Abstract
This chapter explores a homogeneous, nonadiabatic model of delta Cephei. In the pulsation theory of variable stars, it has long been noted that the radial velocity curve of the fundamental mode of a homogeneous star seems to fit the observations of Cepheid variable stars. This chapter explains how close this correspondence is for the radial velocity curve of δ Cephei. It discusses the internal structure of a homogenous star. The function w(t) is the scale factor. It can be independent of the Lagrangian or comoving coordinate ξ only for this particular mode and star. The chapter presents the position of the spherical shells of the star. It also discusses the hydrodynamical fields of a homogeneous star.
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