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An analytical derivation is presented for computing mass-loss rates ofCepheids by using the method of Castor, Abbott, & Klein (1975) modified toinclude a term for momentum input from pulsation and shocks generated in theatmosphere. Using this derivation, mass-loss rates of Cepheids are determinedas a function of stellar parameters. When applied to a set of known Cepheids,the calculated mass-loss rates range from 10^{-10} to 10^{-7}M_{Sun}/yr, largerthan if the winds were driven by radiation alone. Infrared excesses based onthe predicted mass-loss rates are compared to observations from opticalinterferometry and IRAS, and predictions are made for Spitzer observations. Themass-loss rates are consistent with the observations, within the uncertaintiesof each. The rate of period change of Cepheids is discussed and shown to relateto mass loss, albeit the dependence is very weak. There is also a correlationbetween the large mass-loss rates and the Cepheids with slowest absolute rateof period change due to evolution through the instability strip. The enhancedmass loss helps illuminate the issue of infrared excess and the massdiscrepancy found in Cepheids.

On the Enhancement of Mass Loss in Cepheids Due to Radial Pulsation