Observational evidence for mass loss from classical Cepheids

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This paper examines the evidence for mass loss from classical Cepheid variables in the light of recent observational studies of infrared and ultraviolet emission from these objects. Mass-loss rates derived for several stars range between |$10^{-10}M_\odot \text{yr}^{-1}$| and |$10^{-10}M_\odot \text{yr}^{-1}$|⁠. The lower end of this range probably corresponds to the majority of classical Cepheids. Non-variable supergiants show, on average, a somewhat lower rate of infrared excess, but have mass-loss rates of the same order of magnitude as the Cepheids. On the basis of the observations to date, mass loss alone is insufficient in explaining the Cepheid mass discrepancy, indicating that adjustments to the evolutionary or pulsation models present a better prospect of resolving this discrepancy.