Jupiter ’ s atmosphere has been observed to be depleted in helium ( \mbox { $Y _ { atm } $ } \sim 0.24 ) , suggesting active helium sedimentation in the interior . This is accounted for in standard Jupiter structure and evolution models through the assumption of an outer , He-depleted envelope that is separated from the He-enriched deep interior by a sharp boundary . Here we aim to develop a model for Jupiter ’ s inhomogeneous thermal evolution that relies on a more self-consistent description of the internal profiles of He abundance , temperature , and heat flux . We make use of recent numerical simulations on H/He demixing , and on layered ( LDD ) and oscillatory ( ODD ) double diffusive convection , and assume an idealized planet model composed of a H/He envelope and a massive core . A general framework for the construction of interior models with He rain is described . Despite , or perhaps because of , our simplifications made we find that self-consistent models are rare . For instance , no model for ODD convection is found . We modify the H/He phase diagram of Lorenzen et al . to reproduce Jupiter ’ s atmospheric helium abundance and examine evolution models as a function of the LDD layer height , from those that prolong Jupiter ’ s cooling time to those that actually shorten it . Resulting models that meet the luminosity constraint have layer heights of \approx 0.1 –1 km , corresponding to \approx 10 , –20,000 layers in the rain zone between \sim 1 and 3–4.5 Mbars . Present limitations and directions for future work are discussed , such as the formation and sinking of He droplets .