Linear adiabatic periods, which have been mostly used to evaluate the masses of pulsating stars, shouldn\u27t be used for low surface-gravity variable stars, because those differ considerably with linear nonadiabatic periods and nonlinear theoretical periods in some cases. The use of nonadiabatic periods sometimes derive drastically low stellar masses. Taking into account the small occurrence of variable stars at the bluer side of cepheid instability strip on the HR diagram, it may be supposed that most of these variables will be less massive evolved stars
