated by Guinan. The chromospheric emission of the K supergiant may possibly be formed in a shock front near the B star by linear scattering the light of the B star in the wind of the K supergiant. A simplified model of 32 Cygni is proposed. The mass loss rate dM/dt of the K supergiant due to radiation driven stellar winds is estimated.
Acta Astrophysica Sinica
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