IN the eccentric-orbit binary model1,2, a compact object is in an eccentric orbit around a more massive, slightly evolved star. If the compact object accretes mass from the stellar wind of the normal star, the accretion rate is time dependent, so that the resulting X-ray emission would show a maximum at periastron (in the absence of absorption extinction) and a minimum at apastron. It is also possible that accretion might arise from direct mass transfer resulting from contraction of the Roche lobe with decreasing primary to secondary distance. We show here that the stellar wind model, is adequate to describe the majority of transient X-ray sources.