Abstract
ABSTRACT High-resolution Reticon spectra of the F8 Ia-0 supergiant ρ Cas providing lines of differing excitation potential are employed to construct radial-velocity curves which reveal a semiregular pulsation of the atmosphere. Analysis of line-doubling episodes supports the presence of a dominant radial pulsation mode with a period around 500 days, significantly longer than the radial fundamental mode predicted on the basis of Cepheid-like PLC relations for a star evolving to the red supergiant region. Predicted periods for fundamental radial pulsations in stars returning toward the blue supergiant region are comparable to the observed quasi-period.
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